improving the cosmic distance ladder. distance and structure of … · 2017. 10. 11. · the...
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Alma Mater Studiorum
Università degli Studi di Bologna
DIPARTIMENTO DI FISICA E ASTRONOMIA
Dottorato di ricerca in AstronomiaCiclo XXVII
Improving the cosmic distance ladder.Distance and structure of the Large
Magellanic Cloud.
Dottoranda:Tatiana Muraveva
Relatore:Prof. Bruno Marano
Co–Relatori:Dott.sa Gisella Clementini
Dott.sa Marcella Marconi
Dott. Enzo Brocato
Coordinatore:
Prof. Lauro Moscardini
Esame finale anno 2014
Settore Concorsuale: 02/C1 – Astronomia, Astrofisica, Fisica della Terra e dei PianetiSettore Scientifico-Disciplinare: FIS/05 – Astronomia e Astrofisica
Contents
Introduction 1
1 The cosmological distance ladder 5
1.1 Trigonometric parallax . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5
1.2 Gaia . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7
1.3 Variable stars as distance indicators . . . . . . . . . . . . . . . . . . . . . 10
1.4 Classical Cepheids . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12
1.5 RR Lyrae stars . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 14
1.5.1 Metal abundance of RR Lyrae stars . . . . . . . . . . . . . . . . . 15
1.5.2 MV − [Fe/H] and PLKZ relations of RR Lyrae stars . . . . . . . 19
1.6 Eclipsing binaries . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 24
1.6.1 Classification of eclipsing binaries . . . . . . . . . . . . . . . . . . 24
1.6.2 Eclipsing binaries as distance indicators . . . . . . . . . . . . . . . 25
2 The Large Magellanic Cloud 29
2.1 Magellanic System . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 29
2.2 Structure of the LMC . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 30
2.3 Distance to the LMC . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 32
2.4 LMC Surveys . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 35
2.4.1 EROS-2 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 35
2.4.2 OGLE . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 36
2.4.3 VMC . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 38
3 Classical Cepheids in the VMC tile LMC 8_3 41
3.1 EROS-2 data for candidate Classical Cepheids . . . . . . . . . . . . . . . . 41
3.2 Classification of candidate Classical Cepheids . . . . . . . . . . . . . . . . 50
i
CONTENTS
3.3 Strategy for extracting bona-fide Classical Cepheids . . . . . . . . . . . . . 52
4 Eclipsing binaries in the LMC 57
4.1 EROS-2 data for eclipsing binaries . . . . . . . . . . . . . . . . . . . . . . 57
4.2 Cross-correlation with other catalogues of eclipsing binaries in the LMC . . 59
4.3 Characteristics of eclipsing binaries with existing spectroscopy . . . . . . . 63
4.3.1 Cross-matches with the VLT-FLAMES surveys . . . . . . . . . . . 63
4.3.2 AAOmega spectroscopy . . . . . . . . . . . . . . . . . . . . . . . 63
4.4 Classification of eclipsing binaries . . . . . . . . . . . . . . . . . . . . . . 64
4.5 Period-Luminosity relation of eclipsing binaries . . . . . . . . . . . . . . . 67
4.5.1 PL relation of eclipsing binaries from the EROS-2 sample . . . . . 67
4.5.2 PL relation of eclipsing binaries from the OGLE III catalogue . . . 69
4.6 Structure of the LMC from “hot” eclipsing binaries and Classical Cepheids 74
5 RR Lyrae stars in the VMC tile LMC 5_5 77
5.1 Data for RR Lyrae stars in the bar of the LMC . . . . . . . . . . . . . . . . 77
5.2 PLKsZ relation of RR Lyrae stars in the LMC . . . . . . . . . . . . . . . 86
5.2.1 Method . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 86
5.2.2 Zero-point of the PLKsZ relation . . . . . . . . . . . . . . . . . . 87
5.3 Gaia observation of RR Lyrae stars in the Milky Way . . . . . . . . . . . . 90
5.3.1 Simulated Gaia data . . . . . . . . . . . . . . . . . . . . . . . . . 92
5.3.2 Simulation of the MV − [Fe/H] relation of RR Lyrae stars in the
Milky Way . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 95
6 RR Lyrae stars in the VMC tile LMC 8_3 97
6.1 Classification of EROS-2 candidate RR Lyrae stars . . . . . . . . . . . . . 97
6.2 Comparison with the OGLE III catalogue . . . . . . . . . . . . . . . . . . 108
6.3 Fourier analysis of the RR Lyrae stars in tile LMC 8_3 . . . . . . . . . . . 112
6.4 Metallicity of the RR Lyrae stars in tile LMC 8_3 . . . . . . . . . . . . . . 123
6.5 Ks magnitude of the RR Lyrae stars in tile LMC 8_3 . . . . . . . . . . . . 131
6.6 Distance to the tile LMC 8_3 from RR Lyrae stars . . . . . . . . . . . . . . 140
Conclusions 145
Appendix 151
ii
CONTENTS
A Properties of the “hot” eclipsing binaries in the LMC 151
iii
Introduction
The knowledge of distances is crucially important to all branches of astronomy. In order to
measure the distances astronomers have developed a number of different techniques. Some
methods, such as the trigonometric parallax, are based on geometrical principals, others
involve the concept of distance indicators. The successions of techniques used to measure
distances to celestial objects, is called cosmological distance ladder.
The Large Magellanic Cloud (LMC) is widely considered as the first step of the cos-
mological distance ladder, since it contains many different distance indicators. An accurate
determination of the distance to the LMC allows one to calibrate these distance indicators
that are then used to measure the distance to far objects.
In standard cosmology the Universe expands uniformly according to the Hubble law
v = H0d, where v is the recession velocity of a galaxy at a distance d, and H0 is the Hubble
constant which measures the expansion rate at the current epoch. H0 sets the age of the
Universe and the size of the observable Universe. Many of the methods that are used to
measure H0 are calibrated by the distance to the LMC. The LMC is distant enough, and
its main features lie close to the plane of the sky, hence, in first approximation it could be
assumed that its stellar components are all at the same distance from us. However, the LMC
has a rather complex internal structure, that must be taken into account when pushing for
distance comparisons at a few percent level.
The main goal of this thesis is to study the distance and structure of the LMC, as traced
by different distance indicators. For these purposes three types of distance indicators were
chosen: Classical Cepheids,“hot” eclipsing binaries and RR Lyrae stars. These objects
belong to different stellar populations tracing, in turn, different sub-structures of the LMC.
The RR Lyrae stars (age ≥ 10 Gyr) are distributed smoothly and likely trace the halo of the
LMC. Classical Cepheids are young objects (age ∼50-200 Myr), mainly located in the bar
and spiral arm of the galaxy, while “hot” eclipsing binaries mainly trace the star forming
regions of the LMC. Furthermore, we have chosen these distance indicators for our study,
1
INTRODUCTION
since the calibration of their zero-points is based on fundamental geometric methods. The
ESA cornerstone mission Gaia, launched on 19 December 2013, will measure trigonometric
parallaxes for one billion stars with an accuracy of 20 micro-arcsec (µas) at V ∼ 15 mag,
and 200 µas at V ∼ 20 mag, thus will allow us to calibrate the zero-points of Classical
Cepheids, eclipsing binaries and RR Lyrae stars with an unprecedented precision. One goal
of this thesis was to check the impact of Gaia on the determination of distances with RR
Lyrae stars, based on Gaia expected performances.
In this thesis we extensively use the data of the VISTA near-infrared ESO public sur-
vey of the Magellanic Clouds system (VMC, PI M.-R. Cioni, see Cioni et al. 2011). The
determination of the distance to different tiles of the VMC survey by applying the Clas-
sical Cepheid’s period-luminosity (PLKs) and the RR Lyrae period-luminosity-metallicity
(PLKsZ) relations in the Ks passband allows us to study the structure of the LMC. We also
use in our analysis visual data of the microlensing surveys EROS (Tisserand et al., 2007)
and OGLE (Udalski et al., 1997).
Chapters 1 and 2 of the thesis provide the scientific concept of our study. In Chapter 1
we focus on the general description of the cosmological distance ladder with emphasis on
the three types of distance indicators, which were specifically analysed in this study. Chap-
ter 2 gives general information about the LMC. In Chapter 3 we provide the results of our
analysis of Classical Cepheids in the LMC. We use the visual data from the EROS-2 survey
in order to classify Classical Cepheids in the VMC tile LMC 8_3 and determine their basic
properties. These parameters will be used to derive the mean Ks magnitudes of Classical
Cepheids and to estimate the distance to this tile by applying the Classical Cepheid’s PL
relation in the Ks passband. The general strategy developed to classify candidate Classical
Cepheids from the EROS-2 survey, which will be applied to all the tiles covered only by the
EROS-2 survey, is described.
Chapter 4 presents the results of our analysis of “hot” eclipsing binaries in the LMC
observed by the EROS-2 survey. We classified them on the basis of the visual inspection
and the Fourier analysis of their light curves. We then analyse the near-infrared light curves
of the eclipsing binaries that have a counterpart in the VMC catalogue, in order to study
their PL relation and the possibility of using the PL relation to determine the distance to
the LMC.
Chapter 5 and 6 summarize the work done on the RR Lyrae stars in the VMC tiles
LMC 5_5 and 8_3. By using the VMC data for a sample of RR Lyrae stars in tile LMC
2
INTRODUCTION
5_5 we derive our own PLKsZ relation. We then apply this relation in combination with
the relations from the literature to determine the distance to tiles LMC 5_5 and 8_3. The
derived distances allow us to make preliminary conclusions about the structure of the LMC.
In order to check the impact of Gaia on the determination of the RR Lyrae PLKsZ and
MV − [Fe/H] relations we simulate Gaia parallaxes for 25 RR Lyrae stars in the Milky
Way.
In the Conclusions section we summarize the work done, whereas the Appendix con-
tains tables which are too long to be inserted in the main text of the thesis.
3
Chapter 1
The cosmological distance ladder
The cosmological distance ladder is a succession of different techniques by which as-
tronomers measure the distances to celestial objects. The cosmic distance ladder is built
by transfering geometrically measured distances to nearby stars to the far universe via mul-
tiple overlapping steps (Walker, 2012). In order to determine the distance to relatively close
objects the method of trigonometric parallax is being used. However, this geometrical
method is not applicable to derive accurate distance to the objects in other galaxies. In
order to do this one needs to apply the so-called primary distance indicators which could
be calibrated from observations in the Milky Way (MW) or from theoretical considerations
(Rowan-Robinson, 1985). After establishing the distances to nearby galaxies with primary
methods, one can apply them in order to calibrate the secondary distance indicators, which
have to be used up to distances where the Hubble Law connecting the distance to the reces-
sion velocity can be applied and cosmological parameters can be estimated.
1.1 Trigonometric parallax
The most direct distance measurement technique is the method of trigonometric parallax.
Due to the rotation of the Earth around the Sun, the position of the stars on the sky change
with season in a way that depends on the distance to the star and on its direction on the sky.
If the direction of the star lies in the plane of the Earth’s orbit, the star will appear to move
back and forth on a line in this plane by an amount of ±π, where π = re/d rad. Here d is
the distance of the star and re is the radius of the Earth’s orbit around the Sun. If the star
lies perpendicular to the plane of the Earth’s orbit, at the ecliptic pole, the star will appear
to move in a circle of angular radius π = re/d. If the star lies at ecliptic latitude be, it will
move in an eclipse of semimajor axis π = re/d and of semiminor axis π sin be. The quantity
5
1.1. TRIGONOMETRIC PARALLAX
π is called trigonometric parallax of the star, and it is usually measured in arcseconds (′′).
The distance to stars is often expressed in terms of the parallax they would give. The
unit 1 parsec (pc) is defined as the distance at which the star would give a parallax of 1
arcsec. The distance d in parsecs is therefore d = 1/π(′′).
Astronomers deal with enormous ranges of distances, so it is more convenient to use
logarithmic measurements. For this reason the so-called distance modulus is widely used to
describe the distance to the object. It is defined as:
µ = m−M = 5log(d) − 5, (1.1)
where d is the distance in pc, m is the apparent magnitude of the star, and M is the
absolute magnitude, which is the magnitude the object would have at a distance of 10 pc.
The first accurate measurements of the parallax of stars were made in 1838, when
Friedrich Wilhelm Bessel at the Königsberg Observatory in Prussia estimated π = 0′′.31±
0′′.02 for the star 61 Cygni. In 1939 Thomas Henderson found 1′′.16 ± 0′′.11 for α Cen-
tauri. Work on measuring parallaxes proceeded slowly. In 1878 parallaxes of 17 stars were
known, and by 1908 the number increased to 100. The Yale Parallax Catalog published
in 1952 (Jenkins, 1952) gives parallaxes for 5822 stars. However, for the majority of stars
the parallaxes were too small and not known accurately enough to give reliable distances.
To measure the parallaxes with a good accuracy, space telescopes are needed. That’s why
the astronomers developed a space experiment, devoted specifically to precision astrometry,
Hipparcos.
Hipparcos (High precision parallax collecting satellite) was a scientific mission of the
European Space Agency (ESA), launched in 1989 and operated until 1993. The spacecraft
was equipped with a single all-reflective, eccentric Schmidt telescope, with an aperture of
29 cm. The initial objectives of the mission were to determine parallaxes of ∼ 120000
stars to a precision of 2 milli-arcseconds (mas) for the core of the catalogue, along with the
astrometry to 10-20 mas and two-colour photometry for additional 400000 stars (the Ty-
cho experiment). An optimized scanning law allowed to cover the whole sky more or less
regularly in such a way that every object was observed from 25 to 70 times depending on
ecliptic latitude (Mignard, 1998). Regarding the photometry the number of individual ob-
servations per stars varied from 70 to 300. The resulting Hipparcos catalogue of ∼ 120000
stars with an astrometric accuracy of 1 mas or better for the brightest stars, was published
in 1997. Additionally, the lower-precision Tycho Catalogue of more than a million stars
6
CHAPTER 1. THE COSMOLOGICAL DISTANCE LADDER
was published at the same time, while the enhanced Tycho-2 Catalogue of 2.5 million stars
was published in 2000. A new reduction of the Hipparcos astrometric data was published
by van Leeuwen (2007), who claims improvement of accuracies to a factor 4 for nearly all
stars brighter than Hp=8 mag1.
More accurate trigonometric parallaxes are being obtained with the Fine Guidance Sen-
sor (FGS) instrument (Nelan, 2010) on board the Hubble Space Telescope (HST). Unfortu-
nately, the sample of objects, for which accurate HST parallaxes were obtained, is small.
The determination of unprecedentedly accurate parallaxes of a huge sample of objects is
expected with the ESA satellite Gaia (Perryman et al., 2001).
1.2 Gaia
Gaia is the ESA’s cornerstone mission launched using the Soyuz ST-B rocket from Kourou
in French Guiana on 19 December 2013. The satellite is designed to produce the most
accurate three-dimensional (3D) map of the MW to date (Perryman et al., 2001). Gaia is
located at the Lagrangian point L2 and scans the sky with two telescopes by continuously
spinning around the axis perpendicular to the two lines of sight. Each celestial object will
be observed on average 70 times during the five-year mission lifetime. Gaia will determine
the position, distance, and annual proper motion of 1 billion stars with the unprecedented
accuracy of about 20 µas at V ∼ 15 mag, and 200 µas at V ∼ 20 mag. The accuracy of
the Gaia parallaxes in comparison with Hipparcos is shown in Figure 1.1. For the brightest
objects the parallax errors are dominated by calibration errors and range from ∼ 5 to ∼ 14
µas. At the faint end the behaviour of errors as a function of V magnitude is dictated by
photon noise. As it could be seen in Fig. 1.1 at a given V magnitude, parallax accuracies
are higher for red stars. Accuracy predictions include a rough estimate of the effects of
radiation damage and a 20% margin (factor 1.2) to account for unmodelled effects. The
standard errors in position and proper motions can be derived by applying factors ∼ 0.7
and ∼ 0.5, respectively, to the parallax standard errors (Brown, 2013). Some millions of
stars will be measured by Gaia with a distance accuracy of better than 1 per cent; some 100
millions or more to better than 10 per cent.
1Hipparcos magnitude is defined by the passband of the Hipparcos main detection chain which ranges from340 to 850 nm.
7
1.2. GAIA
Figure 1.1 Accuracies of determination of parallaxes as a function of source brightness inthe V band for Gaia and for Hipparcos. Contours and dots show the Hipparcos parallaxerrors from van Leeuwen (2007). The lines show the predicted Gaia sky averaged parallaxstandard errors for an early (blue) and a late (red) spectral type star. The bands around theaverage relations reflect uncertain calibration errors at the bright side and the variation inthe sky coverage at the faint end. Figure is from Brown (2013).
8
CHAPTER 1. THE COSMOLOGICAL DISTANCE LADDER
The astrometric measurements are collected applying a wide photometric band (the Gaia
G band) which covers the range 330-1000 nm. Multi-colour photometry will be obtained for
all objects by means of low-resolution spectrophotometry. The photometric instrument con-
sists of two prisms: one is called RP for Red Photometer and covers the wavelength range
640-1000 nm, the second one, called BP (Blue Photometer), operates in the wavelength
range 330-680 nm.
Before the start of Gaia five-year science phase, the commissioning was performed. It
revealed some unexpected anomalies. One problem detected during commissioning was
associated with ice appeared on some parts of the optics, causing a temporary reduction in
transmission of the telescopes. Heating the affected optics in order to remove the ice has
largely solved this problem. Another issue is associated with “stray light”, which reaches
Gaia’s focal plane at a level higher than it was predicted before launch. This light appears to
be a mixture of light from the Sun finding its way past Gaia’s 10 m-diameter sunshield and
light from other astronomical sources. The effect on the performance of Gaia is negligible
for objects at magnitude V ∼ 15 mag and brighter, but a slight degradation in the positional
accuracy is seen for fainter stars, reaching 50% for objects at Gaia’s nominal faint limit of
V ∼ 20 mag. The phenomenon of stray light will also affect the accuracy to which stellar
brightnesses will be measured. Moreover, the impact of the stray light should be more
significant for faint stars seen by the Gaia’s Radial Velocity Spectrometer (RVS).
Further tests performed during commissioning have shown that it may be possible to
extend Gaia’s reach to stars fainter than V ∼ 20 mag, while at the bright end, software
changes make Gaia to be able to measure almost all of the brightest stars in the sky, previ-
ously considered too bright for such a sensitive system. Both of these extensions will need
further analysis before being applied. Finally, Gaia laser device called the “basic angle
monitor”, designed to measure the angle of separation between Gaia’s two telescopes to an
extremely high level of accuracy, shows that the detected variations in the basic angle are
larger than expected. These variations are caused by thermal changes in the payload as Gaia
spins. Further efforts are being made to measure and accurately calibrate the variations. Af-
ter extensive testing and analysis of the system both in space and on the ground, Gaia began
scientific operations on the 25 of July 2014.
The first intermediate catalogue of science data is expected to be released to the public in
2017. However, in the case of detection of rapidly-changing objects such as supernovae and
other transient events, open alerts are being issued as soon as possible. In fact, in September
9
1.3. VARIABLE STARS AS DISTANCE INDICATORS
2014 Gaia was announced to discover its first supernovae, Gaia14aaa in a distant galaxy.
Gaia is expected to provide a huge contribution to many fields of astronomy, such as
the structure and dynamics of the MW, stellar astrophysics, physics of the Solar system,
extragalactic astronomy and fundamental physics. Moreover, Gaia will provide valuable
samples of variable stars of nearly all types, including detached eclipsing binaries (EBs),
contact or semi-contact binaries, and pulsating stars (Paczynski, 1997). Among pulsating
stars are key distance indicators such as the Cepheids, the RR Lyrae stars and the long-
period variables (LPVs). A complete sample of objects will allow determination of the
frequency of variable objects and accurate calibration of the basic relations that allow to
use these variables as primary distance indicators (see Section 1.3). Estimated numbers
are uncertain, but suggest some 18 million variables in total, including 5 million periodic
variables, 2-3 million EBs, 2000-8000 Cepheids, 60000-240000 δ Scuti variables, 70000
RR Lyrae stars and 140000-170000 Miras (Eyer & Cuypers, 2000).
In order to investigate the performance of the Gaia satellite and the contents of the even-
tual end-of-mission catalogue, Gaia’s Data Processing and Analysis Consortium (DPAC)
has a group working on the simulation of several aspects of the Gaia mission. One major
product of this work is the Gaia Object Generator (GOG, Luri et al. 2014), designed to
simulate both individual Gaia observations and the full contents of the end-of-mission cat-
alogue. GOG includes a full mathematical description of the nominal performance of the
Gaia satellite, and is therefore capable of determining the expected precision in astrometric,
photometric and spectroscopic observations. In general, the precision depends on the ap-
parent magnitude of the star, its colour, and its sky position, which affects the number and
type of observations made (due to the Gaia scanning law). In this thesis work we use GOG
simulations in order to analyse the impact of Gaia on the determination of distances with
the RR Lyrae stars.
1.3 Variable stars as distance indicators
The trigonometric parallax is a powerful tool which allows to derive the distance by using
only geometrical principals. However, in order to determine the distance with some accu-
racy beyond ∼ 10 kpc one needs to apply indirect methods and use distance indicators.
Objects which are widely used as primary distance indicators are variable stars of differ-
ent types. A variable star is an object that shows a variation of luminosity (ranging from a
10
CHAPTER 1. THE COSMOLOGICAL DISTANCE LADDER
limit given by the instrument precision to magnitudes) within a time interval that is small
compared with the evolution time of the star.
Variable stars play a fundamental role in the context of the distance scale, since they
offer several advantages with respect to normal stars. The light variation makes the variable
stars to be more easily recognised than normal stars in the same evolutionary phase, even
when stellar crowding is significant. The most important observables of a variable star
are the period and the amplitude of the luminosity variation, that can be determined with
very high precision (the period in particular) and are both independent of uncertainties on
distance and interstellar extinction.
There are two classes of variable stars: intrinsic and extrinsic variables. The variability
of the former ones is connected with internal physical phenomena. This class of variables
includes pulsating stars and supernovae. Extrinsic variables show variability connected to
external causes and include EBs and pulsars. Among intrinsic periodic variable sources, an
important role is played by the radially pulsating variables.
Radially pulsating variable stars undergo periodic changes in radius and temperature
that are responsible for the change in luminosity. The pulsation period P is related to the
natural oscillation period of a star, which can be shown to be proportional to ρ1/2, where
ρ is the mean density of the star. This natural oscillation period is essentially the time
it would take for a star to collapse if the pressure support were suddenly removed. The
pulsation mechanism is related to variations of the opacity (the so-called κ mechanism) and
the adiabatic exponent in the ionization regions of the most abundant elements in the stellar
envelopes, namely H, He and He+, the so-called γ mechanism (Eddington 1926, Zhevakin
1953, Cox & Whitney 1958). As the driving mechanisms of pulsation are active in external
layers, the inner structure is not involved and can be neglected in pulsating models (King &
Cox 1968 and references therein). Radially pulsating stars share this driving mechanism as
demonstrated by the occurrence of the so-called instability strip, the almost vertical narrow
region in the colour-magnitude diagram (CMD) where most of the pulsators are located.
Stars in different evolutionary phases cross the instability strip at different luminosity levels
so that their observations in Galactic and extra-galactic systems allow us to trace stellar
populations of different ages. In particular: RR Lyrae stars and Type II Cepheids are the
oldest stars (age> 10 Gyr); the Anomalous Cepheids are currently thought to trace the
intermediate-age population (∼ 1-5 Gyr); the Classical Cepheids (CCs) and δ Scuti stars
are the youngest among radially pulsating variables (50-200 Myr).
11
1.4. CLASSICAL CEPHEIDS
In the following sections we will summarise the properties of some classes of variable
stars which are widely being used as distance indicators: CCs, RR Lyrae stars and EBs.
1.4 Classical Cepheids
Classical Cepheids are primary distance indicators that allow to link the local distance scale
to the cosmological distances needed to determine the Hubble constant (Clementini, 2009).
CCs are high-luminosity (−2 > MV > −7), radially pulsating variable stars, with periods
generally ranging from 1 to 100 days, and commonly associated with relatively young stellar
populations, such as those found in open clusters, disks of spiral or irregular galaxies. From
the stellar evolution point of view, these variables are intermediate-mass (3 − 12 M⊙) stars
that cross the instability strip during the core-helium burning phase. The light curve of a
CC in the LMC is presented in the left panel of Figure 1.2.
CCs are widely used as primary distance indicators because they follow a period-luminosity
(PL) relation, which is a two-dimensional projection of the higher-order period-luminosity-
colour (PLC) relation (Madore & Freedman, 2012). The PL relation was discovered by
Henrietta Swan Leavitt (1868-1921), who studied 2400 CCs, mostly located in the Small
Magellanic Cloud (SMC, Leavitt & Pickering 1912). The physical basis of the CC’s PL
relation is related to the above mentioned period-density relation coupled with the Stephan-
Boltzman law, and the assumption of the mass-luminosity (ML) relation predicted by stellar
evolution for intermediate-mass stars in the central He burning phase.
In order to estimate the slope of the PL relation, a statistically significant and homoge-
neous sample of CCs is needed. An extraordinary large amount of CCs was discovered in
the two Magellanic Clouds (MCs) by the microlensing surveys MACHO and OGLE. Udal-
ski et al. (1999) used fundamental mode pulsating CCs in the Large Magellanic and Small
Magellanic Clouds to derive the following PL relations:
V0(LMC) = −2.760logP − 17.042 (1.2)
with σ=0.159 mag
V0(SMC) = −2.760logP − 17.611 (1.3)
with σ=0.258 mag.
12
CHAPTER 1. THE COSMOLOGICAL DISTANCE LADDER
0 0.2 0.4 0.6 0.8 1
16
15.8
15.6
Figure 1.2 Left panel: Light curve of a CC in the LMC observed by the EROS-2 survey.Period, expressed in days, is from the EROS-2 catalogue. Right panel: Ks-band PL relationof CCs in the 30 Doradus field of the LMC from Ripepi et al. (2012). Black open and filledcircles show fundamental mode and first-overtone mode Cepheids, respectively. Blue filledcircles are fundamental mode CCs from Persson et al. (2004). The solid lines are least-squares fit to the data.
The derived slope is in good agreement with the slope of theoretical PL relations
computed by Caputo et al. (2000) from nonlinear convective pulsation models of CCs
(MV = −2.75logP − 1.37, σ = 0.18 mag).
The zero-point of the PL relation can be calibrated either using Galactic CCs, for which
absolute magnitudes are known from parallax measurements and/or Baade-Wesselink anal-
yses (for a general review of the method see, for example, Gautschy 1987) or, by assuming
a value for the distance to the LMC. In the latter case a robust distance determination for
the LMC is necessary. The HST Key Project (Freedman et al., 2001) used the slope of the
CC’s PL relations from Udalski et al. (1999) and a zero-point consistent with an assumed
distance modulus (m − M)0 = 18.5 mag for the LMC, to measure the distances to 31
galaxies in the range from 700 kpc to 20 Mpc. Estimated distances then served to calibrate
other, more far-reaching secondary distance indicators and to determine the Hubble constant
(Freedman et al., 2001).
Despite the fact that the CCs are successfully used to measure the distance up to 20 Mpc
or more, a number of basic questions concerning the PL relation lack an answer (Fouquè
13
1.5. RR LYRAE STARS
et al. 2003, Marconi et al. 2010). The theoretical explanation of the observational evidence
of a PL relation for CCs relies on the ML relation, which is significantly dependent on
several physical and numerical assumptions (Marconi et al., 2010). Thus, the uncertainties
of the ML relation reflect on the PLC relation’s coefficients and zero-point. Another issue
is a possible non-linearity of the PL relation and the existence of a break around 10 days
(Tammann & Reindl 2002, Tammann et al. 2002, Kanbur & Ngeow 2004, Sandage et al.
2004, Ngeow et al. 2008). Moreover, it is not definitely established whether the PL relation
is universal, and consequently, if the slope derived on the basis of LMC’s and SMC’s CCs
can be safely applied to other galaxies. In the last decades, many studies were devoted to
investigate the effect of metallicity on the coefficients of the PL relation. On the theoretical
side, linear and adiabatic models mostly suggest a negligible dependence of the CC’s PL
relations on chemical composition (Chiosi et al. 1993, Alibert et al. 1999, Saio & Gautschy
1998, Sandage 1999), while nonlinear convective pulsation models predict a significant
metallicity effect on the PL relations (Bono et al. 1999, Fiorentino et al. 2002, Marconi et
al. 2005). Some empirical studies support the nonlinear theoretical scenario (Romaniello
et al. 2005, 2008). Some of these issues can be resolved by using the PL relation in the
infrared passbands. The PL relation in the Ks passband of CCs in the LMC observed
with the near-infrared VMC survey (Cioni et al., 2011) is presented in the right panel of
Figure 1.2. It is well known that the intrinsic width of the CC’s PL relation decreases as a
function of increasing wavelength (e. g. Madore & Freedman 1991; McGonegal et al. 1982;
Caputo et al. 2000). The amplitude of pulsation in the infrared passbands is smaller than in
the visual one, so the mean magnitude could be determined more precisely. Moreover, in
the infrared bands the problem of reddening is less important and the effect of metallicity on
the PL seems to be smaller (Groenewegen & Oudmaijer 2000; Caputo et al. 2000; Marconi
et al. 2005). Therefore, the PL relation of CCs in the near-infrared passbands is a very
powerful tool to determine the distances to the LMC and other galaxies.
1.5 RR Lyrae stars
RR Lyrae stars are primary distance indicators located mainly in the halos of galaxies and
in globular clusters. RR Lyrae stars are old (age > 10 Gyr), low-mass (∼ 0.6 − 0.8 M⊙)
core-helium burning stars that lie within the instability strip on the horizontal branch (HB)
of the CMD.
14
CHAPTER 1. THE COSMOLOGICAL DISTANCE LADDER
0 0.2 0.4 0.6 0.8 1
19.5
19
18.5
18
0 0.2 0.4 0.6 0.8 1
19.5
19
18.5
Figure 1.3 Light curves of ab-type (left panel) and c-type (right panel) RR Lyrae stars ob-served by the EROS-2 survey in the LMC. Periods expressed in days are from the EROS-2catalogue.
The prototype star RR Lyrae in the constellation of Lyra was discovered in 1899 by
Williamina Fleming. In the following years a significant number of these pulsators were
observed in globular clusters by Bailey, who classified them on the basis of the period and
shape of the light curve. In particular, RR Lyrae stars were divided into ab-type (RRab),
which have asymmetric light curves, periods in the range from ∼ 0.4 to ∼ 1 day and am-
plitude in the visual band Amp(V ) steadily decreasing as the period increases, and c-type
(RRc) with amplitude ranging from 0.2 to 0.6 mag, sinusoidal shape of the light curves and
period ranging from ∼ 0.2 to ∼ 0.4 day. Examples of light curves of RRab and RRc stars
in the LMC are presented in Figure 1.3. According to the theory of stellar pulsation the
two types of RR Lyrae stars undergo pulsation in different modes. RRab stars pulsate in the
fundamental mode and RRc stars in the first-overtone mode. There is also a third type of
RR Lyrae stars, called double-mode or RRd stars, who undergo pulsation in both modes.
The RRd stars are particularly useful to obtain independent estimates of the stellar mass
(Petersen 1973; Bono et al. 1996; Bragaglia et al. 2001).
1.5.1 Metal abundance of RR Lyrae stars
The RR Lyrae stars are relatively low-mass stars, so the nucleosynthesis of significant
amount of elements heavier than carbon and oxygen is not expected during the lifetime
of these stars (Smith, 1995). Thus, the abundance of heavy elements in the atmosphere of
15
1.5. RR LYRAE STARS
the RR Lyrae stars reflects the abundance of heavy elements in the interstellar gas cloud
from which the stars were formed. This fact makes the RR Lyrae stars useful tracers of the
chemical history of the system they belong to.
In order to describe the iron (Fe) abundance of stars, the [Fe/H] notation is used. In this
notation, the ratio of Fe over hydrogen (H) in the photosphere of a star is related to that ratio
in the Sun:
[Fe/H] = log(Fe/H)star − log(Fe/H)⊙ (1.4)
The metallicity [Fe/H] of RR Lyrae stars ranges from ∼ −2.5 to ∼+0.2 dex.
The metal abundance of RR Lyrae stars is often measured with the ∆S index (Preston
1959). The spectral type of RR Lyrae stars as determined from the hydrogen Balmer lines
is generally later than the spectral type determined from the CaII K-line, and the latter
is generally weaker than expected on the basis of the Balmer line spectral classification.
Preston (1959) defined the ∆S index as the difference in tenths of spectral class between
the spectral type of a RR Lyrae at minimum light estimated from the hydrogen lines [Sp(H)]
and that estimated from the intensity of the CaII K line [Sp(K)]:
∆S = 10[Sp(H)− Sp(K)]. (1.5)
The [Fe/H] abundance is well correlated with the ∆S index, and a number of different cal-
ibrations of the ∆S index in terms of [Fe/H] abundance exist in the literature (e.g. Preston
1959; Jurcsik 1995; Gratton et al. 2004, etc.).
A few high resolution spectroscopic studies of elemental abundances of RR Lyrae stars
are also found in the literature (Butler et al. 1976, 1979; Clementini et al. 1995; Lambert
et al. 1996; Kolenberg et al. 2010; For et al. 2011; Kinman et al. 2012; Govea et al 2014,
Pancino et al. 2014, submitted to MNRAS). For variables in globular clusters, individual
metal abundances can be inferred from the accepted metallicities of the host clusters2.
Indeed, the most appropriate way to measure the metallicity of RR Lyrae stars is through
spectroscopy. Gratton et al. (2004) derived metal abundances of 98 RR Lyrae stars in the2A number of different metallicity scales exist in the literature. Among the most used ones are Zinn & West
(1984) (hereafter referred as ZW) scale which is based on a variety of integrated photometric and spectroscopicindices calibrated from the few echelle photographic spectra existing at the time; Carretta & Gratton (1997)scale which was derived from the analysis of a large sample (∼ 160) of bright giants in 24 globular clusters,whose chemical abundances were obtained from equivalent widths measured on high dispersion CCD spectra;and Carretta et al. (2009) scale (hereinafter, C09) that is based on the analysis of spectra of about 2000 redgiant branch (RGB) stars in 19 Galactic globular clusters. Specifically used for RR Lyrae stars is Jurcsik(1995) metallicity scale (hereafter referred as J95) based on both spectroscopic cluster abundances and ∆Smeasurements of cluster variables. J95 metallicity scale is valid both for globular clusters and field RR Lyrae
16
CHAPTER 1. THE COSMOLOGICAL DISTANCE LADDER
LMC from low resolution spectra by comparing the strength of the CaII K line with that of
the H lines, the derived metallicities are on a metallicity scale which is, on average, ∼ 0.06
dex more metal-rich than the Zinn & West (1984) scale.
However, when spectroscopical observations are not available or feasible, an estimate of
“photometric” metallicity could be inferred from the φ31 parameter of the Fourier decom-
position of RR Lyrae’s light curves. According to Simon & Teays (1982) the light curve of
a RR Lyrae star can be fitted with a Fourier function of the form:
m(t) = A0 +N∑
i=1
Aicos[iω0(t− t0) + φi] (1.7)
where m(t) is the star apparent magnitude at time of observation t, A0 is the average ap-
parent magnitude, N is the number of fitted terms, ω0 is the angular pulsation frequency of
the star (ω0 = 2π/P0), t0 is the time of maximum light, and Ai and φi are the amplitude
and phase coefficients of the individual Fourier terms. The shape of the light curves can be
quantified by the low order coefficients of the fit: Ri1 = Ai/A1 and φi1 = φi − iφ1. The
A1, A2 and the φ21, φ31 parameters of the Fourier decomposition can be used to classify
the RR Lyrae stars (see e.g., Simon & Teays 1982, Cacciari et al. 2005).
Jurcsik & Kovacs (1996) derived a relation between the Fourier parameter φ31 of the
V -band light curve of field ab-type RR Lyrae stars, the period and the star metallicity on
the Jurcsik (1995) metallicity scale:
[Fe/H] = −5.038 − 5.394P + 1.345φ31. (1.8)
Jurcsik & Kovacs (1996) introduced the so-called compatibility condition and defined
a deviation parameter DF :
DF = |Fobs − Fcalc|/σF , (1.9)
where Fobs is the observed value of the given Fourier parameter, Fcalc is its predicted
value from the other observed parameters, σF is the corresponding standard deviation. Dm
is the maximum of the deviation parameters {DF } and measures the regularity of the light
stars, and is related to the ∆S index through the relation:
[Fe/H]J95 = −0.190(±0.007)∆S + 0.027(±0.052) (1.6)
17
1.5. RR LYRAE STARS
curve. According to Jurcsik & Kovacs (1996) only if the light curve of the RRab star satis-
fies the compatibility condition Dm < 3 can Eq. 1.8 be used for a reliable estimate of the
star metal abundance [Fe/H]. However, Cacciari et al. (2005) adopted a relaxed compatibil-
ity condition, and found that a maximum value of 5 for Dm allows to increase the statistic
without affecting significantly the results. Kapakos et al. (2011) found that the criterion
Dm < 3 cannot lead to a robust sample of RRab stars without taking into consideration the
σDm . Thus they applied the criterion σDm < 3 and Dm − σDm < 3 in their analysis.
Morgan et al. (2007) found the relation between metallicity on the ZW metallicity scale,
φ31 and P for RRc stars:
[Fe/H]ZW = 52.466P 2 − 30.075P +0.131φ231 +0.982φ31 − 4.198φ31P +2.424 (1.10)
which has a standard deviation of 0.145 dex. Finally, Nemec et al. (2013) have derived a
new metallicity calibration of the φ31 parameter based on spectroscopic and photometric
properties of 41 RR Lyrae stars observed by the Kepler space telescope and derived P −
φ31 − [Fe/H] relations for RRab and RRc stars, separately. Since Nemec et al. (2013)
metallicity calibrations are derived using high dispersion spectra analysed with standard
reduction procedures, the derived metallicities are on the high dispersion spectroscopy scale
of Carretta et al. (2009).
For ab-type RR Lyrae stars the new calibration equation is:
[Fe/H] = b0 + b1P + b2φs31_kep+ b3φ
s31_kepP + b4(φ
s31_kep)2 (1.11)
The coefficients of equation (1.11) are: b0 = −8.65 ± 4.64, b1 = −40.12 ± 5.18, b2 =
5.96 ± 1.72, b3 = 6.27 ± 0.96, b4 = −0.72 ± 0.17, with rms of the fit of 0.084 dex. The
φs31_kep is the parameter of the sine Fourier decomposition in Kepler magnitudes which
can be derived from the φs31 in the Johnson V band by applying the equation:
φs31_kep = φs
31(V ) + (0.151 ± 0.026) (1.12)
For c-type RR Lyrae stars Nemec et al. (2013) derived the equation:
[Fe/H]C09 = b0 + b1P + b2φc31 + b3φ
c31P + b4P
2 + b5(φc31)
2 (1.13)
The coefficients of equation (1.13) are: b0 = 1.70 ± 0.82, b1 = −15.67 ± 5.38, b2 =
0.20 ± 0.21, b3 = −2.41 ± 0.62, b4 = 18.00 ± 8.70, b5 = 0.17 ± 0.04, and the rms error
of the fit was 0.13 dex. The φc31 is the parameter of the cosine Fourier decomposition in the
18
CHAPTER 1. THE COSMOLOGICAL DISTANCE LADDER
V band which could be derived from the V sine decomposition parameter by applying the
equation:
φc31 = φs
31 − π (1.14)
We will use Nemec et al. (2013) relations in 6 to derive photometric metallicities for the
RR Lyrae stars.
Di Fabrizio et al. (2005) measured photometric metallicities from the φ31 Fourier pa-
rameter for 29 LMC RRab stars and compared their values with the spectroscopic metal
abundances derived for these stars by Gratton et al. (2004). They found that the average
difference between photometric and spectroscopic metallicities is 0.30±0.07 dex, with the
photometric abundances being larger. This test provides an indication of the soundness of
photometric metallicities of RR Lyrae stars.
1.5.2 MV − [Fe/H] and PLKZ relations of RR Lyrae stars
RR Lyrae stars make useful distance indicators because of the existence of an absolute
magnitude-metallicity relation in the V band: MV − [Fe/H] (Sandage 1981a,b) and of a
period-luminosity-metallicity relation in the K band: PLKZ (Longmore et al. 1986, Bono
et al. 2003, Catelan et al. 2004, Sollima et al. 2008, and references therein).
In the past decades several authors studied the MV − [Fe/H] relation for RR Lyrae stars
using a number of methods, including synthetic Horizontal Branch models (Lee, 1994)
and the Baade-Wesselink method (Fernley et al., 1998a). Gratton et al. (2004) combined
spectroscopically determined metallicities with high accuracy photometry in the V band of
∼ 100 RR Lyrae stars in the LMC (Clementini et al., 2003) and derived the luminosity-
metallicity relation:
V0 = (0.214 ± 0.047)([Fe/H] + 1.5) + (19.064 ± 0.017), (1.15)
where V0 is the apparent dereddened average magnitude.
The slope of this relation is in a good agreement with the slope derived for the luminosity-
metallicity relation of RR Lyrae stars in the MW (Fernley et al., 1998a) and HB stars
in the globular clusters of M31 (Rich et al., 2005). This fact supports the idea that the
luminosity-metallicity relation of RR Lyrae stars is, in first approximation, linear and uni-
versal (Clementini, 2009).
The zero-point of the MV − [Fe/H] relation can be determined with a number of dif-
ferent techniques among which are: (i) the parallaxes of RR Lyrae stars in the MW; (ii)
19
1.5. RR LYRAE STARS
the calibration via globular clusters, whose distances are determined using absolute magni-
tudes of subdwarfs measured by the Hipparcos satellite; (iii) various theoretical and empir-
ical assumptions, such as the adoption of the value for the distance to the LMC. Benedict
et al. (2011) derived the zero-point MV = 0.45 ± 0.05 mag for [Fe/H]=−1.5 dex using
HST parallaxes of five MW RR Lyrae stars and adopting the slope from Gratton et al.
(2004). This value is about 0.2 mag brighter than the value of MV = 0.66 ± 0.14 mag
at [Fe/H]=−1.48 ± 0.07 derived by Catelan & Cortes (2008) for RR Lyrae itself, but has a
significantly smaller error.
There are theoretical and empirical suggestions that the MV − [Fe/H] relation is not
linear over the whole metallicity range (Marconi, 2009). The relation may also be affected
by a number of uncertain factors such as evolutionary effects, α-element enhancement, etc.
Finally, the determination of distances from analysis of field RR Lyrae stars observed in the
optical passbands depends on the reddening; this is the strongest driver for moving to the
infrared when at all possible. Three of the five galactic RR Lyrae stars with HST parallaxes
(Benedict et al., 2011) have reddening E(B−V ) ≥ 0.1 mag, so the zero-point is potentially
more robust in the infrared (Walker, 2012). The near-infrared PLKZ relation of RR Lyrae
stars has a list of other advantages in comparison with the visual MV − [Fe/H] relation.
First of all, the luminosity in the K passband is less dependent on metallicity. Moreover,
the light curves of RR Lyrae stars in the K band have smaller amplitudes and are more
symmetrical, hence the determination of the mean K magnitudes is more precise.
The near-infrared PLKZ relation of RR Lyrae stars was studied by several authors both
from a theoretical and an observational point of view. Longmore et al. (1986) pioneering
work was followed by Liu & Janes (1990), Skillen et al. (1993) and Jones et al. (1996). A
comprehensive analysis of the IR properties of RR Lyrae stars was performed by Nemec et
al. (1994).
Bono et al. (2003) derived the semi-theoretical relation:
MK = −2.101logP + (0.231 ± 0.012)[Fe/H] − (0.770 ± 0.044), (1.16)
Catelan et al. (2004) presented a theoretical calibration of the RR Lyrae PLKZ relation
based on synthetic horizontal branch models computed for several different metallicities,
fully taking into account evolutionary effects besides the effect of chemical composition.
They derived the relation:
20
CHAPTER 1. THE COSMOLOGICAL DISTANCE LADDER
Figure 1.4 PLK relation for RR Lyrae stars in the LMC cluster Reticulum. Open symbolsshow RRc stars after their periods have been fundamentalized by adding 0.127 to the loga-rithm of the period. Filled symbols are RRab stars, the line shows the theoretical predictionfrom Bono et al. (2003). Figure is from Dall’Ora et al. (2004).
MK = −2.353logP + 0.175logZ − 0.597 (1.17)
By using Eqs. 9 and 10 in Catelan et al. (2004) and assuming [α/Fe]∼ 0.3 (e.g., Carney
1996) we transformed Eq. 1.17 into the form:
MK = −2.353logP + 0.175[Fe/H] − 0.869 (1.18)
Dall’Ora et al. (2004) obtained the relation between apparent K magnitude and period
for 21 RRab and 9 RRc stars in the LMC globular cluster Reticulum.:
⟨K⟩ = (−2.16 ± 0.09)logP + (17.352 ± 0.025) (1.19)
with standard deviation of 0.03 mag.
Figure 1.4 shows the PLK relation derived by Dall’Ora et al. (2004). They used this
relation in combination with Eq. 1.16 from Bono et al. (2003) to derive (m − M)0 =
18.52±0.005(random)±0.117(systematic) mag for the distance modulus of Reticulum.
21
1.5. RR LYRAE STARS
Del Principe et al. (2006) obtained the PLKZ relation from the analysis of RR Lyrae
stars of different metallicities in the globular cluster ω Cen. Benedict et al. (2011) calibrated
the zero-point of Del Principe et al.’s relation using the HST parallaxes of five RR Lyrae stars
in the MW and obtained:
MK = (−2.71 ± 0.12)(logP + 0.28) + (0.12 ± 0.04)([Fe/H] + 1.58)
−(0.57 ± 0.02) (1.20)
Sollima et al. (2008) derived the PLKZ relation from the analysis of 544 RR Lyrae
variables in 15 Galactic clusters and in the LMC globular cluster Reticulum. Mean K
magnitudes were estimated by combining Two-Micron-All-Sky-Survey (2MASS, Cutri et
al. 2003) photometry and literature data. The zero-point was calibrated on RR Lyrae itself,
whose distance modulus was deried using the star trigonometric parallax by Benedict et al.
(2002). Sollima et al. (2008) provide the relation:
MK = (−2.38 ± 0.04)logP + (0.08 ± 0.11)[Fe/H]CG − (1.07 ± 0.11), (1.21)
where P is the fundamental-mode period, and the metallicity [Fe/H]CG is in the Carretta
& Gratton (1997) metallicity scale. By applying this relation to the K data from Dall’Ora et
al. (2004) the distance modulus of Reticulum was determined to be: (m−M)0 = 18.48±
0.11 mag (Sollima et al., 2008).
Szewczyk et al. (2008) obtained deep infrared J and K observations of five fields lo-
cated in the LMC bar. Using different theoretical and empirical PLKZ calibrations they
found the distance modulus of the LMC to be 18.58±0.03(statistical)±0.11(systematic)
mag.
Borissova et al. (2009) combined near-infrared photometry and spectroscopically mea-
sured metallicity for a sample of 50 field RR Lyrae stars in inner regions of the LMC, and
derived the relation:
MK = (−2.11 ± 0.17)logP + (0.05 ± 0.07)[Fe/H] − 1.05 (1.22)
Borissova et al. (2009) had 5 measurements in the K passband for most stars in their
sample. Templates from Jones et al. (1996) were used to fit the light curves of the RR Lyrae
stars and derive mean K magnitudes. The zero-point of the relation was calculated using
22
CHAPTER 1. THE COSMOLOGICAL DISTANCE LADDER
Figure 1.5 LogP vs. J0 and LogP vs K0 plots for field RR Lyrae stars in the LMC. As-terisks represent Szewczyk et al. (2008) data, open circles are data from Borissova et al.(2009). Solid lines show the best-fit relations obtained using only Borissova et al. (2009)data, dashed lines are for the combined samples. Figure is from Borissova et al. (2009).
the mean K magnitude, the reddening andthe trigonometric parallax of RR Lyrae itself,
from Sollima et al. (2008). By applying Eq. 1.22 Borissova et al. (2009) determined the
LMC distance modulus to be: (m−M)0 = 18.53 ± 0.13 mag.
Figure 1.5 shows the PLK relation obtained by Borissova et al. (2009) combining their
data with the data from Szewczyk et al. (2008). Comparing the PLK relation derived for
the RR Lyrae stars in the Reticulum cluster (Fig. 1.4) and to the relation for field LMC RR
Lyrae stars (Fig. 1.5) one can see that the spread is significantly smaller for the objects in the
cluster. It could be due to depth effects or, more likely, it could suggest that the metallicity
effect should be taken into account.
Metallicities in all the above relations are on, or close to the Zinn & West metallicity
scale, except for Eq. 1.21, which is on the Carretta & Gratton (1997) metallicity scale.
The PLKZ relation is a very powerful tool to measure distances. However, the PLKZ
23
1.6. ECLIPSING BINARIES
relations published in the literature often were derived from small samples of RR Lyrae
stars. Additionally, the small number of observations in the K band limited the determina-
tion of accurate mean K magnitudes. A large sample of RR Lyrae stars in the LMC with
12 or more epochs in the Ks band light curves is provided by the VMC survey (Cioni et
al., 2011). One goal of this thesis work was to derive a new PLKsZ relation based on
the VMC photometry. Another fundamental issue is the derivation of the zero-point of the
PLKZ relation. This problem will be solved when unprecedentedly accurate trigonometric
parallaxes for large numbers of RR Lyrae stars will be provided by Gaia. In this thesis we
present simulated parallaxes for bright RR Lyrae stars in the MW and use them to establish
the accuracy of the PLKZ and MV − [Fe/H] relations zero-points as it will be calibrated
with Gaia.
1.6 Eclipsing binaries
EBs are binary stars in which the orbit plane of the two stars lies nearly in the line of the
sight of the observer, so the components of the system undergo mutual eclipses. Examples
of the light curves of EBs are presented in Figure 1.6.
1.6.1 Classification of eclipsing binaries
The classification of EBs is based on the distance between components, relative to their
sizes. If the two components do not fill their Roche lobes, the system is considered to be
a detached binary. In a semi-detached binary one of the two components fills its Roche
lobe and mass transfer occurs. In contact EBs both stars fill their Roche lobes. To classify
contact and detached/semi-detached binaries analysis of the Fourier parameters and visual
inspection of the light curves are necessary.
Rucinski (1993) showed that a simple description of the light variation of binaries could
be obtained through the cosine Fourier decomposition∑
ai cos(2πiφ). In this decompo-
sition the coefficient a0 is the average magnitude of the model fit, a1 and a3 represent
the difference in depth between the two eclipses, a2 reflects the total amplitude of the bi-
nary variability and a4 is related to the eclipse “peakedness" that goes to zero for the light
curves of contact binaries. Hence, the combination of the two cosine coefficients a2 and a4
could serve as a separator of contact and non-contact (detached and semi-detached) binaries.
Namely, the curve described by the relation a4 = a2(0.125 − a2), where both coefficients
are negative, separates the regions of the contact and non-contact binaries on the a2 versus
24
CHAPTER 1. THE COSMOLOGICAL DISTANCE LADDER
lm0467n17850 P=4.324035 N=500
lm0447n7830 P=1.715561 N=490
lm0375k19793 P=2.158691 N=346
lm0366k19655 P=1.295471 N=303
lm0344m10932 P=2.077371 N=443
lm0211k9308 P=2.341696 N=420
Figure 1.6 Light curves in the REROS band of EBs observed in the LMC by the EROS-2survey. P - period (day), N - number of the observations. Figure is from Muraveva et al.(2014a).
a4 plane (Rucinski, 1993). Rucinski (1997) performed the Fourier analysis of the IC-band
light curves to extract a sample of the contact binaries from OGLE EBs in nine fields in
Baade’s Window.
However not only genuine contact binaries, but also variables with contact-like light
curves such as the ellipsoidal variables may be misclassified as contact binaries. Ellipsoidal
variability is observed in close binary systems when one or both components is (are) dis-
torted by the tidal interaction with the companion. The main reason of the variability is the
change of the projected areas on the sky because of the orbital motion of the components.
Large samples of ellipsoidal variables were published by Soszynski et al. (2004), who used
OGLE II and OGLE III photometry, and by Derekas et al. (2006), who used the MACHO
database. Since the light curves of contact binaries and non-eclipsing ellipsoidal variables
have similar shapes and could be easily mistaken, in the following analysis we adopt the
term “contact-binary-like” systems for all objects passed by the Fourier filter.
1.6.2 Eclipsing binaries as distance indicators
EBs can be used as distance indicators, since some fundamental stellar parameters can be
determined using geometrical constraints of the systems. Masses of components are esti-
25
1.6. ECLIPSING BINARIES
mated dynamically via radial velocities, radii from the eclipse durations and the temperature
ratio (strictly the surface-brightness ratio) from the eclipse depths. The radii and tempera-
ture together are used to measure the luminosity of the system. From the estimated luminos-
ity and observed fluxes the distances to the EBs can be determined. This method requires
photometric and spectroscopic data (see reviews by Andersen 1991; Torres et al. 2010) and
is used to measure the distances to nearby galaxies. Recently, Pietrzynski et al. (2013) used
EBs to measure a distance to the LMC which is considered to be accurate to 2 %.
EBs may serve as distance indicators even when spectroscopy is not available. W UMa
type stars are contact binary systems with orbital periods typically less than 1 day, com-
posed of main sequence turn-off stars (Rucinski, 1998). It was shown that this class of
binaries could be used as distance indicators since the size of the two components could
be determined from the orbital period, which in combination with the colour information
allows one to derive absolute magnitudes (Rucinski 1997, and references therein). Indeed,
Rucinski (1997) used the method to determine the distance to W UMa-type contact systems
in the Galactic Bulge.
While W UMa type stars in the Galaxy seem to be limited to periods P < 1.3−1.5 day,
massive, young, blue systems of W UMa type with longer orbital periods of 2-3 day exist
in the LMC (Rucinski, 1999). These objects may follow a PL relation. Rucinski (1999)
suggested the existence of a PL relation at maximum light in the visual band (Figure 1.7),
but with a large scatter, possibly due to unaccounted effects of the interstellar extinction.
One goal of this thesis was to check the existence of the PL relation for young massive
contact EBs in the LMC and the possibility of using this relation to determine the distance
to this galaxy.
26
CHAPTER 1. THE COSMOLOGICAL DISTANCE LADDER
Figure 1.7 Relation between the orbital period and the V -magnitude at maximum light forEBs in the LMC. Different symbols mark three colour index ranges: filled circles representextra-blue binaries, open circles - red binaries, semi-filled circles are moderately-blue sys-tems (see Rucinski 1999 for details). Lines represent linear fits to the extra-blue (solid line)and moderately-blue (dashed line) subsamples. Figure is from Rucinski (1999).
27
1.6. ECLIPSING BINARIES
28
Chapter 2
The Large Magellanic Cloud
2.1 Magellanic System
The Magellanic System (MS) is located at a distance of about 57 kpc (Cioni et al., 2000)
from the MW and is formed by the LMC, the SMC, the Bridge connecting them and the
Magellanic Stream, a trailing HI component. The LMC is a dwarf irregular galaxy, also
considered as a late type spiral system. The SMC is a dwarf irregular galaxy sometimes
referred to as a dwarf Spheroidal galaxy (dSph; Zaritsky 2000). The LMC has an inclination
angle of ∼ 35 deg (Nikolaev et al. 2004, Olsen & Salyk 2002, van der Marel & Cioni 2001),
but main structures of the galaxy lie reasonably close to the plane of the sky, while the SMC
forms an extended structure almost along the line of sight (Cardwell & Coulson, 1986).
Optical and infrared surveys of the MS show that the LMC and SMC are distinct objects
separated in space by a projected distance of ∼ 20 kpc. However, the HI distribution shows
a different picture.The MCs are connected by a low-metallicity bridge of gas and share a
common gaseous envelope (Putman et al. 2003, Brüns et al. 2005). The existence of such
features suggests that the LMC and the SMC are a binary interacting pair.
The Magellanic Stream is formed by HI gas and does not contain stars (Guhathakurta &
Reitzel, 1998). It trails behind the Clouds at least 150 deg across the sky (Braun & Thilker
2004, Nidever et al. 2010). The Stream has historically been explained as the product of
a tidal or hydrodynamical interaction between the MCs and the MW (Gardiner & Noguchi
1996, Mastropietro et al. 2005, Connors, Kawata & Gibson 2006). This picture is based
on the assumption that the MCs have experienced multiple close passages near the MW.
However, HST proper motion measurements of the MCs (Kallivayalil et al. 2006a; Kalli-
vayalil et al. 2006b) have challenged this model. These studies suggest instead that the
MCs have, at best, completed one obit around the MW, or that they may even be still on
29
2.2. STRUCTURE OF THE LMC
their first passage. Besla et al. (2010) introduced a model to explain the observed large-scale
gas morphology of the MS, according to which the Magellanic Bridge and Stream could be
explained through tidal interaction between the LMC and the SMC. Since the MW is not re-
sponsible for removing material from the system, this picture is consistent with the scenario
of the first infall of the MS towards the MW. There is evidence that the tidal interactions of
the MCs could also account for the internal structure of the LMC (Besla et al., 2012).
2.2 Structure of the LMC
The LMC has a diameter ∼ 4.3 kpc and contains one spiral arm and a bar. The LMC bar is
a long-standing puzzle because it is off-centered relatively to the dynamical centre. Using
relative distance measurements to Cepheids in the LMC, Nikolaev et al. (2004) showed that
the bar is located ∼ 0.5 pc in front of the main disc. There are also evidences that the bar
could be warped relatively to the disc plane, so the east and west ends are nearer the MW
than the middle part (Subramaniam 2003, Lah et al. 2005, Koerwer 2009). The bar is not
seen in the gas distribution (Kim et al., 1998) or as a site of ongoing star formation. Besla
et al. (2012) showed that the internal structure and kinematics of the LMC strongly favour a
scenario in which the MCs have recently (100-300 Myr ago) experienced a direct collision.
The LMC contains large (∼ 1 kpc in diameter) star-forming regions: 30 Doradus, located
slightly above the bar, and Constellation III, located close to the LMC spiral arm (Dolphin
& Hunter, 1998).
The structure of the LMC as traced by probes of different stellar populations was dis-
cussed in Moretti et al. (2014). In this paper we have compared the distribution of RR
Lyrae stars, "hot" eclipsing binary stars (HEBs) and CCs from the OGLE III, OGLE IV and
EROS-2 surveys (Figure 2.1). RR Lyrae stars (age ∼ 10 Gyr) have a larger density in the
central region of the LMC, but in general they are distributed smoothly and likely trace the
halo of the galaxy. On the contrary, CCs and HEBs are strongly concentrated towards the
LMC bar and spiral arm, and almost disappear in the peripheral areas. Fig. 2.1 shows that
distributions of CCs and HEBs are very similar, but HEBs (age∼ 12 Myr) are more sharply
concentrated toward recent star-forming regions (30 Doradus and Constellation III), while
CCs (age ∼ 50− 200 Myr) mostly follow the bar and spiral arm of the LMC. Since HEBs,
RR Lyrae stars and CCs trace different stellar populations, they serve as perfect tools to
study the internal structure of this galaxy.
30
CHAPTER 2. THE LARGE MAGELLANIC CLOUD
Figure 2.1 Distribution of RR Lyrae stars (upper-left), CCs (upper-right) and HEBs (cen-tral) in the LMC. Black points represent sources with OGLE data; red points are EROS-2variables that do not have an OGLE counterpart within 5′′. α0 = 81◦.0 and δ0 = 69◦.0.The sky coverage of the VMC survey (blue rectangles), OGLE III (red contour), OGLE IV(cyan contour) is shown. Green rectangles underline VMC tiles completely observed as ofJuly 2013. Figure is from Moretti et al. (2014).
31
2.3. DISTANCE TO THE LMC
2.3 Distance to the LMC
The LMC is the closest large satellite of the MW and the first step of the cosmic distance
ladder. The galaxy contains a large number of different distance indicators that allows its
distance to be determined through many independent techniques. However, in spite of the
large number of independent measurements of the last twenty years, a general consensus
on the LMC distance has not been reached yet. Furthermore, when pushing distance un-
certainties down to a few percent the effects of sample size, spatial distribution, depth and
geometry become important and properly accounting for the LMC internal structure be-
comes necessary.
Figure 2.2 from Benedict et al. (2002) shows an impressive summary of the different
values for the distance modulus of the LMC published during the ten years from 1992 to
2001. Values from 18.1 to 18.8 mag were reported in literature, with those less than 18.5
mag supporting the so-called “short” distance scale, and those larger than 18.5 mag, the
“long” one. During the last decades dramatic progress in the calibration of the different
distance indicators led the dispersion in the LMC distance modulus to shrink significantly,
thus extreme values such as those listed in Benedict et al. (2002) are not very often seen in
the recent literature (Clementini, 2009).
A number of analyses of the distances to the LMC as derived from different distance
indicators have been performed (Gibson 2000; Benedict et al. 2002; Clementini et al. 2003;
Schaefer 2008; De Grijs et al. 2014). Clementini et al. (2003) compared the LMC distances
obtained from Population I and Population II indicators and showed that all distance deter-
minations converge within 1σ error on a distance modulus (m − M)0 = 18.515 ± 0.085
mag. De Grijs et al. (2014) compiled 233 separate distance determinations, published from
1990 March to 2013 December, and concluded that the canonical modulus of (m−M)0 =
18.49 ± 0.09 mag may be used for all practical purposes. These results are consistent with
the recent determination of direct distances to eight long-period, late-type EBs in the LMC,
which is claimed to be accurate to ∼ 2% (Pietrzynski et al., 2013). These authors found
the distance to the LMC to be: DLMC = 49.97 ± 0.19(stat) ± 1.11(syst) kpc, which
corresponds to the distance modulus (m − M)0 = 18.494 ± 0.049 mag. However, this
result was called into question by Schaefer (2013) who, in addition to concerns on possible
bandwagon effects, also pointed out that Pietrzynski et al. (2013) distance for the LMC dif-
fers significantly from the average distance to four hot, early-type EBs, D=47.1±1.4 kpc,
32
CHAPTER 2. THE LARGE MAGELLANIC CLOUD
published by Guinan et al. (1998), Fitzpatrick et al. (2002, 2003), and Ribas et al. (2002).
Despite the large number of studies claiming to have determined independently the distance
to the LMC, systematic uncertainties remain. Moreover, there were significant concerns
about a possible “publication bias" affecting distances (Schaefer 2008, Rubele et al. 2012,
Walker 2012). In particular, Schaefer (2008) noted that from 2002 to 2007, 31 independent
papers reported new measurements of the distance of the LMC, and the new values clus-
tered tightly around the value (m−M)0 = 18.5±0.1 mag, adopted by the HST Key Project
on the extragalactic distance scale (Freedman et al. 2001). Schaefer (2008) considered the
effects of "publication bias" to be the most likely cause of the clustering of LMC distance
measurements. Improvements in the instrumentation over the past decade and a half have
allowed the Cepheid distance scale to be extended well beyond the Local Group. Measure-
ments with the HST FGS have provided a direct calibration via parallaxes of 10 Galactic
CCs (Benedict et al., 2007). HST parallaxes of five RR Lyrae stars in the MW were ob-
tained by Benedict et al. (2011). Gaia, the ESA cornerstone mission, successfully launched
on December 2013, will measure parallaxes of one billion stars with unprecedented accu-
racy. All these facts will likely reduce the importance of the LMC as the first rung of the
cosmic distance ladder. But the history shows that the systematic errors are inevitable. The
famous phrase: ”The Hubble Constant at any given time has always been known to 10 per-
cent, despite having changed over the period by a factor of 10" should not be forgotten. For
this reason the careful determination of the distance to the LMC is still crucially important,
since this galaxy provides a sanity check of the validity of the lower rungs of the distance
ladder (Walker, 2012).
This thesis work is focused on three types of distance indicators: CCs, HEBs and RR
Lyrae stars. There are several reasons of this choice. Firstly, how it was discussed in
Section 2.2, HEBs, CCs and RR Lyrae stars probe different stellar populations, hence, serve
as perfect tools to study the internal structure of the LMC. Secondly, these three types of
distance indicators follow relations which zero-points can be calibrated with fundamental
geometric methods. These calibrations will be greatly improved when Gaia parallaxes will
become available.
33
2.3. DISTANCE TO THE LMC
Baade-Wesselink Double-mode
Eclipsing binaries Globular Cluster Dyn. mods
High Amplitude d Scuti Long Period Variables
M Stars Luminosity Main Sequence fitting
Masers Mean V magnitude
Modelling Li-rich Ca stars Nonlinear Pulsation modelling Planetary Nebulae Luminosity
Red Clump Red Clump & RR Lyraes
SN 1987A Statistical parallaxes
Subdwarf fitting Tip of the Red Giant Branch
Trigonometric parallax White Dwarf cooling sequence
19.0018.7518.5018.2518.00 LMC Distance Modulus
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
16
17
18
19
20
21
22
23
24
25
26
27
28
29
30
31
32
33
34
35
3637
38
394041
42
43
44
45
46
47
47
48
4950
51
52
53
54
55
56
57
58
5960
61
62
63
64
65
66
67
6869
70
71
71
72
73
74
75
76
77
77
78
7980
8182
83
84
Figure 2.2 Determinations of the distance modulus of the LMC compiled by Benedict etal. (2002). Colors represent the various methods, numbers refer to individual investigations(see Table 10 in Benedict et al. 2002). The thick vertical line denotes the distance modulusadopted by the HST Distance Scale Key Project (Freedman et al., 2001) and the Type IaSupernovae Calibration Team (Saha et al., 1999). Results for the distance modulus of theLMC from Benedict et al. (2002) are in bold.
34
CHAPTER 2. THE LARGE MAGELLANIC CLOUD
2.4 LMC Surveys
In this thesis work we extensively use the near-infrared photometry being collected by the
VMC survey (Cioni et al., 2011) and visual photometry obtained by the EROS-2, OGLE III
and OGLE IV surveys.
2.4.1 EROS-2
EROS-2 (Expérience pour la Recherche d’Objets Sombres) is a microlensing survey (Tis-
serand et al., 2007) which monitored about 88 deg2 of the LMC discovering a large number
of CCs, RR Lyrae stars, binaries and LPVs, both in the centre and in the outer regions of the
galaxy. The survey was carried out with the Marly 1-m telescope at ESO, La Silla, from July
1996 to February 2003. Observations were performed in two wide passbands, the so-called
REROS band centered close to the I standard band, and the BEROS band intermediate be-
tween the standard V and R bands. The BEROS passband covers the wavelength interval
from 420 to 720 nm, the REROS passband covers the interval from 620 to 920 nm. EROS
magnitudes can be transformed to the Johnson-Cousins standard system to a precision of
∼0.1 mag, using the following equations from Tisserand et al. (2007):
REROS = IC (2.1)
BEROS = VJ − 0.4(VJ − IC) (2.2)
The detection of variable stars and the determination of periods (PEROS) were per-
formed by an automatic pipeline based on the Analysis of Variance (AoV) method and soft-
ware developed by Beaulieu et al. (1997) and Schwarzenberg-Czerny (2003) (see Marquette
et al. 2009 and references therein for further details). The left panel of Figure 2.3 shows the
(BEROS , BEROS−REROS) CMD obtained from the EROS-2 catalogue of the LMC candi-
date variables (red points). The candidate RR Lyrae stars were extracted by selecting in the
CMD objects with 18.46 < BEROS < 20.03 mag, and 0.05 < BEROS − REROS < 0.58
mag (blue points).
Candidates CCs were visually selected in the BEROS versus PEROS diagram on the ba-
sis of the PL relation of CCs. The right panel of Fig. 2.3 shows how the selection was per-
formed. The selected candidate CCs have EROS-2 periods in the range 0.89 < PEROS <
15.85 days, and BEROS magnitudes in the range 13.39 < ⟨BEROS⟩ < 17.82 mag. The
faint magnitude/short period limit allows to reduce the contamination of the candidate CCs
35
2.4. LMC SURVEYS
Figure 2.3 Left panel: BEROS versus BEROS-REROS CMD of LMC candidate variablesfrom the EROS-2 data (red points). A blue box marks the region populated by the RR Lyraecandidates. Right panel: distribution of the EROS-2 candidate variables in the LMC (redpoints) in the LogP versus BEROS plane. Blue points represent the candidate CCs. Figureis from Moretti et al. (2014).
by shorter period variables, such as the RR Lyrae stars, whereas the bright magnitude/long
period limit reflects the bright cut of the EROS-2 data available to us.
As part of the collaboration between the VMC and EROS-2 teams, REROS and BEROS
time-series photometry (and related errors), periods and mean magnitudes for 5800 can-
didate CCs and 16337 candidate RR Lyrae stars were kindly made available to us by the
EROS-2 team. We used these data in oder to study the CCs (see Chapter 3) and the RR
Lyrae stars (see Chapter 6) in the outer regions of the LMC. Moreover, visual inspection
of the light curves of candidate CCs showed that the sample contains also a large fraction
(1768) of EBs. These accidentally found EBs also became subject of this thesis research
(see Chapter 4).
2.4.2 OGLE
The Optical Gravitational Lensing Experiment (OGLE) is a wide-field sky survey started
in 1992. The main goal of this survey was to search for microlensing events (Soszynski et
al. 2008, and references therein). The observing strategy of the project, originally proposed
by Paczynski (1986), was the regular monitoring of brightness of about 200 million stars in
the MCs and Galactic bulge, on time-scales of at least two years, in order to detect lensing
36
CHAPTER 2. THE LARGE MAGELLANIC CLOUD
events connected with “dark halo” objects. As a byproduct, these observations provided
an enormous database of photometric measurements. OGLE photometry is in the standard
BJohnson, VJohnson and ICousins filters.
The first phase of the project (OGLE I) started in 1992 and lasted till 1995. The 1 m
Swope telescope at the Las Campanas Observatory, Chile, was used (Udalski et al., 1992).
The project was very successful (Udalski et al., 1993) but it suffered from limited availabil-
ity of telescope time. Therefore observations were performed only in the Galactic bulge, and
the covered area on the sky was relatively small. The second phase of the project (OGLE II)
was conducted between 1997 and 2000. The observations were performed with the new
1.3 m Warsaw Telescope dedicated to massive photometric surveys of dense stellar fields
(Udalski et al., 1997). As a byproduct, catalogues of thousands of Cepheids, RR Lyrae stars,
EBs and LPVs in the Galactic Bulge and the MCs were produced (Szymanski, 2005).
The OGLE III phase started on June 2001 with the 1.3 m Warsaw telescope equipped
with the new eight 2048 × 4096 CCD detector mosaic camera at the Las Campanas Ob-
servatory, Chile (Udalski, 2003). OGLE III catalogues are publicly available at the OGLE
website1 and contain 3361 CCs (Soszynski et al., 2008), 24906 RR Lyrae stars (Soszynski
et al., 2009), 26121 EBs (Graczyk et al., 2011) in the LMC and 4630 CCs (Soszynski et
al., 2010a), 2475 RR Lyrae stars (Soszynski et al., 2010b) and 6138 EBs (Pawlak et al.,
2013) in the SMC. For each object, the catalogues provide right ascension, declination,
mean Johnson-Cousins V , I magnitudes, period, I-band amplitude, along with the Fourier
parameters R21, φ21, R31 and φ31 of the I-band light curves (Soszynski et al., 2009).
The most extended area coverage of the MS with OGLE was obtained during the third
phase, however, a significant extension of the observed area is expected with OGLE IV.
Nowadays, only a small region containing the LMC South Ecliptic Pole (SEP) field, ob-
served with the OGLE IV, is publicly available. The so-called Gaia SEP (GSEP) is an area
of about 5.3 deg2 around the SEP, of which a central rhombus-shaped portion of 5 × 0.7
deg2 corresponds to the region that Gaia observed repeatedly during commissioning. The
OGLE collaboration made the GSEP field data available after only two years of observations
because this data could be potentially useful for the Gaia mission. The data set consists of
photometry in the V and I bands for 6789 variables, with a number of data points between
338 and 351 in the I band, and about 29 epochs in the V band. The catalogue of variables
in the GSEP field contains 132 CCs, 686 RR Lyrae stars, 2819 LPVs, 1377 EBs and 156
1http://ogle.astrouw.edu.pl/
37
2.4. LMC SURVEYS
Figure 2.4 Sky coverage of the LMC for EROS-2 (black), OGLE III (red) and the firstrelease of OGLE IV (cyan). VMC tiles are indicated in blue. Tiles already completed as ofJuly 2013 are labelled. α0 = 81◦.0 and δ0 = 69◦.0. Figure is from Moretti et al. (2014).
ellipsoidal variables.
The areas covered in the LMC by the EROS-2 (black), the OGLE III (red) and the
first release of OGLE IV (cyan) surveys are shown in Figure 2.4. EROS-2 provided so far
the largest coverage of the LMC, however, the EROS-2 team made available to us only
catalogues of “candidate" CCs and RR Lyrae stars. Therefore, visual inspection of the light
curves was necessary to validate the classification. Moreover, the EROS-2 observations are
performed in non standard passbands. Therefore, in our study we used the OGLE III data
whenever available (i.e. in the internal regions of the LMC), and the EROS-2 data in the
outer regions of the galaxy.
2.4.3 VMC
The VISTA for Magellanic Clouds near-infrared survey (Cioni et al., 2011) started in Novem-
ber 2009 and is expected to extend beyond the originally planed ∼ 5 years time span. The
main purpose of this survey is to study of the star formation history (SFH) and the 3D struc-
ture of the MS using both constant and variable stars. The strategy, main goals and first data
were presented in Cioni et al. (2011), first results for pulsating variables, based on the VMC
38
CHAPTER 2. THE LARGE MAGELLANIC CLOUD
Ks-band light curves, were described in Ripepi et al. (2012) for CCs in the LMC, Ripepi
et al. (2014a) for LMC Anomalous Cepheids (ACs), and Ripepi et al. (2014b, accepted to
MNRAS) for Type II Cepheids in the LMC. In Moretti et al. (2014) we present the strategy
of using CCs, RR Lyrae stars and EBs observed by VMC to study the LMC’s structure.
Muraveva et al. (2014a) used the VMC data to study the PL relations of the LMC EBs.
The VMC survey is observing ∼ 200 deg2 of the MS in the Y , J , Ks (λ = 1.02, 1.25 and
2.15 µm, respectively) passbands reaching a sensitivity limit on the stacked images close to
Vega magnitudes Y = 21.1 mag, J = 21.3 and Ks = 20.7 mag with a signal-to-noise ratio
S/N = 10. The survey covers the LMC area (116 deg2) with 68 tiles, the SMC (45 deg2)
with 27 tiles and the Bridge area (20 deg2) with 13 tiles. Two additional tiles cover 3 deg2
in the Stream. The VMC Ks-band are taken over 12 separate epochs (Cioni et al., 2011),
each epoch reaches a limiting magnitude of Ks ∼ 19.3 mag with a S/N ∼ 5. This limit
allows us to detect the minimum light of RR Lyrae stars in both the LMC and SMC. For
bright stars, the VMC survey is limited by saturation at Ks ∼ 11.4 mag. The VMC images
are processed by the Cambridge Astronomical Survey Unit (CASU) through the VISTA
Data Flow System (VDFS) pipeline. The reduced data are then sent to the Wide Field
Astronomy Unit (WFAU) in Edinburgh where the single epochs are stacked and catalogued
by the VISTA Science Archive (VSA; Lewis et al. 2010, Cross et al. 2012).
The VMC coverage of the LMC is shown in Fig. 2.4 (blue) from Moretti et al. (2014).
Tiles which were completely observed (12 epochs) as of July 2013, are labelled. One ad-
ditional LMC tile (tile 6_8) was completed after July 2013. The data for five LMC tiles
(namely tiles 8_8, 8_3, 6_6, 6_4 and 5_5) are now publicly available.
The time sampling of the VMC survey along with the significantly reduced amplitude
of the light variation in the Ks band allows us to derive mean Ks magnitudes with a great
precision (Ripepi et al. 2012, Ripepi et al. 2014a) but we have to rely in our research on
variable star catalogues from the optical microlensing surveys for the identification, coordi-
nates and pulsation properties, such as the period, epoch of maximum light and parameters
of the Fourier decomposition of the visual light curves (Moretti et al., 2014).
39
Chapter 3
Classical Cepheids in the VMC tileLMC 8_3
There are 11 tiles in the LMC that the VMC survey (Cioni et al., 2011) has completely
observed (12 epochs in the Ks band) as of October 2014. In this thesis we have analysed
the CCs in tile LMC 8_3, the RR Lyrae stars in tiles LMC 8_3 and 5_5, and the HEBs in all
LMC tiles, for which Ks data were available as of January 2014.
In this chapter we present results from the analysis of the EROS-2 candidate CCs lo-
cated in the LMC outer tile 8_3. The analysis of this tile was particularly useful to develop
the methods for the classification of candidate CCs from the EROS-2 catalogue. The lower
portion of tile LMC 8_3 is covered also by the OGLE III survey (Fig. 2.4), making it pos-
sible a direct comparison between the EROS-2 and OGLE III results. Periods, epochs of
maximum light, etc. derived in our analysis will be combined with the near-infrared data
from the VMC survey to determine the distance to tile LMC 8_3 from CCs.
3.1 EROS-2 data for candidate Classical Cepheids
The EROS-2 team provided us the catalogue and individual light curves in the BEROS
and the REROS passbands for 5800 candidate CCs in the LMC. Among them we selected
objects which are located in tile LMC 8_3. The coordinates of the center of the tile are: RA
= 05h : 04m : 53.952s , DEC= −66◦ : 15′: 29.880
′′(Cioni et al., 2011), the rotator angle
is -97.2489 deg. In order to extract objects located in this tile from the EROS-2 catalogue
and study the completeness of the EROS-2 catalogue with respect to the VMC catalogue
we performed the following steps:
41
3.1. EROS-2 DATA FOR CANDIDATE CLASSICAL CEPHEIDS
• We selected on the VISTA Science Archive website1 all sources located in tile LMC
8_3 (1024384 objects). This procedure set the range of coordinates (RA and DEC) to
use for extracting objects covering exactly the same area of the EROS-2 catalogue.
• We converted the RA and DEC coordinates of these objects to Cartesian (X and Y)
coordinates using the center of the tile as a reference.
• We calculated new X1 and Y1 coordinates by rotating the reference system such as:
X1 = Xcos(90 − α)− Y sin(90− α) (3.1)
Y 1 = Xsin(90− α) + Y cos(90 − α) (3.2)
where α is the rotator angle
• By plotting the new X1 and Y1 coordinates we derived a straight-looking tile in which
we were able to determine the range covered in each coordinate.
• We applied the same procedure to the EROS-2 catalogue. We converted the RA and
DEC coordinates of the candidate CCs from the EROS-2 catalogue to the Cartesian
(X and Y) coordinates using the center of tile LMC 8_3 as a reference. Then we
determined new X1 and Y1 coordinates of the objects by rotating the reference system
(equation 3.1, 3.2). When both catalogues were in the same system we were able to
extract objects from the EROS-2 catalogue which are located in the area of the VMC
tile LMC 8_3 by using the range of coordinates determined as described above.
By applying the described procedure we extracted 201 candidate CCs located in tile
LMC 8_3, 200 of them have counterparts in the VMC catalogue within a pairing radius of
1 arcsec. The counterpart of one object (EROS-2 id: lm0310k4094) was found within a
pairing radius of 1.2 arcsec. The comparison of the Ks and EROS-2 optical light curves
confirms the star counteridentification.
We analysed the EROS-2 light curves of the 201 candidate CCs with the GRaphical
Analyser of TIme Series (GRATIS) software developed at the Bologna Observatory by
P. Montegriffo (see, e.g., Clementini et al. 2000), and derived BEROS and REROS mean
magnitudes, amplitudes and epochs of maximum light in the BEROS passband for each
object. The results of our analysis are presented in Table 3.1. We corrected the period for
16 stars, since the EROS-2 catalogue provided aliases of the actual periods.1http://horus.roe.ac.uk/vsa/
42
CHAPTER 3. CLASSICAL CEPHEIDS IN THE VMC TILE LMC 8_3
ERO
S-2
idR
AD
ECPe
riod
⟨BEROS⟩
Amp(B)
Epoc
h(m
ax)
⟨REROS⟩
Amp(R)
Col
our
Type
(deg
)(d
eg)
(day
)(m
ag)
(mag
)B
EROS
(mag
)(m
ag)
(mag
)lm
0444
l123
69a
77.7
0978
-65.
7891
20.
6649
9517
.27
0.27
2451
189.
6194
16.9
90.
200.
28cA
Clm
0435
n136
03a
77.7
0995
-65.
7891
50.
6649
9717
.12
0.26
2451
556.
6837
16.8
80.
180.
24cA
Clm
0293
l260
6974
.964
89-6
6.90
412
0.89
7376
16.9
90.
2724
5233
4.56
0816
.71
0.18
0.28
cclm
0301
n220
2877
.124
42-6
6.53
385
0.90
4527
17.1
30.
0824
5230
5.65
3717
.30
0.08
-0.1
7sm
.am
lm04
36n2
1036
76.8
1620
-66.
2044
30.
9445
9317
.01
0.57
2451
126.
7584
17.2
80.
54-0
.27
bin
lm03
00l2
3623
75.5
1875
-66.
5668
70.
9549
2316
.55
0.30
2451
901.
7383
16.2
90.
210.
26cc
lm04
37k1
3766
77.1
5688
-65.
9986
50.
9643
8916
.97
0.25
2451
533.
6376
16.6
70.
180.
30cc
lm04
36m
1006
976
.660
67-6
5.98
062
0.96
6700
16.4
90.
4224
5147
6.66
4216
.72
0.41
-0.2
2bi
nlm
0437
m21
444
77.6
8774
-66.
0528
70.
9850
9916
.88
0.26
2450
332.
8638
16.6
10.
190.
27cc
lm03
12l1
1935
77.4
3583
-66.
8343
30.
9878
9616
.55
0.28
2451
100.
6816
14.7
70.
181.
78lp
vlm
0427
n127
8876
.053
93-6
6.15
369
1.02
4246
17.6
80.
2524
5145
4.87
2217
.80
0.22
-0.1
3bi
nlm
0300
l857
875
.763
46-6
6.45
715
1.02
7220
16.1
30.
0324
5255
1.69
6014
.97
0.02
1.16
lpv
lm04
24n1
4561
74.9
1334
-65.
8054
51.
0472
3516
.51
0.34
2450
342.
8891
16.7
90.
34-0
.28
bin
lm04
26n2
3242
75.0
2346
-66.
2171
81.
0473
6516
.42
0.36
2451
482.
6228
16.7
50.
34-0
.33
bin
lm03
03n1
5295
77.0
3270
-66.
8369
51.
0695
0317
.39
0.08
2451
060.
8754
17.7
10.
07-0
.31
sm.a
mlm
0427
k197
6675
.278
64-6
6.05
269
1.07
5378
16.6
80.
4724
5118
2.68
7216
.40
0.34
0.28
cclm
0310
k455
077
.559
31-6
6.27
774
1.08
5795
16.6
80.
3324
5188
9.62
7116
.43
0.24
0.25
cclm
0301
m26
336
76.8
7621
-66.
4116
51.
0907
8217
.63
0.12
2452
239.
5837
17.7
80.
15-0
.15
bin
lm04
25n2
6027
75.7
4082
-65.
8787
41.
0908
4917
.78
0.44
2451
510.
5912
17.9
20.
44-0
.15
bin
lm04
37k1
6072
77.2
4041
-66.
0147
11.
1042
4515
.95
0.07
2451
830.
7454
16.2
00.
08-0
.24
sm.a
mlm
0293
k197
8874
.662
97-6
6.71
494
1.11
7755
16.0
90.
0324
5171
6.92
6016
.32
0.03
-0.2
4sm
.am
lm03
10k1
5114
77.5
2638
-66.
3516
41.
1329
1817
.56
0.50
2451
645.
5360
17.7
60.
50-0
.20
bin
lm03
01m
1369
676
.886
49-6
6.32
851
1.16
0762
16.5
90.
3024
5147
2.65
5916
.30
0.21
0.29
cclm
0426
m23
482a
75.0
7795
-66.
0628
41.
1727
8714
.87
0.11
2450
418.
6526
15.2
20.
10-0
.34
sm.a
mlm
0437
n826
777
.381
03-6
6.11
499
1.17
6646
17.3
90.
2424
5162
3.56
3617
.54
0.23
-0.1
6bi
nlm
0303
l234
2876
.800
88-6
6.88
609
1.18
3669
17.5
00.
7324
5085
5.61
2817
.72
0.69
-0.2
2bi
nlm
0312
k155
2377
.480
35-6
6.73
194
1.18
8117
17.5
50.
2124
5177
2.85
0717
.53
0.18
0.02
bin
lm03
10k4
094
77.3
1567
-66.
2746
21.
2125
1416
.76
0.34
2451
266.
5345
16.4
40.
240.
32cc
lm03
02n1
2595
76.3
2740
-66.
8322
31.
2131
5116
.89
0.21
2452
535.
7713
17.1
80.
15-0
.29
bin
lm03
03n1
0523
77.2
0164
-66.
8071
21.
2463
2117
.54
0.44
2451
502.
6255
17.8
80.
44-0
.34
bin
43
3.1. EROS-2 DATA FOR CANDIDATE CLASSICAL CEPHEIDSlm
0302
l135
0475
.711
78-6
6.84
312
1.26
1500
16.4
30.
3524
5122
4.60
8016
.16
0.25
0.27
cclm
0436
k895
276
.366
02-6
5.96
754
1.27
5596
17.7
00.
1724
5078
4.83
0817
.83
0.14
-0.1
4bi
nlm
0437
n926
777
.580
30-6
6.12
241
1.28
0097
16.4
80.
2124
5149
7.71
4216
.15
0.15
0.32
cclm
0293
l140
8974
.996
18-6
6.83
478
1.29
2040
17.4
90.
1124
5031
7.85
9617
.74
0.11
-0.2
6bi
nlm
0291
m59
0575
.361
89-6
6.27
604
1.30
3899
16.3
20.
4024
5125
2.54
2516
.14
0.27
0.18
cclm
0293
n443
875
.103
26-6
6.77
718
1.31
5011
17.5
60.
0924
5115
6.78
8517
.82
0.08
-0.2
6sm
.am
lm04
26m
6757
75.1
0942
-65.
9426
61.
3727
8516
.36
0.14
2451
564.
5990
16.6
00.
12-0
.24
bin
lm04
27k7
569
75.4
8319
-65.
9596
11.
4235
2616
.32
0.58
2452
008.
5146
16.5
90.
54-0
.27
bin
lm04
36m
2067
5a76
.555
30-6
6.06
799
122.
4455
0016
.31
0.51
2450
226.
7490
14.1
30.
282.
18lp
vlm
0300
k223
3175
.895
90-6
6.40
058
1.48
1380
17.6
60.
3424
5135
3.90
4917
.92
0.36
-0.2
6bi
nlm
0300
k232
3375
.716
98-6
6.40
716
1.52
8732
15.5
90.
2224
5035
1.89
7215
.52
0.18
0.08
cclm
0426
n226
2075
.073
70-6
6.21
255
1.52
9313
16.1
20.
1024
5042
5.78
0816
.44
0.10
-0.3
2bi
nlm
0427
m21
459
75.7
9042
-66.
0647
91.
5465
4716
.67
0.30
2450
372.
7347
17.0
10.
29-0
.33
bin
lm03
01k1
2039
76.7
7238
-66.
3204
61.
5500
5815
.87
0.43
2451
934.
6566
15.6
10.
290.
26cc
lm04
24n1
5978
ab
75.1
8656
-65.
8146
91.
5609
3016
.64
0.27
2451
479.
6292
16.4
10.
210.
23cc
lm04
34m
2103
876
.544
71-6
5.69
327
1.58
5547
16.0
80.
1224
5040
4.78
4516
.33
0.12
-0.2
5bi
nlm
0435
l575
277
.272
69-6
5.73
683
1.59
7033
17.5
80.
5624
5162
3.56
3617
.75
0.54
-0.1
7bi
nlm
0305
k407
276
.493
98-6
6.97
811
1.61
9923
17.1
60.
0524
5114
9.64
0317
.29
0.05
-0.1
3sm
.am
lm04
25n1
5511
75.6
5717
-65.
8027
31.
6233
8417
.47
0.26
2451
627.
5233
17.6
90.
25-0
.23
bin
lm04
24n1
0133
74.9
7782
-65.
7724
61.
6353
9016
.06
0.13
2450
498.
6499
16.3
20.
11-0
.25
bin
lm04
27m
4029
75.9
0082
-65.
9288
21.
6363
0016
.06
0.28
2451
784.
7345
15.7
70.
190.
29cc
lm03
02n2
6730
76.2
3651
-66.
9413
21.
6639
4516
.35
0.26
2451
212.
7016
16.0
40.
190.
31cc
lm02
91l1
1728
74.9
6100
-66.
4698
11.
6706
6216
.88
0.30
2451
895.
7390
16.5
10.
220.
37cc
lm03
03m
1696
377
.037
60-6
6.69
697
1.70
2557
16.0
80.
2024
5260
4.76
2215
.90
0.14
0.18
cclm
0301
m21
301
76.9
4809
-66.
3780
41.
7099
1516
.04
0.18
2451
511.
6292
15.7
10.
120.
33cc
lm03
03k5
608
76.5
2968
-66.
6303
41.
7272
3716
.67
0.63
2451
642.
4916
16.4
10.
450.
26cc
lm02
91k2
0831
74.8
0414
-66.
3784
71.
7396
2716
.13
0.34
2452
245.
6216
15.7
10.
230.
42cc
lm04
36l1
4585
76.4
2263
-66.
1591
71.
7569
7115
.73
0.23
2451
830.
7454
16.1
10.
26-0
.38
bin
lm02
93k1
6840
74.6
4961
-66.
6982
31.
7725
0815
.86
0.36
2451
553.
6111
15.6
10.
240.
26cc
lm03
03k1
3861
76.7
6351
-66.
6787
91.
7728
4517
.01
0.10
2450
351.
8972
17.2
00.
10-0
.19
bin
lm02
91m
2186
975
.078
96-6
6.38
380
1.77
4816
17.2
10.
7024
5230
4.67
1717
.40
0.68
-0.1
9bi
nlm
0303
l196
8076
.454
61-6
6.86
658
1.79
3979
15.7
10.
3624
5122
4.60
8015
.51
0.25
0.19
cclm
0291
n743
6a75
.255
35-6
6.44
051
1.79
4205
16.1
40.
2624
5082
6.62
9315
.77
0.18
0.36
cc
44
CHAPTER 3. CLASSICAL CEPHEIDS IN THE VMC TILE LMC 8_3lm
0300
k545
075
.843
31-6
6.28
245
1.80
1747
15.7
20.
0824
5208
4.89
9116
.05
0.07
-0.3
3bi
nlm
0435
n218
9477
.627
52-6
5.84
829
1.80
1802
15.9
20.
3224
5187
8.63
6615
.65
0.23
0.27
cclm
0434
n101
5276
.507
05-6
5.77
485
1.81
4666
15.7
90.
3724
5260
9.67
8315
.52
0.26
0.27
cclm
0301
m24
570
76.8
5416
-66.
3999
91.
8215
2615
.75
0.37
2451
577.
6660
15.4
30.
260.
32cc
lm03
03n1
7856
76.9
2380
-66.
8528
51.
8277
1016
.23
0.12
2451
257.
5461
16.5
40.
11-0
.31
bin
lm04
24m
1510
475
.125
83-6
5.64
843
1.86
1021
15.8
40.
0724
5183
0.71
4216
.11
0.07
-0.2
7bi
nlm
0310
k155
2777
.598
90-6
6.40
988
1.87
2873
15.7
00.
2624
5042
4.83
3115
.41
0.17
0.29
cclm
0291
l253
4974
.751
74-6
6.55
471
1.87
4248
16.8
60.
1224
5182
6.71
3016
.93
0.12
-0.0
7bi
nlm
0310
l188
4877
.465
63-6
6.53
873
1.89
4299
15.7
80.
3324
5075
5.72
5415
.44
0.23
0.34
cclm
0293
l239
8274
.830
80-6
6.89
299
1.89
8197
15.8
20.
3424
5124
6.59
0015
.56
0.24
0.26
cclm
0312
k163
00a
77.3
7623
-66.
7373
61.
9069
0015
.83
0.34
2451
178.
8033
15.4
60.
250.
37cc
lm04
24n2
4516
75.0
5272
-65.
8827
51.
9153
8615
.39
0.08
2451
497.
6153
15.7
10.
11-0
.33
bin
lm03
01l2
2532
76.4
6532
-66.
5436
61.
9251
0115
.93
0.54
2452
265.
6419
16.1
30.
52-0
.20
bin
lm02
91m
1445
275
.271
95-6
6.33
402
1.92
8768
15.7
50.
2224
5155
5.59
1115
.48
0.15
0.26
cclm
0300
m12
894
76.1
8996
-66.
3303
01.
9441
9115
.68
0.19
2451
830.
7320
15.4
80.
140.
20cc
lm04
37m
1575
2a77
.722
49-6
6.00
990
1.96
6639
15.9
10.
2524
5037
6.74
4515
.60
0.16
0.31
cclm
0446
k151
42a
77.7
2235
-66.
0099
11.
9666
4516
.00
0.25
2451
556.
6964
15.6
20.
170.
38cc
lm03
03n1
3787
76.8
3778
-66.
8297
21.
9667
8015
.86
0.22
2452
129.
8190
15.6
60.
150.
21cc
lm03
02l5
812a
75.8
0726
-66.
7917
61.
9886
6015
.70
0.36
2450
835.
6299
15.4
20.
250.
28cc
lm03
01l2
1365
76.6
3322
-66.
5351
82.
0660
4215
.70
0.40
2452
183.
7002
15.3
70.
280.
33cc
lm03
03l2
2257
a76
.401
39-6
6.88
160
2.07
8516
15.6
20.
3024
5165
5.51
8915
.43
0.21
0.19
cclm
0302
l166
6075
.607
09-6
6.86
448
2.08
5372
15.6
90.
2424
5100
6.94
4215
.53
0.17
0.16
cclm
0293
k296
175
.031
27-6
6.61
400
2.09
5923
15.5
60.
3724
5188
9.59
4015
.32
0.26
0.24
cclm
0435
l259
6077
.217
29-6
5.87
469
2.19
0691
15.4
20.
0824
5038
9.80
4415
.70
0.07
-0.2
8sm
.am
lm03
00m
2557
176
.144
99-6
6.41
666
2.20
0747
15.6
10.
2024
5225
7.60
6515
.92
0.20
-0.3
1bi
nlm
0310
k108
1377
.436
35-6
6.42
755
2.21
1064
15.7
50.
2724
5087
9.56
9515
.37
0.19
0.37
cclm
0303
n124
0376
.834
86-6
6.82
148
2.23
4478
16.4
20.
3424
5155
1.64
1016
.69
0.35
-0.2
7bi
nlm
0301
n983
276
.878
18-6
6.45
832
2.24
2879
15.9
60.
1124
5116
9.71
4016
.10
0.11
-0.1
4bi
nlm
0300
m17
427
76.2
0188
-66.
3609
42.
2803
8415
.56
0.27
2452
683.
7579
15.3
10.
190.
25cc
lm03
05m
2711
76.8
7207
-66.
9661
42.
3576
0715
.88
0.87
2452
355.
5595
15.6
40.
610.
23cc
lm03
03k1
2257
76.7
9103
-66.
6688
02.
3681
9215
.47
0.32
2450
369.
8289
15.2
80.
220.
19cc
lm03
10k1
9198
77.3
8119
-66.
3809
22.
3822
4616
.07
0.73
2451
790.
8087
15.7
20.
510.
35cc
lm04
27m
1691
576
.034
40-6
6.02
195
2.38
2868
17.0
90.
3324
5144
7.75
0817
.41
0.31
-0.3
2bi
n
45
3.1. EROS-2 DATA FOR CANDIDATE CLASSICAL CEPHEIDSlm
0437
m92
6877
.337
03-6
5.96
636
2.39
2800
15.0
40.
1124
5133
9.93
7215
.29
0.10
-0.2
5sm
.am
lm04
35k1
0984
76.9
5992
-65.
6247
52.
4676
2416
.05
0.66
2452
304.
7042
15.6
90.
480.
36cc
lm04
27l1
0110
75.2
8292
-66.
1340
22.
4892
5416
.49
0.28
2451
467.
6728
16.7
50.
31-0
.26
bin
lm03
03m
2160
476
.860
80-6
6.72
639
2.50
7010
15.9
50.
1224
5125
7.54
6116
.29
0.13
-0.3
4bi
nlm
0291
k186
1874
.735
26-6
6.36
418
2.51
8067
16.1
90.
7224
5229
7.65
5215
.76
0.51
0.43
cclm
0291
k119
7974
.843
01-6
6.31
999
2.53
1380
15.7
00.
1824
5233
7.55
5415
.28
0.12
0.42
cclm
0434
l156
0576
.106
65-6
5.82
192
2.54
6594
15.5
10.
2824
5162
7.53
7415
.19
0.19
0.32
cclm
0312
k971
577
.363
94-6
6.66
809
2.56
5057
15.4
90.
3324
5078
8.84
9015
.08
0.24
0.41
cclm
0427
m16
528
75.7
7647
-66.
0217
82.
6082
2616
.01
0.26
2451
793.
7228
16.3
10.
26-0
.30
bin
lm04
25n8
591
75.9
3291
-65.
7526
62.
6152
9915
.95
0.67
2450
435.
7555
15.6
70.
480.
28cc
lm03
03n1
6128
76.8
2415
-66.
8436
42.
6211
9616
.76
0.50
2450
845.
7351
17.0
20.
49-0
.26
bin
lm03
00m
2600
976
.262
00-6
6.41
913
2.68
2304
15.8
70.
9524
5224
2.56
5115
.63
0.67
0.24
cclm
0301
k120
7876
.607
72-6
6.32
178
2.68
4560
15.6
80.
4224
5107
8.76
3115
.39
0.29
0.29
cclm
0305
m11
940
77.0
0428
-67.
0213
62.
6948
1915
.82
0.93
2451
948.
6978
15.5
90.
670.
23cc
lm04
35l7
382
76.9
1829
-65.
7501
42.
6972
9315
.81
0.97
2451
124.
7468
15.4
90.
690.
32cc
lm04
34k9
723
76.2
6202
-65.
6199
52.
7012
9715
.95
0.72
2450
410.
8229
15.5
90.
530.
37cc
lm02
91l5
438
74.8
6958
-66.
4304
72.
7036
8015
.75
0.60
2450
781.
6213
15.8
30.
60-0
.07
bin
lm03
10k1
7708
77.4
5565
-66.
3704
22.
7368
8316
.10
0.68
2451
201.
6079
15.7
00.
490.
40cc
lm04
27l9
939
75.4
6303
-66.
1315
42.
7714
8916
.20
0.57
2451
897.
7396
15.8
80.
460.
32cc
lm04
27k1
5685
75.5
2656
-66.
0762
92.
7915
9515
.55
0.11
2451
398.
8270
15.8
70.
12-0
.32
bin
lm03
10l1
9242
77.4
7706
-66.
5420
72.
8100
2416
.05
0.64
2451
886.
6343
15.6
50.
460.
41cc
lm03
05k7
040
76.5
2476
-66.
9954
22.
8617
4015
.98
0.51
2451
571.
6250
15.5
90.
370.
39cc
lm04
24n2
3353
75.0
9632
-65.
8668
92.
8693
1214
.65
0.28
2450
396.
7221
15.0
40.
32-0
.38
bin
lm03
03l6
182
76.4
9645
-66.
7874
02.
8947
1315
.73
0.89
2450
419.
5964
15.4
90.
590.
24cc
lm04
27n7
395
75.9
9907
-66.
1070
62.
8991
4615
.94
0.66
2451
606.
5799
15.6
20.
460.
32cc
lm03
00k8
884
75.7
5457
-66.
3069
62.
9218
3416
.61
0.31
2450
812.
8682
16.8
90.
26-0
.28
bin
lm04
26n1
7949
75.1
0564
-66.
1767
92.
9246
2816
.23
0.11
2451
872.
6350
16.5
40.
11-0
.31
bin
lm03
03m
5318
76.9
2088
-66.
6270
42.
9260
8216
.82
0.31
2451
920.
6912
17.1
00.
29-0
.27
bin
lm03
03k2
0577
76.6
5658
-66.
7190
82.
9313
1215
.93
0.61
2451
082.
8328
15.6
20.
440.
30cc
lm04
35n9
522
77.6
7406
-65.
7609
12.
9339
4415
.85
0.52
2450
410.
8229
15.5
40.
360.
31cc
lm03
03m
5774
76.9
8484
-66.
6292
42.
9576
1615
.71
0.63
2450
776.
7430
15.5
30.
430.
18cc
lm04
37l1
2785
77.2
8106
-66.
1555
52.
9638
8815
.96
0.66
2451
625.
5553
15.5
90.
480.
37cc
lm04
36n1
8193
a76
.755
75-6
6.18
253
3.00
0081
15.8
10.
8124
5032
1.57
7215
.50
0.58
0.32
cc
46
CHAPTER 3. CLASSICAL CEPHEIDS IN THE VMC TILE LMC 8_3lm
0426
n224
58a
74.9
9331
-66.
2112
43.
0011
7215
.87
0.72
2451
786.
7259
15.5
60.
390.
31cc
lm02
91k2
974
74.8
3436
-66.
3202
63.
0488
6316
.01
0.71
2451
455.
7233
15.4
20.
460.
59cc
lm04
37l7
188
76.9
3822
-66.
1091
53.
0622
7815
.94
0.63
2451
317.
4928
15.5
40.
440.
41cc
lm03
10l9
678
77.4
4955
-66.
5960
73.
0902
7315
.03
0.22
2452
247.
8307
14.6
80.
150.
35cc
lm04
35k1
6509
77.1
8997
-65.
6611
53.
0914
2215
.79
0.54
2451
329.
4786
15.4
60.
410.
33cc
lm03
00m
5551
76.0
1798
-66.
2797
13.
0954
4015
.87
0.60
2451
595.
6926
15.6
00.
430.
26cc
lm03
03k8
191
76.5
7712
-66.
6457
23.
1133
8715
.83
0.69
2451
905.
7471
15.5
60.
490.
27cc
lm03
01l8
214
76.5
8141
-66.
5965
53.
1231
5815
.91
0.66
2450
800.
6827
15.4
70.
470.
43cc
lm02
91m
2221
575
.078
76-6
6.42
292
3.12
7545
15.8
10.
6524
5249
5.81
3715
.43
0.46
0.39
cclm
0436
l797
276
.307
73-6
6.10
797
3.12
8903
15.7
30.
7924
5200
1.55
5215
.36
0.56
0.36
cclm
0436
l209
2476
.071
18-6
6.20
891
3.14
0133
16.1
10.
4524
5268
1.74
4715
.70
0.30
0.41
cclm
0300
k130
8175
.733
68-6
6.33
645
3.14
8857
15.8
70.
3224
5157
7.66
6015
.53
0.23
0.34
cclm
0427
n176
7675
.681
83-6
6.19
575
3.16
7981
15.7
60.
8224
5246
6.88
1715
.45
0.58
0.31
cclm
0301
n160
4976
.805
37-6
6.49
814
3.18
6794
15.2
90.
3124
5107
5.84
6314
.92
0.23
0.37
cclm
0300
l988
375
.660
61-6
6.46
650
3.18
8358
16.0
00.
3324
5111
0.76
0915
.58
0.24
0.42
cclm
0303
k193
4176
.736
29-6
6.71
116
3.19
3448
15.7
00.
7524
5175
6.86
0315
.47
0.54
0.23
cclm
0434
k243
1576
.448
97-6
5.72
779
3.20
7143
15.7
50.
7524
5134
2.93
8015
.38
0.54
0.37
cclm
0444
k211
8877
.724
76-6
5.69
096
3.24
5950
15.9
40.
6224
5158
3.67
5615
.56
0.45
0.38
cclm
0301
n144
2276
.953
64-6
6.48
692
3.26
4528
15.7
00.
7724
5112
5.62
8415
.34
0.54
0.36
cclm
0435
k200
2377
.255
56-6
5.68
476
3.28
1595
16.6
80.
1924
5037
2.76
0716
.90
0.22
-0.2
2bi
nlm
0435
n137
7877
.560
30-6
5.79
180
3.28
6657
15.7
00.
6924
5258
2.62
9915
.39
0.48
0.31
cclm
0436
l190
0776
.280
93-6
6.19
386
3.30
1123
14.9
60.
0524
5224
0.57
5415
.26
0.05
-0.3
0bi
nlm
0437
k165
8676
.911
84-6
6.02
031
3.32
7489
16.0
10.
4824
5190
1.74
7215
.59
0.34
0.42
cclm
0301
k175
1376
.717
01-6
6.35
814
3.32
8361
16.0
10.
5724
5176
3.89
4115
.66
0.42
0.35
cclm
0300
m80
1076
.021
62-6
6.29
691
3.37
7967
15.8
70.
4524
5157
5.66
2815
.55
0.32
0.32
cclm
0301
m60
2576
.831
90-6
6.27
650
3.41
2130
15.7
50.
8024
5149
1.64
3015
.43
0.56
0.32
cclm
0424
m26
545
75.0
6331
-65.
7273
83.
5094
4415
.69
0.83
2451
908.
7288
15.3
50.
590.
34cc
lm03
10l1
8849
77.5
5575
-66.
5834
73.
5187
8515
.75
0.68
2451
067.
7701
15.3
30.
490.
41cc
lm04
35l2
4878
76.9
1970
-65.
8690
03.
5407
3915
.76
0.66
2452
605.
7595
15.3
70.
470.
39cc
lm04
36k1
1123
76.4
2184
-65.
9850
43.
5992
9915
.69
0.61
2451
951.
6654
15.3
50.
430.
34cc
lm04
35l1
1832
77.2
6535
-65.
7781
63.
6301
8615
.85
0.30
2452
096.
8743
15.4
50.
220.
41cc
lm03
03l2
4720
76.7
1642
-66.
8940
63.
6306
6516
.40
0.05
2451
920.
6912
16.6
20.
05-0
.22
sm.a
mlm
0425
n188
7475
.938
26-6
5.82
298
3.64
9476
15.6
50.
8324
5231
5.63
1215
.35
0.59
0.30
cc
47
3.1. EROS-2 DATA FOR CANDIDATE CLASSICAL CEPHEIDSlm
0303
m26
388b
77.0
9012
-66.
7525
83.
7004
8215
.38
0.31
2451
116.
8084
15.2
30.
230.
15cc
lm03
00k1
5119
75.6
4848
-66.
3508
93.
7058
0015
.73
0.42
2451
153.
6115
15.3
50.
310.
38cc
lm04
27l7
011
75.4
3113
-66.
1062
13.
7350
4415
.53
0.79
2452
259.
5869
15.1
90.
550.
35cc
lm02
91l4
891
75.0
0036
-66.
4261
43.
7518
2915
.15
0.51
2450
838.
6385
15.4
30.
50-0
.27
bin
lm03
03m
3523
76.8
6127
-66.
6162
23.
7564
9415
.62
0.54
2450
879.
5630
15.3
70.
380.
25cc
lm03
02k1
5867
75.6
5471
-66.
7497
53.
8328
0915
.50
0.73
2451
255.
5600
15.1
30.
530.
38cc
lm04
37m
3722
77.5
2490
-65.
9244
33.
8936
8715
.69
0.32
2451
595.
7028
15.3
10.
230.
38cc
lm04
36k1
3349
76.2
3076
-66.
0033
73.
9163
6215
.67
0.61
2451
761.
8185
15.2
70.
440.
40cc
lm04
37l1
4075
77.2
0916
-66.
1657
83.
9650
0015
.70
0.47
2451
306.
5146
15.2
80.
330.
41cc
lm03
03n1
9840
77.1
9733
-66.
8618
83.
9681
6815
.53
0.72
2450
532.
5716
15.3
10.
510.
22cc
lm04
37n1
8565
77.6
8727
-66.
2021
63.
9726
6415
.76
0.66
2450
763.
7960
15.4
20.
470.
35cc
lm03
00m
2201
975
.954
69-6
6.39
246
3.98
6529
16.3
40.
4424
5146
8.61
7416
.62
0.46
-0.2
8bi
nlm
0303
n114
62a
76.8
4417
-66.
8156
74.
0034
1415
.55
0.53
2452
582.
6163
15.2
60.
370.
29cc
lm04
35m
2108
877
.427
68-6
5.68
669
4.05
0212
15.6
00.
4224
5183
3.73
9815
.20
0.31
0.40
cclm
0303
n141
1076
.823
39-6
6.83
168
4.24
0275
15.5
40.
6024
5112
5.62
8415
.26
0.42
0.28
cclm
0436
n217
7576
.611
75-6
6.21
120
4.32
5470
15.4
50.
3324
5124
6.62
7715
.15
0.28
0.30
cclm
0436
l174
6576
.050
97-6
6.23
806
4.37
7315
14.7
10.
1224
5232
7.61
6915
.00
0.13
-0.2
9sm
.am
lm03
10k1
9077
77.5
7698
-66.
3797
74.
3908
8015
.48
0.47
2450
369.
8365
15.0
60.
340.
41cc
lm03
03n1
9424
77.0
5204
-66.
8607
84.
4607
3315
.46
0.65
2451
844.
7158
15.2
00.
450.
26cc
lm03
00n1
8729
76.0
9649
-66.
5252
74.
4841
9315
.63
0.38
2451
563.
6306
15.2
40.
270.
40cc
lm03
01n2
1884
76.8
2732
-66.
5812
44.
5081
6115
.43
0.66
2450
855.
6128
14.9
90.
470.
44cc
lm03
00k1
4043
75.5
9119
-66.
3434
04.
6050
9915
.49
0.55
2452
207.
5989
15.1
30.
390.
36cc
lm04
36n2
2963
76.5
6901
-66.
2204
04.
6621
9115
.44
0.71
2451
899.
7779
15.0
60.
490.
38cc
lm04
36k1
6816
76.1
8391
-66.
0304
94.
7514
1915
.46
0.25
2450
756.
7592
15.0
30.
180.
42cc
lm04
27l1
2767
75.2
7200
-66.
1554
44.
8059
3215
.88
0.13
2451
815.
7447
16.1
50.
13-0
.27
bin
lm04
25n1
4050
76.0
3249
-65.
7895
14.
8192
0415
.36
0.39
2450
846.
7634
15.0
30.
280.
33cc
lm04
36n2
3124
76.8
2989
-66.
2207
34.
8710
8015
.47
0.67
2451
492.
6289
15.1
00.
480.
37cc
lm04
26n2
3478
75.1
8067
-66.
2184
94.
9366
4416
.27
0.10
2451
751.
9015
16.2
40.
090.
04sm
.am
lm04
27k1
3855
75.5
5629
-66.
0060
55.
0164
6915
.64
0.45
2451
948.
6800
15.8
90.
43-0
.25
bin
lm04
27k7
505
75.4
2766
-65.
9593
95.
1229
6415
.17
0.11
2452
355.
5460
15.4
40.
13-0
.27
bin
lm04
27m
1369
775
.899
42-6
6.07
558
5.60
6188
15.0
80.
5924
5151
0.59
1214
.76
0.41
0.33
cclm
0427
n162
72a
76.0
3168
-66.
1820
56.
0037
4014
.97
0.12
2451
564.
5990
15.2
70.
12-0
.30
bin
lm03
03k2
3599
76.5
7203
-66.
7373
16.
4630
8515
.36
0.43
2451
038.
8223
15.5
90.
41-0
.23
bin
48
CHAPTER 3. CLASSICAL CEPHEIDS IN THE VMC TILE LMC 8_3lm
0427
n121
2275
.865
53-6
6.14
977
7.19
4033
15.4
80.
1824
5212
3.84
1915
.77
0.20
-0.2
9bi
nlm
0435
m12
381
77.5
5651
-65.
6277
47.
6965
5115
.87
0.62
2451
888.
6354
16.0
40.
57-0
.17
bin
lm04
34k8
023
76.2
3518
-65.
6071
88.
1263
9614
.54
0.70
2451
341.
9322
14.1
10.
510.
43cc
lm04
36k1
1112
76.3
8695
-65.
9850
011
.331
810
14.3
90.
0824
5256
2.67
7214
.11
0.06
0.27
sm.a
mlm
0436
m12
100a
76.7
5148
-65.
9970
610
9.89
9010
16.1
70.
5124
5026
2.48
3614
.29
0.21
1.88
lpv
lm03
04m
5953
75.9
4165
-66.
9901
22.
7122
2116
.03
0.67
2450
800.
6827
15.6
60.
490.
36cc
Tabl
e3.
1:Pr
oper
ties
ofca
ndid
ate
CC
sin
tile
LMC
8_3
(Col
umn
1:ER
OS-
2id
entifi
catio
nnu
mbe
r;C
olum
n2:
Rig
htas
cens
ion
from
the
ERO
S-2
cata
logu
e;C
olum
n3:
Dec
linat
ion
from
the
ERO
S-2
cata
logu
e;C
olum
n4:
Perio
dfr
omth
eER
OS-
2ca
talo
gue
(a-
Star
sfo
rw
hich
ane
wpe
riod
estim
ate
was
deriv
ed.
See
text
for
deta
ils;b
-Dou
ble-
mod
eC
Cs,
the
first
perio
d,de
rived
with
GR
ATIS
,is
give
n.Se
ete
xtan
dTa
-bl
e3.
2fo
rde
tails
);C
olum
n5:
Mea
nm
agni
tude
inth
eB
EROS
band
;C
olum
n6:
Am
plitu
dein
theB
EROS
band
;Col
umn
7:Ep
och
ofm
ax-
imum
light
inth
eB
EROS
band
;C
olum
n8:
Mea
nm
agni
tude
inth
eR
EROS
band
;Col
umn
9:A
mpl
itude
inth
eR
EROS
band
;Col
umn
10:
Col
ourB
EROS−
REROS
;C
olum
n11
:C
lass
ifica
tion:
cc-
confi
rmed
Cla
ssic
alC
ephe
ids,
cAC
-can
dida
teA
nom
alou
sC
ephe
ids,
bin
-bin
ary
star
s,sm
.am
-sm
alla
mpl
itude
varia
bles
,lpv
-lon
gpe
riod
varia
bles
).
49
3.2. CLASSIFICATION OF CANDIDATE CLASSICAL CEPHEIDS
EROS-2 id P1,GRATIS P2,GRATIS P2/P1,GRATIS P1,OGLE III P2,OGLE III P2/P1,OGLE III
(day) (day) (day) (day)lm0424n15978 1.560930 1.135416 0 .7274 - - -lm0303m26388 3.700482 2.653466 0.7171 3.700349 2.653591 0.7171
Table 3.2 Double-mode CCs in tile LMC 8_3. (Column 1: EROS-2 identification of thestar; Column 2: First period derived with GRATIS; Column 3: Second period derived withGRATIS; Column 4: Ratio of the periods; Column 5: First period from the OGLE IIIcatalogue; Column 6: Second period from the OGLE III catalogue; Column 7: Ratio of theperiods from OGLE III).
By analysing the light curves with GRATIS we discovered two double-mode pulsators,
namely lm0303m26388 and lm0424n15978. For lm0303m26388 our second periodicity
is also confirmed by the OGLE III survey, while for lm0424n15978 there is no OGLE III
counterpart. Information about these two objects is presented in Table 3.2.
3.2 Classification of candidate Classical Cepheids
The visual inspection of the light curves of the 201 candidate CCs returned a sample of 126
bona-fide CCs, 58 EBs, 13 variables with small amplitudes (generally around 0.1 mag or
lower) and 4 LPVs. The latter accidentally fall in the sample of the candidate CCs, based
on the PEROS and BEROS values, because their EROS periods are aliases of the actual
periods, which are usually in the range from tens to thousands of days for LPVs. In the
sample of confirmed Cepheids we have also found two candidate Anomalous Cepheids:
lm0435n13603 (P=0.664997 days) and lm0444l12369 (P=0.664995 days). These objects
have shorter periods, than CCs, and are relatively fainter being located in the lower part
of the Cepheid’s region on the CMD (1.2-1.4 mag brighter than HB stars). Results of our
classification for the 201 candidate CCs in tile LMC 8_3 are presented in Table 3.1.
OGLE III covers the lower 1/4 of tile LMC 8_3 and identified 52 CCs in this region,
of which 36 are in common with EROS-2 and 16 do not have a counterpart in the EROS-2
catalogue of CC candidates. Four of these 16 objects have a counterpart in the general cat-
alogue of EROS-2 stars but they were not classified as CC candidates. Information about
the 36 CCs in common between the EROS-2 and OGLE III catalogues is presented in Ta-
ble 3.3. There are a total number of 142 CCs in this tile, of which 141 have a counterpart
in the VMC catalogue within a pairing radius of 1′′. This corresponds to a 99 % complete-
ness of the VMC survey with respect to the number of CCs identified by both EROS-2 and
50
CHAPTER 3. CLASSICAL CEPHEIDS IN THE VMC TILE LMC 8_3
0 1 218
17
16
15
14
0 0.5 118
17
16
15
14
Log(P)0 0.5 1
18
17
16
15
14
Log(P)
Figure 3.1 Left panel: BEROS , BEROS − REROS CMD of EROS-2 candidate CCs in the
VMC tile LMC 8_3. Blue crosses, green filled circles and black filled triangles represent
EBs, bona-fide CCs and small amplitude variables, respectively. Red filled squares are
LPVs. Black empty circles are 36 CCs observed also by the OGLE III survey, confirming
their classification as CCs. Right panel: PL relations in the REROS (upper-right) and
BEROS (lower-right) bands of the EROS-2 candidate CCs in tile LMC 8_3. Symbols and
colours coding are as in the left panel. The LPVs were omitted. Figure is from Moretti et
al. (2014).
OGLE III.
The results of the classification show that the candidates CCs selected by the EROS-2
on the basis of the PL distribution (right panel of Fig. 2.3) are mainly contaminated by EBs.
We have investigated whether we could find methods to clean the candidate CCs without
checking visually all the light curves, and found that the EROS-2 CMD is well suited for
this purpose, as also was pointed out by Spano et al. (2011) in their Fig. 8. The left panel of
Fig. 3.1 shows the BEROS , BEROS − REROS CMD of the EROS-2 candidate CCs in tile
LMC 8_3. In the CMD objects classified as EBs (blue crosses) after visual inspection of the
light curves are very well separated and definitely bluer (BEROS−REROS < 0.1 mag) than
sources confirmed to be CCs (green circles). Furthermore, both binaries and CCs appear
to be constrained in small BEROS − REROS colour ranges. A number of small amplitude
51
3.3. STRATEGY FOR EXTRACTING BONA-FIDE CLASSICAL CEPHEIDS
variables (black triangles in Fig. 3.1) also fall in the region of EBs. As suggested by the
amplitude smaller than 0.1 mag, the typical periods and the blue colours, they likely are
main sequence variables such as β Cepheids, Be stars, slowly pulsating B variables (see, e.g
Baldacci et al. (2005) and reference therein, for characteristics of these types of variables).
Four LPVs (red squares in Fig. 3.1) lie at colours redder than BEROS −REROS ∼ 1 mag.
Spano et al. (2011) analysed light curves of 856864 variables in the EROS-2 data obtaining
a final list of 43551 LPVs in the LMC. The catalogue of 5800 EROS-2 candidate CCs has
296 objects in common with the LPV catalogue from Spano et al. (2011). The 4 LPVs
found in tile LMC 8_3 are all included in the catalogue of LPVs published by Spano et al.
(2011).
The right panel of Fig. 3.1 shows the PL relations in the REROS (upper panel) and
BEROS (lower panel) passbands of the EROS-2 candidate CCs (the LPVs were omitted).
The bona-fide CCs are distributed along the two loci occupied by first-overtone and funda-
mental mode CCs, respectively. EBs significantly contaminate the Cepheid’s BEROS PL,
while seem to be more separated from bona-fide CCs in the REROS PL. To summarize,
by combining BEROS , BEROS −REROS CMD and the BEROS , REROS PLs it should be
possible to separate quite easily bona-fide CCs from binaries and small amplitude variables.
3.3 Strategy for extracting bona-fide Classical Cepheids
In the analysis of the VMC tiles for which information on the variable stars is available
only from the EROS-2 survey, we will use the following strategy to extract bona-fide CCs
from the EROS-2 sample of candidate CCs. As a general rule we expect that sources with
0.1 < (BEROS−REROS) < 1 mag are likely to be bona-fide CCs, sources with (BEROS−
REROS) < 0.1 mag are likely to be EBs, and objects with (BEROS−REROS) ≥ 1 mag are
LPVs (Moretti et al., 2014). According to this method out of the 5800 EROS-2 candidate
CCs in the LMC, 3484 (60.1 %) are bona-fide CCs, 2003 (34.5 %) are EBs and 313 (5.4 %)
are likely LPVs. However, we are aware that the above colour separations may sometimes
be too crude. Especially for tiles where reddening is large and patchy (internal regions of
the LMC), there may be sources with colours between the two main distributions that may
belong to one or the other group, and thus will need to be checked visually.
In order to check the robustness of the described procedure and verify that bona-fide
CCs selected on the basis of the colour-cuts in the CMD are no longer contaminated by
52
CHAPTER 3. CLASSICAL CEPHEIDS IN THE VMC TILE LMC 8_3
Figure 3.2 Left panel: CMD of the 3488 candidate CCs that have a counterpart in the
OGLE III catalogue of EBs or CCs. Blue points represent EROS-2 candidate CCs with
colour BEROS − REROS < 0.1 mag. Cyan circles represent EROS-2 candidate CCs with
an OGLE III counterpart classified as EBs. Green points are EROS-2 candidate CCs with
colour 0.1 < (BEROS − REROS) < 1.0 mag. Black circles are EROS-2 candidate CCs
with an OGLE III counterpart classified as CCs. Red crosses mark two CCs, that fall in
the region of the CMD mainly occupied by EBs. Red filled circles are EBs falling in the
region of the CMD occupied by bona-fide CCs (67 objects). Right panel: PL in the REROS
passband of the objects with 0.1 < (BEROS −REROS) < 1.0 mag. Figure is from Moretti
et al. (2014).
53
3.3. STRATEGY FOR EXTRACTING BONA-FIDE CLASSICAL CEPHEIDS
spurious sources, we have compared our selection of the EROS-2 candidate CCs with the
OGLE III catalogues of CCs and EBs. The EROS-2 catalogue of candidate CCs contains
a total number of 5800 sources, this number reduces to 5487 if only objects with colour
bluer than 1.0 mag are selected (i.e after discarding the LPVs). Of these 5487 objects, 3488
have a counterpart in the OGLE III catalogues of CCs and EBs within a pairing radius of 1
arcsec.
The left panel of Figure 3.2 shows the CMD of the 3488 stars with a counterpart in
the OGLE III catalogue. This sample contains 2357 CCs and 1062 EBs according to the
colour-cut criteria and the OGLE III classification. There are only two objects (red crosses
in Fig. 3.2) that we would classify as EBs based on their colours and are instead CCs ac-
cording to the OGLE III classification and the visual inspection of the light curves. These
are stars with EROS-2 identification lm0551n20500 and lm0036k8214, corresponding to
OGLE-LMC-CEP-0962 and OGLE-LMC-CEP-2595, respectively. The latter has a clean
light curve, while OGLE-LMC-CEP-0962 has variable mean luminosity. According to the
OGLE III remarks its classification as CC is uncertain. On the other hand, there are 67 ob-
jects (red filled circles in Fig. 3.2) that we would classify as CCs based on their colours and
are instead EBs both according to OGLE III and the visual inspection of the EROS-2 light
curves. This corresponds to a 3 % contamination of the bona-fide CCs sample. Thirty-three
of these binaries have colour in the range [0.1;0.2] mag, suggesting that stars with these
colours need visual inspection to be properly classified.
The right panel of Fig. 3.2 shows the PL distributions in the REROS passband of the
sources with 0.1 < (BEROS − REROS) < 1.0 mag. There are two separate sequences
formed by the fundamental and the first-overtone mode pulsators. Part of EBs that still
contaminate the CCs sample (red points in Fig. 3.2) deviate significantly from the CCs
sequences and could be eliminated with a sigma-clipping procedure. This will allow us to
further reduce the 3 % contamination of the sample of bona-fide CCs. In summary, the
application of colour-cuts in the CMD is a robust criterion that combined with the analysis
of the scatter in the PL relations allows one to extract a sample of bona-fide CCs more
than 97 % clean from contaminating sources (Moretti et al., 2014). In any case, a 3 %
contamination is not expected to affect significantly the PLKs relations of CCs in regions
where only the EROS-2 data are available.
54
CHAPTER 3. CLASSICAL CEPHEIDS IN THE VMC TILE LMC 8_3
OG
LEII
Iid
ERO
S-2
idR
AD
ECTy
peI
VP
(HH
:MM
:SS)
(DD
:MM
:SS)
(mag
)(m
ag)
(day
)O
GLE
-LM
C-C
EP-0
598
lm02
93l2
6069
4:59
:51.
63-6
6:54
:15.
21
16.5
6817
.215
0.89
7332
OG
LE-L
MC
-CEP
-076
9lm
0302
l135
045:
02:5
0.85
-66:
50:3
5.5
116
.019
16.5
721.
2612
91O
GLE
-LM
C-C
EP-0
876
lm03
02n2
6730
5:04
:56.
83-6
6:56
:29.
11
15.8
2516
.540
1.66
4000
OG
LE-L
MC
-CEP
-105
0lm
0303
m16
963
5:08
:09.
07-6
6:41
:49.
21
15.6
6216
.378
1.70
2563
OG
LE-L
MC
-CEP
-094
1lm
0303
k560
85:
06:0
7.13
-66:
37:4
9.3
F16
.228
16.8
471.
7272
54O
GLE
-LM
C-C
EP-0
534
lm02
93k1
6840
4:58
:35.
95-6
6:41
:53.
81
15.4
4415
.995
1.77
2482
OG
LE-L
MC
-CEP
-092
1lm
0303
l196
805:
05:4
9.15
-66:
52:0
0.0
115
.345
15.9
331.
7939
72O
GLE
-LM
C-C
EP-0
574
lm02
93l2
3982
4:59
:19.
44-6
6:53
:35.
21
15.3
8216
.007
1.89
8245
OG
LE-L
MC
-CEP
-112
6lm
0312
k163
005:
09:3
0.30
-66:
44:1
4.7
115
.312
15.8
981.
9069
54O
GLE
-LM
C-C
EP-1
000
lm03
03n1
3787
5:07
:21.
10-6
6:49
:47.
41
15.4
6716
.182
1.96
6774
OG
LE-L
MC
-CEP
-079
2lm
0302
l581
25:
03:1
3.78
-66:
47:3
0.6
115
.242
15.8
271.
9886
42O
GLE
-LM
C-C
EP-0
911
lm03
03l2
2257
5:05
:36.
39-6
6:52
:54.
01
15.2
10-9
9.99
2.07
8685
OG
LE-L
MC
-CEP
-074
6lm
0302
l166
605:
02:2
5.73
-66:
51:5
2.4
115
.381
16.0
612.
0854
01O
GLE
-LM
C-C
EP-0
618
lm02
93k2
961
5:00
:07.
52-6
6:36
:50.
71
15.1
2415
.638
2.09
5957
OG
LE-L
MC
-CEP
-101
8lm
0305
m27
115:
07:2
9.33
-66:
57:5
8.3
F15
.525
16.1
282.
3576
19O
GLE
-LM
C-C
EP-0
988
lm03
03k1
2257
5:07
:09.
87-6
6:40
:07.
71
15.0
4115
.595
2.36
8493
OG
LE-L
MC
-CEP
-112
1lm
0312
k971
55:
09:2
7.37
-66:
40:0
5.4
114
.913
15.5
352.
5649
91O
GLE
-LM
C-C
EP-1
039
lm03
05m
1194
05:
08:0
1.06
-67:
01:1
7.1
F15
.448
16.0
962.
6948
34O
GLE
-LM
C-C
EP-0
818
lm03
04m
5953
5:03
:46.
02-6
6:59
:24.
6F
15.4
8916
.182
2.71
2216
OG
LE-L
MC
-CEP
-093
9lm
0305
k704
05:
06:0
5.98
-66:
59:4
3.9
F15
.483
16.2
022.
8617
35O
GLE
-LM
C-C
EP-0
933
lm03
03l6
182
5:05
:59.
19-6
6:47
:15.
0F
15.3
4115
.977
2.89
4750
OG
LE-L
MC
-CEP
-096
0lm
0303
k205
775:
06:3
7.62
-66:
43:0
8.8
F15
.432
16.1
412.
9312
99O
GLE
-LM
C-C
EP-1
035
lm03
03m
5774
5:07
:56.
39-6
6:37
:45.
4F
15.2
7115
.913
2.95
7635
OG
LE-L
MC
-CEP
-113
4lm
0310
l967
85:
09:4
7.91
-66:
35:4
6.1
114
.575
15.1
623.
0900
31O
GLE
-LM
C-C
EP-0
951
lm03
03k8
191
5:06
:18.
53-6
6:38
:44.
7F
15.3
7515
.992
3.11
3395
OG
LE-L
MC
-CEP
-095
2lm
0301
l821
45:
06:1
9.60
-66:
35:4
7.8
F15
.384
16.0
753.
1232
34O
GLE
-LM
C-C
EP-0
974
lm03
03k1
9341
5:06
:56.
76-6
6:42
:40.
3F
15.2
5615
.907
3.19
3414
OG
LE-L
MC
-CEP
-115
0lm
0310
l188
495:
10:1
3.39
-66:
35:0
0.7
F15
.323
16.1
253.
5187
52O
GLE
-LM
C-C
EP-1
064
lm03
03m
2638
85:
08:2
1.68
-66:
45:0
9.5
F115
.014
15.6
893.
7003
49O
GLE
-LM
C-C
EP-1
013
lm03
03m
3523
5:07
:26.
73-6
6:36
:58.
5F
15.1
3615
.890
3.75
6495
55
3.3. STRATEGY FOR EXTRACTING BONA-FIDE CLASSICAL CEPHEIDSO
GLE
-LM
C-C
EP-0
762
lm03
02k1
5867
5:02
:37.
14-6
6:44
:59.
4F
14.9
6115
.632
3.83
2815
OG
LE-L
MC
-CEP
-108
5lm
0303
n198
405:
08:4
7.38
-66:
51:4
3.0
F15
.063
15.8
273.
9681
88O
GLE
-LM
C-C
EP-1
003
lm03
03n1
1462
5:07
:22.
63-6
6:48
:56.
8F
15.0
8115
.847
4.00
3405
OG
LE-L
MC
-CEP
-099
4lm
0303
n141
105:
07:1
7.64
-66:
49:5
4.5
F15
.054
15.8
484.
2402
70O
GLE
-LM
C-C
EP-1
056
lm03
03n1
9424
5:08
:12.
53-6
6:51
:39.
2F
14.9
7715
.774
4.46
0721
OG
LE-L
MC
-CEP
-099
7lm
0301
n218
845:
07:1
8.60
-66:
34:5
2.7
F14
.805
15.5
794.
5081
96Ta
ble
3.3:
Prop
ertie
sofC
Cs
intil
eLM
C8_
3,w
hich
have
aco
unte
rpar
tin
the
OG
LEII
Ica
talo
gue
(Col
umn
1:O
GLE
III
iden
tifica
tion
ofth
est
ar;
Col
umn
2:Id
entifi
catio
nof
the
star
from
the
ERO
S-2
cata
logu
e;C
olum
n3:
Rig
htas
cens
ion
from
the
OG
LEII
Ica
talo
gue;
Col
umn
4:D
eclin
atio
nfr
omth
eO
GLE
III
cata
logu
e;C
olum
n5:
Type
acco
rdin
gto
the
OG
LEII
Icl
assi
ficat
ion:
F-
Fund
amen
talm
ode
CC
s,1
-Fi
rst-
over
tone
mod
eC
Cs,
F1-D
oubl
e-m
ode
CC
s;C
olum
n6:
OG
LEII
II
mea
nm
agni
tude
;Col
umn
7:O
GLE
IIIV
mea
nm
agni
tude
;Col
umn
8:Pe
riod
from
the
OG
LEII
Icat
alog
ue).
56
Chapter 4
Eclipsing binaries in the LMC
The EROS-2 sample of candidate CCs is significantly contaminated by EBs. These objects
have blue colours, hence, we classed them as “hot” eclipsing binaries (HEBs; Muraveva et
al. 2014a). In this chapter we describe the results of our analysis of these HEBs.
4.1 EROS-2 data for eclipsing binaries
As it was described in Section 3.3 a large number of objects with colour (BEROS−REROS) <
0.1 mag are EBs. It was also noted that sources with colour 0.1 < (BEROS−REROS) < 0.2
mag are located in the CMD between the distributions of CCs and EBs and may belong to
one or the other group. Thus, stars with these colour need visual inspection of the light
curves to be properly classified. In order to characterise the EROS-2 EBs that contaminate
the sample of LMC bona-fide CCs we extract from the EROS-2 catalogue of candidate CCs
all objects with colour (BEROS − REROS) < 0.2 mag (2085 sources). We explicitly note
that the EROS-2 catalogue of candidate variables contains a much larger number of EBs.
Recently, Kim et al. (2014) identified new EBs in the LMC based on the full EROS-2 dataset
by applying a machine learning approach. However, in this thesis work we focused only on
the objects contaminating the CC sample.
The analysis of these sources was performed running GRATIS on the REROS light
curves and showed that 83 objects from the sample are bona-fide CCs, 225 are small ampli-
tude variables, nine objects have light curves which are too noisy to be classified, and 1768
stars are EBs. Information on these EBs is presented in Table A.1 (Appendix).
We transformed the BEROS , REROS average magnitudes of the sources to V , I stan-
dard magnitudes by applying equations 2.1 and 2.2 (Subsection 2.4.1). The left panel of
Figure 4.1 shows the distributions of mean V, I magnitudes and V − I colours for our sam-
57
4.1. EROS-2 DATA FOR ECLIPSING BINARIES
17 16 15 140
20406080
17 16 15 140
20406080
17 16 15 140
20406080
100
-1 -0.5 00
100200300400500
5 10 15 20
0
100
200
300
400
Period (days)
Figure 4.1 Distributions of mean V, I magnitudes and V −I colours (left panels), and period(right panel) of the LMC EBs in our sample. Figure is from Muraveva et al. (2014a).
ple of EBs. The mean V and I magnitudes range from ∼17.8 to ∼13.2 mag (which reflects
the initial cuts in magnitude used to extract the sample of candidate CCs from the EROS-2
catalogue) and from ∼18.1 to ∼13 mag, respectively, with a peak around 17.1-17.2 mag in
both bands. The V − I colours range from ∼ −1.3 to 0.33 mag and peak at V − I = −0.3
mag, which reflects instead the colour selection we applied to separate binaries from bona-
fide CCs. According to their blue colours the EBs in our sample are mainly composed by
hot components: main sequence stars or blue giants, hence, we classified them as HEBs.
We have compared the periods provided by the EROS-2 survey for the HEBs with those
determined by the visual inspection of light curves with GRATIS (PGRATIS). For the ma-
jority of binaries PGRATIS is in good agreement with PEROS . However, in some cases,
PEROS was a harmonic or a subharmonic of the actual period. We corrected the period of
225 objects in the sample by multiplying PEROS by different constants until the shape of
the light curve was consistent with that of an EB. The same technique was used by Derekas
et al. (2007) as part of the redetermination of periods for 3031 EBs in the MACHO cata-
logue. Examples of the light curves before and after the period correction are presented in
Figure 4.2. The systems in the middle and bottom panels of Figure 4.2 have rather eccen-
tric orbits which hinders the automatic determination of the period. In some cases it was
not clear if EROS-2 determined aliases of the true period or if the binary star had only one
58
CHAPTER 4. ECLIPSING BINARIES IN THE LMC
Figure 4.2 Light curves of EBs before (left panels) and after (right panels) correction of theperiod (see text for details). Figure is from Muraveva et al. (2014a).
strong expressed minimum. For these objects we decided to use the periods provided by
EROS-2.
We studied the period distribution of our sample of HEBs even though the true periods
of these objects cover a relatively narrow range (from ∼ 0.89 to ∼ 20 day). The distribution
of periods is shown on the right panel of Fig. 4.1. Most of our HEBs are short-period
systems. The distribution sharply peaks between 1 and 2 days and the majority of HEBs in
our sample (94 %) have periods shorter than 5 days.
4.2 Cross-correlation with other catalogues of eclipsing binariesin the LMC
Nine different catalogues of EBs detected in the LMC by the microlensing surveys have
been published. During the first stage of the EROS survey, 79 candidate EBs were identified
in the bar of the LMC (Grison et al., 1995). The MACHO survey identified an initial sample
of 611 LMC EBs (Alcock et al., 1997). Subsequently, Derekas et al. (2007) reanalysed the
eclipsing variables in the MACHO database, corrected their periods and presented a “clean"
sample of 3031 EBs. Faccioli et al. (2007) provided a new sample of 4634 EBs in the LMC
from the MACHO catalogue, expanding the previous sample of 611 objects from Alcock et
59
4.2. CROSS-CORRELATION WITH OTHER CATALOGUES OF ECLIPSINGBINARIES IN THE LMC
al. (1997). Using the OGLE II data, 3332 EBs were identified in the LMC (Wyrzykowski
et al. 2003, Groenewegen 2005, Graczyk & Eyer 2010). Graczyk et al. (2011) provided
a sample of 26121 LMC EBs detected by the OGLE III survey. Finally, Soszynski et al.
(2012) identified 1377 EBs and 156 ellipsoidal variables in the GSEP area based on the
OGLE IV survey.
We cross-correlated our sample of 1768 HEBs with the catalogues of EBs identified in
the LMC by the various microlensing surveys. Specifically, we considered: the first stage
of the EROS survey (Grison et al. 1995), the MACHO survey (Alcock et al. 1997; Derekas
et al. 2007; Faccioli et al. 2007), the OGLE III (Graczyk et al. 2011) and IV (Soszynski
et al. 2012) surveys. Objects in the various catalogues were cross-identified when their
right ascension and declination differed by less than 10′′, and the periods differed by less
than 1%. We also considered objects located within less than 10′′ and with the ratio of
the periods approximately equal to integer numbers, in case one of the surveys had picked
harmonics or subharmonics of the true period. We used a rather large pairing radius in order
to avoid missing counterparts of our EBs in other catalogues, however, we note that the vast
majority of the counterparts were found to be within a pairing radius of 1′′ (OGLE III: 99%;
MACHO from Faccioli et al. 2007: 57%; MACHO from Derekas et al. 2007: 63%; EROS:
100%).
Twenty-five out of seventy-nine EBs detected in the LMC bar by the first stage of the
EROS microlensing survey (Grison et al. 1995) have a counterpart in our sample of HEBs.
Panel (a) of Figure 4.3 shows the position of those 25 EBs (green dots) on the map of our
1768 HEBs (black dots). The cross-correlation with Derekas et al. (2007) and Faccioli et
al. (2007) catalogues of EBs detected in the LMC by the MACHO survey shows that 797
objects were already known (panel (b) of Fig. 4.3). The cross-correlation with the sample
of 26121 EBs from the OGLE III catalogue (Graczyk et al. 2011), the 1377 EBs and the
156 ellipsoidal stars in the OGLE IV catalogue (Soszynski et al. 2012) showed that 1074
objects were already known (panel (c) of Fig. 4.3). We also cross-matched our sample with
the spectroscopy of massive stars available from the VLT-FLAMES surveys of Evans et al.
(2006,2011), in the NGC 2004, N11 and 30 Doradus regions of the LMC. Eight objects
from our sample have been observed by these surveys: four stars in 30 Doradus by the
VLT-Flames Tarantula Survey (VFTS), two in NGC 2004 and two in N11, as summarized
in Table 4.1. Four of these eight objects have a counterpart in the OGLE III catalogue, one
was observed by the MACHO project, three objects have not been detected before. Optical
60
CHAPTER 4. ECLIPSING BINARIES IN THE LMC
90 80 70
-72
-70
-68
-66
-64
RA (deg)
-72
-70
-68
-66
-64
90 80 70RA (deg)
Figure 4.3 Panels (a)-(c): spatial distribution of the 1768 HEBs analysed in this study (blackdots) compared with those detected from previous surveys; (a) the first stage of the EROSsurvey (green dots), (b) the MACHO project (red dots), (c) the OGLE III/IV surveys (bluedots). Panel (d) shows the location of the 493 EBs detected only by the EROS-2 survey.Figure is from Muraveva et al. (2014a).
spectroscopy is available for a further five of our detected EBs, from observations with
the AAOmega multi-object spectrograph on the Anglo-Australian Telescope, one of these
objects has not been detected by previous surveys.
To summarize, a total number of 1275 sources in our EROS-2 HEBs sample had pre-
viously been detected by other surveys (OGLE III, OGLE IV, MACHO, EROS, with the
FLAMES and AAOmega spectrographs), whereas 493 were observed only by the EROS-2
survey. The positions of these objects in the LMC are shown in panel (d) of Figure 4.3. As
expected they are mainly located in the outer regions of the LMC.
We also compared our corrected periods with the periods from other catalogues of EBs
(MACHO, OGLE III, OGLE IV). Among the 225 objects for which we corrected the period
163 were also detected by the OGLE III survey, and our corrected periods are in good
agreement (to within 1%) for all but one system. Other 6 and 19 objects with corrected
periods were observed by the OGLE IV and MACHO (Faccioli et al. 2007, Derekas et al.
2007) surveys, respectively. The corrected periods for all of these are in good agreement
with the published values (to within 1%). In conclusion, of the 225 objects for which we
61
4.2. CROSS-CORRELATION WITH OTHER CATALOGUES OF ECLIPSINGBINARIES IN THE LMC
0 2 4 6 8 10
-0.02
-0.01
0
0.01
0.02
0 0.2 0.4 0.6 0.8 1
15.75
15.7
15.65
15.6
0 0.2 0.4 0.6 0.8 1
15.75
15.7
15.65
15.6
0 0.2 0.4 0.6 0.8 1
15.85
15.8
15.75
15.7
0 0.2 0.4 0.6 0.8 1
15.85
15.8
15.75
15.7
Figure 4.4 Left panel: comparison between periods adopted in this study and those inthe OGLE III and OGLE IV catalogues for the 1072 EBs in common. Two objects,namely lm0185l23772 and lm0030n12500, were not included because their OGLE peri-ods differ significantly from our values. Right panels: light curves of lm0185l23772 andlm0030n12500 with the periods used in this thesis work (on the left) and provided by theOGLE III catalogue (on the right). Figure is from Muraveva et al. (2014a).
corrected the periods, 188 were detected by other surveys and our estimates are confirmed
in all but one of these cases (i.e. > 99%).
The left panel of Figure 4.4 shows the comparison of the periods adopted in this thesis
work with those provided by the OGLE III and OGLE IV catalogues for the 1072 objects in
common. Two objects, namely lm0185l23772 and lm0030n12500 are not shown in the plot
because their OGLE III periods are harmonics of the periods derived in this study so they
differ significantly. We checked the light curves of these objects with GRATIS and could
not confirm the periods in the OGLE III catalogue. In particular, for lm0185l23772 (OGLE-
LMC-ECL-09445) we confirmed the period provided by the EROS-2 catalogue (P=4.97
days), whereas for lm0030n12500 (OGLE-LMC-ECL-20762) we determined a new period
(P=1.4998 days) which is one third of the period provided by EROS-2, while OGLE III
determined a period approximately equal to two thirds of the EROS-2 period. The light
curves of these objects are presented on the right panel of Figure 4.4. Apart from these
two objects, the periods adopted in this thesis work and those in the OGLE III catalogue
generally differ by less than 0.03% (left panel of Fig. 4.4).
62
CHAPTER 4. ECLIPSING BINARIES IN THE LMC
4.3 Characteristics of eclipsing binaries with existing spectroscopy
4.3.1 Cross-matches with the VLT-FLAMES surveys
As already mentioned in Section 4.2, eight HEB systems in our sample have existing optical
spectroscopy from surveys with FLAMES at the VLT (Evans et al. 2006, Evans et al. 2011),
as summarized in Table 4.1. All were detected as binaries in the multi-epoch spectroscopy,
except for VFTS 462 (Dunstall et al. in prep). In addition to the EROS-2 periods, estimates
are also available from the OGLE III data for the four VFTS systems (Graczyk et al., 2011),
with excellent agreement in all cases; the other four systems (in NGC 2004 and the N11
region) are beyond the OGLE III survey area.
Quantitative analysis of the VFTS spectra is still underway, but evolutionary mass es-
timates (of the primaries) of the other systems are available from Hunter et al. (2008);
M = 13M⊙ for both N11-107 and N11-119, and M = 11 and 10M⊙ for NGC 2004-079
and NGC 2004-094, respectively1. Photospheric chemical abundances were presented for
the two systems in NGC 2004 by Hunter et al. (2009), with seemingly unremarkable nitro-
gen abundances. The spectroscopy from the FLAMES surveys was effective in detecting
spectroscopic binaries, but further monitoring is generally required to characterize the or-
bital parameters (e.g., Ritchie et al. 2012). Indeed, spectroscopic monitoring of a subset
of the O-type binaries discovered by the VFTS is now underway (P.I. Sana), and includes
VFTS 061 among its targets.
4.3.2 AAOmega spectroscopy
Optical spectroscopy is available for a further five of our detected EBs, from observations
with the AAOmega multi-object spectrograph on the Anglo-Australian Telescope, obtained
during 2006 February 22-24 (P.I. van Loon). The five targets discussed here were obtained
as part of two fields centred on N11 and 30 Dor. AAOmega is a twin-arm spectrograph
(providing simultaneous blue/red coverage), but only the blue data are discussed here. Both
fields were observed on the first night with the 1700B grating and two central wavelengths
(4100 and 4700 Å), giving coverage of 3765-5015 Å, at a resolution of 1 Å. The 30 Doradus
field was also observed on the second night with the 1500V grating, at a central wavelength
of 4375 Å, providing coverage of 3975-4755 Å, at a resolution of 1.25 Å. These data were
reduced using the AAOmega reduction pipeline and the relevant spectra were rectified and1However, note that these estimates were on the basis of effective temperatures adopted from the spectral
classifications, and the expected uncertainties on these masses is typically 30% (Hunter et al., 2008).
63
4.4. CLASSIFICATION OF ECLIPSING BINARIES
EROS-2 id RA(J2000) DEC(J2000) Period Period Alternative id Spectral type Notes Ref.(deg) (deg) EROS-2 OGLE III
lm0290l18998 73.88709 −66.54208 3.224805 − N11-107 B1-2+Early B SB2 E06lm0290l5213 73.95604 −66.43437 1.791025 − N11-119 B1.5 V SB2 E06lm0344l12773 82.6699 −67.19545 4.952487 − NGC 2004-079 B2 III SB1 E06lm034l21656 82.78869 −67.25619 4.164156 − NGC 2004-094 B2.5 III Binary E06lm0030m4163 84.37804 −69.08817 2.333416 2.333427 VFTS 061 ON8.5III:+O9.7: V: SB2 W14lm0030m3468 84.42029 −69.07812 1.674098 1.674119 VFTS 112 Early B+Early B SB2 E14lm0030m9744 84.46997 −69.16274 1.434738 1.434745 VFTS 189 B0.7: V Binary E14lm0226n24168 84.66296 −69.02808 1.176008 1.176008 VFTS 462 B0.5-0.7 V − E14lm0426m23482 75.07795 −66.06284 2.345573 − − B1: V SB2? . . .lm0294m4825 74.53203 −66.98277 2.97779 2.9778 − B0-0.5 V SB? . . .lm0436l19007 76.28093 −66.19386 3.301123 − − B2 V − . . .lm0020n19615 82.67397 −69.32445 4.585353 4.585031 − B1.5 Ib SB1? . . .lm0031l22987 85.19681 −69.34126 5.413977 5.414011 − B1 III SB2 . . .
Table 4.1 EROS-2 HEBs with existing optical spectroscopy; E06 (Evans et al., 2006); W14(Walborn et al., 2014); E14 (Evans et al. in prep). OGLE III periods are from Graczyk et al.(2011). SB1 and SB2 stand for single- and double-lined spectroscopic binaries, respectively.
co-added.
Spectral classifications for the five systems are presented in Table 4.1, in which we
have employed the same framework as that used by Evans et al. 2014 (in prep.). All five
systems have early B-type spectra (in line with the expectation of these as HEBs), with
morphological evidence for binarity (double-lined and/or asymmetric profiles) in all but
one.
4.4 Classification of eclipsing binaries
Our classification of the EBs was based on both the Fourier analysis (Rucinski 1993,1997
and Maceroni & Rucinski 1999) and the visual inspection of the light curves. As it was
shown in Subsection 1.6.1 the combination of two cosine coefficients of the Fourier de-
composition of EB’s light curves, a2 and a4, could serve as a separator of contact and non-
contact binaries. Namely, the curve described by the relation a4 = a2(0.125 − a2), where
both coefficients are negative, separates the regions of the contact and non-contact bina-
ries on the a2 versus a4 plane (Rucinski, 1993). We adopt the term “contact-binary-like"
systems for all objects passed by the Fourier filter (see Subsection 1.6.1).
By analysis of the Fourier decomposition of the light curves in the REROS passband we
identified the contact-like binaries in our sample. The light curves were not expressed in
magnitudes but in intensity units, relative to the maxima at phases in the range [0.24, 0.26].
Columns from 8 to 13 of Table A.1 (Appendix) present the 6 Fourier coefficients a0 to a5
of the Fourier analysis for the 1768 EBs in our sample.
64
CHAPTER 4. ECLIPSING BINARIES IN THE LMC
0 0.2 0.4 0.6 0.8 1
0.6
0.8
1
0 0.2 0.4 0.6 0.8 1
0.6
0.8
1
1.2
Figure 4.5 Examples of the Fourier fit obtained using 6 harmonics to model the light curveof detached (upper panel) and contact-like (bottom panel) binaries in our sample. Blackdots represent the observational data, red solid lines show the resultant Fourier fits. Six har-monics are clearly not sufficient to reproduce detached systems. Figure is from Muravevaet al. (2014a).
Figure 4.5 shows examples of the resultant fits for both contact-like (lower panel) and
non-contact (upper panel) binary systems. It should be noticed that six harmonics generally
allow very satisfactory fits for contact-like systems, whereas some noticeable differences
arose between the observations and the fitted curves for non-contact binaries, which would
indeed require a much larger number of harmonics (8-10 or more) to be modelled. This is
often due to elliptical orbits, yielding a shift of the secondary minimum from phase 0.5 of
the non-contact systems.
Figure 4.6 shows the position of 1768 EBs in our sample on the a2 versus a4 plane. The
solid line in the figure is the contact locus line defined by Rucinski (1993). We classified
objects located below the line as contact-like binaries (324 sources) and those above as non-
contact binaries (1444 sources). However, being aware that detached and semi-detached
systems could accidentally appear below the locus line due to a bad fit of the light curve, we
visually inspected the light curves of all the objects (324 stars) located below the line; we
discovered eight objects which have light curves without the characteristic form of contact
binaries, so we discarded them. In conclusion, in our analysis a system is classified as
contact-like if it is located below the locus line from Rucinski (1993) on the a2 versus a4
65
4.4. CLASSIFICATION OF ECLIPSING BINARIES
0 -0.1 -0.2
0
-0.05
-0.1
Figure 4.6 Fourier coefficients a2 and a4 of the 1768 HEBs in our sample. The solid curveis described by the relation a4 = a2(0.125 − a2) which, according to Rucinski (1993),separates the regions of contact and non-contact binaries. Objects located below the line areconsidered to be contact systems. Red filled triangles identify objects classified as contactbinaries in the OGLE III catalogue (see text for details). Figure is from Muraveva et al.(2014a).
66
CHAPTER 4. ECLIPSING BINARIES IN THE LMC
plane and its light curve has the characteristic shape of a contact system.
We compared our classifications with those from the OGLE III catalogue. Out of 1055
objects in common, 48 stars were classified as contact systems in the OGLE III catalogue
(red filled triangles in Figure 4.6). Figure 4.6 shows that the majority of these objects are
in fact located below the locus line traced by Rucinski (1993), while the majority of the
systems classified as non-contact variables by OGLE III are above the curve. However,
eight objects located marginally above the locus line were classified as contact binaries
by OGLE III. We checked their light curves and confirmed that these binaries are indeed
contact-like systems. When including these, the final number of contact-like binaries in
our sample is 324. In contrast, 50 of 1055 objects in common were classified as contact-
like systems by us, but as detached, semi-detched or ellipsoidal systems by OGLE III.
We double checked their light curves, and found that our classification is in disagreement
with OGLE III in some cases. The majority of these objects have low amplitudes so it
is difficult to provide an exact classification by visual inspection of light curves. In the
following analysis we use our classification for those objects, thus our final sample consists
of 324 contact-like binaries and 1444 non-contact systems.
4.5 Period-Luminosity relation of eclipsing binaries
4.5.1 PL relation of eclipsing binaries from the EROS-2 sample
The PL relation of blue, luminous contact systems, observed in the LMC by the MACHO
project, was studied by Rucinski (1999). He suggested the existence of a PL relation at
maximum light in the visual band, but with a large scatter, possibly due to unaccounted
effects of the interstellar extinction (see Section 1.6). Following Rucinski (1999) we have
investigated whether our sample of HEBs follows a PL relation at maximum light using
the red passband photometry of EROS-2 (REROS) and near-infrared photometry in the Ks-
band obtained as part of the VMC survey (Cioni et al. 2011). The latter was used in order
to minimize possible extinction effects.
When this study was performed, the complete multi-epoch dataset was available for
ten LMC tiles, whereas further seven tiles had been observed at least once. These 17 tiles
sample different regions of the LMC from the inner bar to the outer regions.
We have cross-matched our catalogue of 1768 HEBs against the VMC catalogue avail-
able at VSA (observations completed until the 1st of April 2013) for the 17 tiles and found
67
4.5. PERIOD-LUMINOSITY RELATION OF ECLIPSING BINARIES
Figure 4.7 Light curves in the Ks (left panels) and REROS (right panels) passbands ofexample HEBs with a counterpart in the VMC catalogue. P - period (day), N - number ofobservations in the corresponding passband. Figure is from Muraveva et al. (2014a).
68
CHAPTER 4. ECLIPSING BINARIES IN THE LMC
999 binaries in common using a pairing radius of 1′′. Examples of the Ks and REROS light
curves for some of these binaries are shown in Figure 4.7. The number of phase-points of
the Ks-band light curves varied from a minimum of one for EBs located in tiles with incom-
plete observations to a maximum of over 30 phase points for EBs located in regions where
different tiles overlap. Furthermore, the EBs in our sample are relatively bright sources.
Therefore the shallow VMC epochs, for which the integration time of observation is half
that for deep epochs, or epochs not meeting the original quality criteria (e.g., seeing, etc.)
were enough to measure the EBs thus increasing the number of available phase-points.
The REROS and Ks magnitudes at maximum light of the binaries that have a VMC
counterpart are presented in Table A.2 (Appendix). In order to better determine the Ks-band
magnitudes at maximum light, we performed an additional analysis of the light curves with
GRATIS, for those HEBs which have 13 or more good-quality observations. The left panel
of Figure 4.8 shows the PL distribution in the REROS band of the 999 EBs with a VMC
counterpart, whereas the right panel shows their PL distribution in the Ks band. In both
figures red open circles identify the sources which we classified as contact-like systems. The
contact binaries for which we have 13 or more Ks-band epochs (and for which maximum
magnitudes were determined with GRATIS) are highlighted in green. Unfortunately, the
use of a more robust method to determine the Ks magnitude at maximum light does not
decrease the scatter. Both the optical and near-infrared PL distributions exhibit a very large
dispersion, which is of the same order of the scatter observed in the PL relation originally
used by the EROS-2 team to extract the candidate CCs from the EROS-2 general catalogue
of LMC variables (see right panel of Fig. 2.3). Thus, a PL relation for HEBs doesn’t seem
to exist.
4.5.2 PL relation of eclipsing binaries from the OGLE III catalogue
In order to study the PL relation of contact binaries in a more general sample and over
a larger range of periods we have used the OGLE III catalogue of EB stars published by
Graczyk et al. (2011). We extracted all the objects which were classified as contact bina-
ries in the Graczyk et al. (2011) catalogue. Among them we selected objects with VMC
counterparts and, with both V and I magnitudes from OGLE III, giving 563 objects in to-
tal. Twenty-five of these sources have their counterparts in our sample of HEBs from the
EROS-2 catalogue and were already discussed in Section 4.5.1. To account for extinction
we used the LMC reddening maps derived by Haschke et al. (2011) on the basis of OGLE III
69
4.5. PERIOD-LUMINOSITY RELATION OF ECLIPSING BINARIES
0 0.5 1
18
16
14
0 0.5 1
18
16
14
Figure 4.8 PL distribution in the REROS (left panel) and Ks (right panel) passbands of999 HEBs that have a counterpart in the VMC catalogue (black dots). Red open circles areobjects which we classified as contact binaries. Green filled circles are 90 contact EBs forwhich we have 13 or more epochs in the Ks light curves. Figure is from Muraveva et al.(2014a).
data. To compute extinction values in the various bands we used the relations from Schlegel
et al. (1998) and Cardelli et al. (1989), these were then applied to correct each source.
The reddening corrected V0, (V − I)0 CMD of contact binaries from the OGLE III
catalogue is shown in Figure 4.9. Contact binaries are located in two regions in the CMD:
HEBs which contain MS stars or blue giants have (V − I)0 < 0.3 mag, whereas EBs with a
red giant component have (V − I)0 ≥ 0.3 mag. The corresponding PL distributions in the
I0 and Ks,0 bands are presented in Figure 4.10. In the figures HEBs are indicated with black
dots and binary systems containing red giants are indicated with red triangles. For 164 EBs
with a red giant component, which have 13 or more good-quality epochs from the VMC
survey, we analysed the light curves with GRATIS in order to determine the Ks magnitude
at maximum light with a good accuracy. On the right panel of Fig. 4.10 we have highlighted
these objects with green triangles. While contact HEBs from the OGLE III sample do not
distribute along a PL sequence, contact binaries containing red giant components seem to
follow at least one, maybe two, different PL sequences.
To further investigate this point we restricted our analysis to 164 objects with carefully
determined Ks maximum magnitudes (green triangles on the right panel of Fig. 4.10). Their
PL distribution is shown in Figure 4.11. As it could be seen, there are 11 objects with short
70
CHAPTER 4. ECLIPSING BINARIES IN THE LMC
-1 0 1 2 3
20
18
16
14
12
Figure 4.9 CMD of 563 contact binary stars which have V and I (OGLE III) and Ks (VMC)magnitudes. Black dots are objects with (V − I)0 < 0.3 mag and red triangles are objectswith (V − I)0 ≥ 0.3 mag. The dashed line corresponds to (V − I)0 = 0.3 mag. Figure isfrom Muraveva et al. (2014a).
-1 0 1 2 3
20
18
16
14
12
-1 0 1 2 3
20
18
16
14
12
Figure 4.10 PL distribution at I0 maximum (left panel) and at Ks,0 maximum (right panel)of the 563 contact binaries shown in Fig. 4.9. Black dots are objects with (V − I)0 < 0.3mag, red triangles are objects with (V − I)0 ≥ 0.3 mag of which those with 13 or moreepochs in the Ks-band are marked in green. Figures are from Muraveva et al. (2014a).
71
4.5. PERIOD-LUMINOSITY RELATION OF ECLIPSING BINARIES
-1 0 1 2 3
18
16
14
12
Figure 4.11 PL distribution of contact binaries containing red giant components. Blue opencircles are candidate HEBs falling in the region of binaries with red giant components (theirerrors are smaller than the size of the circles), red and black dots represent EBs whichdeviate less (red) and more (black) than 3σ from a linear regression, respectively. The lineis the weighted linear fit obtained from the objects marked in red. Figure is from Muravevaet al. (2014a).
72
CHAPTER 4. ECLIPSING BINARIES IN THE LMC
periods which do not follow any PL sequence (blue open circles in Fig. 4.11). We checked
the position of these objects in the CMD (Fig. 4.9) and found that they are located in the
border region between HEBs and binaries with red giant components. Since these objects
do not follow the PL sequence and could be HEBs, we discarded them from the following
analysis.
For other 153 EBs we computed a weighted linear regression through the data by pro-
gressively discarding objects which deviate more than 3σ from the linear regression. The
majority of contact systems with carefully determined Ks maximum magnitudes (red dots
in Figure 4.11) appear to follow the relation :
Ks,0 = (−2.888 ± 0.096)log(P ) + (20.139 ± 0.171) (4.1)
with rms=0.406 mag.
In Figure 4.11 we have highlighted objects located more than 3σ from the PL distri-
bution with black dots. Some of them seem to follow a PL sequence parallel to the one
described by Eq. 4.1 and located ∼ 1 mag fainter than the previous one.
To summarize, HEBs do not follow any PL relation while the existence of red giant
PL sequence(s) (at least, one) seems quite clear and, as shown by Fig. 4.10, this relation
appears to be narrower in the Ks passband. However, the large scatter makes it impossi-
ble to use these sequences any further. On the other hand, that red giants follow multi-
ple PL relations was already reported in many studies (Wood et al. 1999, Soszynski et al.
2004, Derekas et al. 2006). Wood et al. (1999) were the first to recognize five different
PL-sequences: A, B and C, occupied by pulsating red giants, D composed by stars that
have long secondary periods (LSPs), and sequence E, containing red giants in contact EBs
and ellipsoidal variables. Soszynski et al. (2004) showed that a PL relation of ellipsoidal
variables could be well described by a simple model using the Roche-lobe geometry and
that sequences E and D merge at specific luminosities. Derekas et al. (2006) presented a
period-luminosity-amplitude analysis of 5899 red giant and binary stars in the LMC from
the MACHO database and discovered that the PL sequence of binaries is composed only by
contact EBs, while detached and semi-detached systems are spread everywhere in the PL
plane. Moreover, they concluded that sequence E, is located at periods a factor two greater
and overlaps with the sequence of LSPs (sequence D). In our study we confirm the existence
of a PL sequence containing contact binaries with red giant components (Eq. 4.1) and find
evidence for a possible additional PL sequence of contact binaries located ∼ 1 mag fainter.
73
4.6. STRUCTURE OF THE LMC FROM “HOT” ECLIPSING BINARIES ANDCLASSICAL CEPHEIDS
Furthermore, thanks to the depth achieved by the VMC data, we are able to extend the PL
relation of contact binaries, containing red giants, to Ks ∼ 18 mag, roughly two magnitudes
fainter than in Derekas et al. (2006). The existence of PL relation(s) for red giant EBs and
its absence for HEBs could be explained by intrinsic differences occurring between the two
samples. In the case of contact systems with red giants the total luminosity of the binary
system is dominated by one component - the red giant star, the luminosity of the second
component being negligible. On the contrary, for HEBs the ratio of luminosities of the two
O-B components could vary significantly. Therefore, the scatter of the PL relation of bi-
naries with O-B components is expected to be much larger than the scatter of the PLKs
relation of contact systems with a red giant component.
4.6 Structure of the LMC from “hot” eclipsing binaries and Clas-sical Cepheids
The distribution of the LMC CCs and HEBs is presented in Figure 4.12. As it was discussed
in the previous sections, we suggested that the EROS-2 candidate CCs with colour 0.2 ≤
(BEROS−REROS) ≤ 1 mag are bona-fide CCs. The upper-left panel of Figure 4.12 shows
the distribution of CCs in the LMC. CCs are relatively young objects (50-200 Myr), so they
trace the bar of the galaxy and the spiral arm. In the upper-right panel of Figure 4.12 the
distribution of 1768 HEBs from our sample is shown. It differs from the distribution of
CCs as it could be seen on the bottom-left panel of Figure 4.12 . HEBs are more clustered,
do not follow the entire bar and locate in the regions of recent star formation activity, such
as 30 Doradus and Constellation III, and supergiant shells (SGS 11, SGS 7, SGS 3, SGS
12 and others). On the bottom-right panel of Figure 4.12 the distribution of objects which
were classified as contact-like binary stars is shown. It is similar to the distribution of the
whole sample of EBs. These results are in agreement with the Star Formation History of the
LMC. Harris & Zaritsky (2009) found that the bar of the LMC had partially active episodes
of star formation 5 Gyr, 500 Myr and 100 Myr ago. CCs in the bar were formed during the
last episode of star formation activity 100 Myr years ago, while the activity at 12 Myr is
dominated by 30 Doradus and the Constellation III regions, which are not related to the bar
and where the majority of binary stars from our sample is concentrated.
74
CHAPTER 4. ECLIPSING BINARIES IN THE LMC
-75
-70
-65
90 80 70
-75
-70
-65
90 80 70
-75
-70
-65
90 80 70
Figure 4.12 Distribution of CCs (black dots), HEBs (red dots) and contact-like binaries(blue dots) in the LMC.
75
Chapter 5
RR Lyrae stars in the VMC tile LMC5_5
RR Lyrae stars make useful distance indicators because of the existence of a MV − [Fe/H]
relation in the visual band and of a PLZ relation in the infrared passbands (see Subsec-
tion 1.5.2). In this chapter we present results of the analysis of 71 RR Lyrae stars located
in tile LMC 5_5, close to the bar of the galaxy, for which individual spectroscopically
determined [Fe/H] abundances exist in the literature (Gratton et al., 2004). Combining the
metallicities of these stars, precise periods from the OGLE III catalogue and multi-epoch Ks
photometry from the near-infrared VISTA survey of the Magellanic Clouds system (Cioni
et al., 2011) we derive a new near-infrared PLKsZ relation for RR Lyrae variables. In order
to check the impact of Gaia (Section 1.2) on the determination of the zero-points of the RR
Lyrae PLKsZ and MV − [Fe/H] relations, we simulate Gaia parallaxes for 25 RR Lyrae
stars in the Milky Way.
5.1 Data for RR Lyrae stars in the bar of the LMC
Optical photometry for the LMC RR Lyrae stars discussed in this chapter was obtained
using the Danish 1.54 meter telescope, the 3.6 m, and the VLT ESO telescopes, at two
different sky positions, hereafter called fields A and B. Both are located in tile LMC 5_5,
close to the bar of the galaxy (Clementini et al. 2003, Di Fabrizio et al. 2005). As a result,
accurate B, V and I light curves tied to the Johnson-Cousins standard system and pulsation
characteristics (period, epoch of maximum light, amplitudes and mean magnitudes; Di Fab-
rizio et al. 2005) for 125 RR Lyrae stars were obtained. Low-resolution spectra for 98 of
these RR Lyrae stars were collected by Gratton et al. (2004) using the FORS1 (FOcal Re-
ducer/low dispersion Spectrograph) instrument mounted at the ESO VLT. They were used
77
5.1. DATA FOR RR LYRAE STARS IN THE BAR OF THE LMC
to derive metal abundances by comparing the strength of the Ca II K line with that of the
H lines (Preston, 1959). For the calibration of the method, four Galactic globular clusters
with metallicities in the range [−2.06; −1.26] dex were used. The obtained metallicities are
tied to a scale, which is, on average, 0.06 dex more metal-rich than the Zinn & West (1984)
metallicity scale.
We cross-matched the sample of 98 RR Lyrae variables with known metallicities against
the catalogue of RR Lyrae stars observed by the OGLE III survey (Soszynski et al., 2009).
The OGLE III catalogue contains information about the position, photometric and pulsation
properties of 24906 RR Lyrae stars in the LMC (see Subsection 2.4.2). We found that,
respectively, 94, 2 and 2 objects are cross-identified with sources in the OGLE III catalogue
within a pairing radius of 1′′, 3′′ and 7′′. The 2 stars with a counterpart at more than 5′′
are OGLE-LMC-RRLYR-10345 and OGLE-LMC-RRLYR-10509; for these two stars we
checked both the OGLE III finding charts and Gratton et al. (2004) Figure 5 (field B1)
in order to understand if they are affected by any problem. Star OGLE-LMC-RRLYR-
10345 is an isolated lightly elongated star without any clear blending problem, while star
OGLE-LMC-RRLYR-10509 is very close to another source possibly making more difficult
to accurately locate the star center. Considering that Gratton et al. (2004) and OGLE III
periods for these 2 stars agree within 0.5%, we kept these stars in our sample.
We compared the periods of the 98 RR Lyrae stars provided by Di Fabrizio et al. (2005)
and those in the OGLE III catalogue (Soszynski et al., 2009). For 96 objects the periods
agree within ∼ 2%, while for two objects periods differ significantly. For star A6332 the
difference is ∼ 25% and for star A5148 it is ∼ 37% (star identifications are from Di Fabrizio
et al. 2005). Moreover, star A5148 has been classified as a first-overtone RR Lyrae star in
the OGLE III catalogue, and as a fundamental-mode RR Lyrae by Di Fabrizio et al. (2005).
Since accurately estimated periods and classifications play a key role in the current study,
we decided to discard these two objects from the following analysis.
Seven objects (B2811, B4008, B3625, B2517, A2623, A2119, A10360) in our sample
are classified as RRc by Di Fabrizio et al. (2005) and as RRe in the OGLE III catalogue.
We removed them from our analysis because of the uncertain classification. Furthermore,
since one of the main purposes of the current research is to study the PLKsZ relation of
RR Lyrae stars of ab- and c-types we also discarded seven objects, which were classified as
double-mode RR Lyrae stars (RRd) by Di Fabrizio et al. (2005): A7137, A8654, A3155,
A4420, B7467, B6470 and B3347. This left us with a final sample of 61 RRab and 21
78
CHAPTER 5. RR LYRAE STARS IN THE VMC TILE LMC 5_5
RRc stars, which have counterparts in the OGLE III catalogue. The period search for the
RR Lyrae stars in the OGLE III catalogue was performed using an algorithm based on
the Fourier analysis of the light curves (Soszynski et al., 2009). The uncertainties in the
OGLE III periods for the 82 RR Lyrae stars in our sample are declared to be less than
5× 10−6 days. Therefore we used the periods provided by the OGLE III catalogue in order
to fit the PLKsZ relation, and do not consider errors in the periods since they are negligible
in comparison to the other uncertainties.
In order to derive mean Ks magnitudes for the RR Lyrae stars in our sample we used
data from the VMC survey (Cioni et al. 2011, see Subsection 2.4.3). The majority of RR
Lyrae stars in our sample are located within the VMC tile LMC 5_5. PSF photometry of the
time-series data for this tile was performed on the homogenised epoch-tile images (Rubele
et al., 2012) using the IRAF Daophot (Stetson et al., 1990) packages. On each epoch-
tile image the PSF model was created using 2500 stars uniformly distributed, finally the
Daophot ALLSTAR routine was used to perform the PSF photometry on all epoch images
and time-series catalogues were correlated within a tolerance of one arcsec. We have cross-
matched our sample of 82 RR Lyrae stars against the PSF photometry catalogue of tile LMC
5_5. VMC counterparts for 71 objects were found within a pairing radius of 1′′. For 70 of
them we have 13 epochs in the Ks-band, and for one object (B4749) we have observations
only in 6 epochs.
We determined mean Ks magnitudes using Ks-band light curve templates for RR Lyrae
stars from Jones et al. (1996) to fit the 13 different epochs (6 for B4749) available for
the 71 stars. All available epochs were used in the present analysis. However, checks are in
progress to verify that photometric errors and varying observing conditions of the individual
epochs do not affect the derived PLKsZ relation. Jones et al. (1996) developed one Ks-band
light curve template for RRc variables and four different templates for RRab stars, the latter
vary depending on the Johnson V amplitude of pulsation (VJ ). Di Fabrizio et al. (2005)
provides amplitudes in the V passband (hereinafter, Amp(V )) for the majority but not all
the 71 RR Lyrae stars in our sample. Specifically, Amp(V ) of star A26715 is missing and
for five other objects (B6798, A16249, B1907, A28066, B24089) Di Fabrizio et al. (2005)
provided more than one value of amplitude, likely because these objects have photometric
problems, e.g. blends. On the other hand, the OGLE III catalogue provides Cousins I band
(IC) amplitudes [Amp(I)] for all the variables in our list. We have transformed them to VJ
79
5.1. DATA FOR RR LYRAE STARS IN THE BAR OF THE LMC
Figure 5.1 Distribution of the differences between the V -band amplitudes provided by DiFabrizio et al. (2005) and those derived by transforming to Amp(V ) the Amp(I) values inthe OGLE III catalogue.
amplitudes using the relation by Di Criscienzo et al. (2011):
Amp(V ) = 1.58×Amp(I) (5.1)
and have compared the derived Amp(V ) values with those published by Di Fabrizio et al.
(2005). This comparison is shown in Fig.5.1. The distribution of amplitude differences is
symmetric around the value zero and for the vast majority of sources is smaller than 0.1
mag. Only in a few extreme cases this difference is as large as 0.31 mag. Given the higher
completeness of OGLE III dataset, in order to fit templates to the light curves of the 71 RR
Lyrae stars in our sample we have thus adopted OGLE III epochs of maximum light and the
IC amplitudes transformed to VJ as discussed above. We also corrected for any phase shift
between template and data points when necessary. Examples of the Ks-band light curves of
RR Lyrae stars in our sample and their fitting templates are presented in Fig. 5.2.
In order to test the robustness of our determination of the Ks mean magnitudes using
templates, for a number of RR Lyrae stars with evenly sampled light curves mean Ks mag-
nitudes were also derived by Fourier fitting the light curves with GRATIS period search
package. This analysis showed that the Ks mean magnitudes derived with the GRATIS are
consistent within the errors with those obtained by applying templates, thus supporting our
80
CHAPTER 5. RR LYRAE STARS IN THE VMC TILE LMC 5_5
Figure 5.2 Examples of the Ks-band light curves of RR Lyrae stars in our sample. Identifi-cation numbers are from Di Fabrizio et al. (2005), periods are from the OGLE III catalogue(Soszynski et al., 2009) and are given in days. Solid (red) lines are best fitting templates.
81
5.1. DATA FOR RR LYRAE STARS IN THE BAR OF THE LMC
estimates of mean Ks magnitudes via template fitting.
After deriving the Ks mean magnitudes we performed the dereddening procedure. Clemen-
tini et al. (2003) estimated reddening values of E(B−V ) = 0.116±0.017 and 0.086±0.017
mag in fields A and B, respectively, using the method from Sturch (1966) and the colours
of the edges of the instability strip defined by the RR Lyrae variables. Applying the co-
efficients from Cardelli et al. (1989) of AK/AV = 0.114 and assuming a ratio of total to
selective absorption of RV = 3.1, we estimated the extinction in the Ks-band as:
AKs = 0.35 × E(B − V ) (5.2)
Table 5.1 summarizes the properties of the sample of 71 RR Lyrae stars. The first two
columns of the table give the identification of the stars in Di Fabrizio et al. (2005) and in the
OGLE III catalogue, respectively. The table also shows coordinates and classification of the
stars from the OGLE III catalogue, metallicity with errors from Gratton et al. (2004) and
dereddened mean Ks magnitudes, determined by template fitting, along with their errors.
82
CHAPTER 5. RR LYRAE STARS IN THE VMC TILE LMC 5_5
Star
OG
LEID
RA
DEC
Type
[Fe/
H]
σ[Fe/
H]
P⟨K
s,0⟩
σ⟨K
s,0⟩
(J20
00)
(J20
00)
(dex
)(d
ex)
(day
s)(m
ag)
(mag
)A
2866
5O
GLE
-LM
C-R
RLY
R-1
2944
5:22
:06.
55-7
0:27
:55.
6c
-0.6
30.
240.
3008
299
18.4
690.
014
A78
64O
GLE
-LM
C-R
RLY
R-1
3857
5:23
:39.
25-7
0:31
:38.
1c
-1.3
60.
220.
3129
458
18.5
040.
014
B49
46O
GLE
-LM
C-R
RLY
R-1
0621
5:18
:11.
08-7
0:59
:35.
6c
-1.1
10.
250.
3130
142
18.3
690.
008
A26
36O
GLE
-LM
C-R
RLY
R-1
3548
5:23
:09.
09-7
0:39
:08.
1c
-1.6
10.
290.
3154
437
18.5
580.
013
A88
37O
GLE
-LM
C-R
RLY
R-1
3326
5:22
:45.
70-7
0:30
:14.
3c
-1.5
20.
220.
3165
579
18.5
840.
011
A86
22O
GLE
-LM
C-R
RLY
R-1
3164
5:22
:28.
93-7
0:30
:35.
9c
-1.4
40.
280.
3212
334
18.4
050.
010
A72
31O
GLE
-LM
C-R
RLY
R-1
3680
5:23
:22.
42-7
0:32
:35.
4c
-1.4
60.
260.
3228
047
18.2
250.
011
A22
34O
GLE
-LM
C-R
RLY
R-1
3479
5:23
:01.
47-7
0:39
:44.
4c
-1.5
30.
180.
3228
060
18.3
230.
009
B47
49O
GLE
-LM
C-R
RLY
R-1
0406
5:17
:49.
73-7
1:00
:01.
4c
-1.4
50.
160.
3267
353
18.3
640.
014
A43
88O
GLE
-LM
C-R
RLY
R-1
2614
5:21
:31.
67-7
0:36
:46.
3c
-1.3
30.
270.
3417
737
18.3
950.
012
A10
113
OG
LE-L
MC
-RR
LYR
-140
465:
24:0
0.38
-70:
28:0
6.1
c-1
.52
0.25
0.35
0661
818
.237
0.01
2B
6255
OG
LE-L
MC
-RR
LYR
-101
115:
17:1
7.88
-70:
57:2
6.4
c-1
.52
0.16
0.35
3559
618
.297
0.01
0B
4179
OG
LE-L
MC
-RR
LYR
-101
425:
17:1
9.95
-71:
01:0
2.1
c-1
.53
0.27
0.35
4523
218
.150
0.00
9A
8812
OG
LE-L
MC
-RR
LYR
-131
505:
22:2
6.44
-70:
30:1
9.1
c-1
.23
0.24
0.35
4966
018
.254
0.01
3A
2671
5O
GLE
-LM
C-R
RLY
R-1
2593
5:21
:29.
33-7
0:29
:23.
4c
-1.3
90.
180.
3569
006
18.2
910.
012
A20
24O
GLE
-LM
C-R
RLY
R-1
3572
5:23
:11.
02-7
0:40
:03.
3c
-1.6
20.
260.
3590
534
18.2
440.
008
B61
64O
GLE
-LM
C-R
RLY
R-1
0612
5:18
:10.
17-7
0:57
:30.
7c
-1.8
80.
220.
3744
821
18.0
270.
008
A27
697
OG
LE-L
MC
-RR
LYR
-130
125:
22:1
4.03
-70:
28:3
5.0
c-1
.33
0.25
0.38
2570
018
.030
0.01
1A
1945
0O
GLE
-LM
C-R
RLY
R-1
3841
5:23
:37.
95-7
0:34
:06.
7ab
-0.7
60.
130.
3979
182
18.5
500.
011
B70
64O
GLE
-LM
C-R
RLY
R-1
0708
5:18
:18.
63-7
0:55
:58.
7c
-2.0
30.
200.
4004
744
17.9
970.
009
B69
57O
GLE
-LM
C-R
RLY
R-1
0702
5:18
:18.
08-7
0:56
:08.
7c
-1.4
80.
180.
4047
399
18.0
500.
008
B23
502
OG
LE-L
MC
-RR
LYR
-105
095:
18:0
0.25
-70:
54:3
1.0
ab-1
.55
0.14
0.47
2468
118
.249
0.00
8A
3061
OG
LE-L
MC
-RR
LYR
-137
045:
23:2
5.18
-70:
38:2
8.9
ab-1
.26
0.12
0.47
4441
018
.324
0.00
9B
1081
1O
GLE
-LM
C-R
RLY
R-1
0684
5:18
:16.
01-7
1:04
:27.
0ab
-1.4
20.
200.
4760
753
18.2
380.
009
B34
00O
GLE
-LM
C-R
RLY
R-1
0072
5:17
:14.
51-7
1:02
:26.
6ab
-1.4
50.
240.
4852
148
18.3
440.
011
A73
25O
GLE
-LM
C-R
RLY
R-1
3855
5:23
:39.
13-7
0:32
:24.
8ab
-1.1
80.
260.
4864
544
18.2
340.
009
B30
33O
GLE
-LM
C-R
RLY
R-1
0659
5:18
:14.
04-7
1:03
:00.
5ab
-1.2
60.
210.
4986
975
18.0
820.
008
B20
55O
GLE
-LM
C-R
RLY
R-1
0108
5:17
:17.
44-7
1:04
:50.
2ab
-1.7
00.
230.
5207
746
18.2
530.
010
A26
525
OG
LE-L
MC
-RR
LYR
-128
115:
21:5
2.50
-70:
29:2
8.7
ab-1
.41
0.22
0.52
2502
918
.140
0.00
8A
7211
OG
LE-L
MC
-RR
LYR
-130
925:
22:2
1.17
-70:
32:4
3.9
ab-1
.33
0.19
0.52
2685
718
.170
0.00
8
83
5.1. DATA FOR RR LYRAE STARS IN THE BAR OF THE LMCA
2767
OG
LE-L
MC
-RR
LYR
-136
345:
23:1
7.75
-70:
38:5
5.9
ab-1
.37
0.08
0.53
2587
118
.069
0.01
2B
2408
9O
GLE
-LM
C-R
RLY
R-1
0345
5:17
:43.
51-7
0:54
:02.
7ab
-1.4
80.
160.
5580
613
18.0
420.
009
A87
88O
GLE
-LM
C-R
RLY
R-1
3678
5:23
:22.
41-7
0:30
:14.
6ab
-1.6
10.
210.
5591
710
18.1
770.
011
A63
98O
GLE
-LM
C-R
RLY
R-1
3294
5:22
:40.
76-7
0:33
:50.
2ab
-1.4
00.
300.
5619
466
17.9
550.
008
A72
47O
GLE
-LM
C-R
RLY
R-1
3708
5:23
:25.
58-7
0:32
:33.
4ab
-1.3
80.
210.
5621
512
18.0
250.
008
A25
301
OG
LE-L
MC
-RR
LYR
-126
385:
21:3
4.00
-70:
30:2
4.5
ab-1
.58
0.27
0.56
3114
618
.279
0.00
9A
1538
7O
GLE
-LM
C-R
RLY
R-1
2603
5:21
:30.
43-7
0:37
:11.
3ab
-1.8
10.
120.
5635
914
18.0
370.
009
B22
917
OG
LE-L
MC
-RR
LYR
-107
135:
18:1
9.10
-70:
54:5
6.1
ab-1
.29
0.16
0.56
4680
318
.159
0.00
8A
9245
OG
LE-L
MC
-RR
LYR
-135
365:
23:0
7.67
-70:
29:3
6.5
ab-1
.27
0.18
0.56
7876
318
.043
0.00
9A
1289
6O
GLE
-LM
C-R
RLY
R-1
3330
5:22
:46.
15-7
0:38
:54.
9ab
-1.5
30.
100.
5719
281
18.1
470.
008
A76
09O
GLE
-LM
C-R
RLY
R-1
3941
5:23
:48.
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362
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418
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LE-L
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821
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LE-L
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2249
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LE-L
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9550
617
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0.01
0
84
CHAPTER 5. RR LYRAE STARS IN THE VMC TILE LMC 5_5A
8720
OG
LE-L
MC
-RR
LYR
-139
565:
23:5
0.19
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30:1
6.7
ab-1
.88
0.34
0.65
0817
417
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0.00
8B
7063
OG
LE-L
MC
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-109
735:
18:4
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55:5
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0.14
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4869
817
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0.01
0B
7620
OG
LE-L
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-105
415:
18:0
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0.12
0.65
6160
217
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0.00
7A
7477
OG
LE-L
MC
-RR
LYR
-140
685:
24:0
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32:0
8.6
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0.28
0.65
6408
417
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2829
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2758
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3196
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090.
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48O
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-LM
C-R
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3285
5:22
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120.
6623
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560.
008
A80
94O
GLE
-LM
C-R
RLY
R-1
3306
5:22
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7420
663
17.8
700.
008
Tabl
e5.
1:Pr
oper
ties
ofth
e71
RR
Lyra
est
ars
inth
eV
MC
tile
LMC
5_5
used
tode
rive
ane
wPLK
sZ
rela
tion
(Col
umn
1:Id
entifi
catio
nof
the
star
from
DiF
abriz
ioet
al.(
2005
);C
olum
n2:
Iden
tifica
tion
from
the
OG
LEII
Ica
talo
gue
(Sos
zyns
kiet
al.,
2009
);C
olum
n3:
Rig
htas
-ce
nsio
n(O
GLE
);C
olum
n4:
Dec
linat
ion
(OG
LE);
Col
umn
5:R
RLy
rae
type
;Col
umn
6:M
etal
licity
from
Gra
tton
etal
.(20
04);
Col
umn
7:Er
-ro
rofm
etal
licity
from
Gra
tton
etal
.(20
04);
Col
umn
8:Pe
riod
(OG
LE);
Col
umn
9:D
ered
dene
dm
eanK
sm
agni
tude
from
the
VM
Csu
rvey
;Col
-um
n10
:Err
orof
the
mea
nK
sm
agni
tude
).
85
5.2. PLKSZ RELATION OF RR LYRAE STARS IN THE LMC
5.2 PLKsZ relation of RR Lyrae stars in the LMC
5.2.1 Method
Using the dereddened mean Ks magnitudes of the 71 RR Lyrae stars derived as described
in Section 5.1, spectroscopically determined metallicities from Gratton et al. (2004) and ac-
curately estimated periods from the OGLE III catalogue (with RRc stars "fundamentalized"
by adding 0.127 to the logarithm of the period) we can now fit the PLKsZ relation. The fit
was performed using a Bayesian fitting approach developed by Max Palmer, PhD student of
the University of Barcelona. This method takes into account potentially significant intrinsic
dispersion of the data, not-negligible errors in two dimensions (Ks and [Fe/H]) and the pos-
sibility of inaccuracy in the formal error estimates (e.g. in the determination of the precision
metallicity estimates). The detailed description of the method is presented in Muraveva et
al. (2014b, submitted to AJ).
By applying this method we found the following relation between periods of pulsation,
metallicities and mean apparent Ks magnitudes determined with templates:
Ks,0 = (−2.70 ± 0.22)logP + (0.03 ± 0.06)[Fe/H]
+ (17.44 ± 0.05) (5.3)
The intrinsic dispersion of the relation is found to be 0.09 mag.
The projections of the PLKsZ relation (Eq. 5.3) on the Log(P )−Ks and Ks − [Fe/H]
planes is shown in Figure 5.3. The grey lines in the figure are lines of equal metallicity
(top) or equal period (bottom). The method finds the relation (values of A, B, and C for the
relation Ks = A logP+B [Fe/H]+C) in three dimensions (logP, Ks, and [Fe/H]). So each of
the grey lines in the top plot are Ks = A logP+B [Fe/H]+C for the full range of periods, at
the metallicity of each star (one line per star). Thus, by following the line up and down it
is seen how Ks changes with period at some specific metallicity. The lines do not always
cross the points on the diagram because the line is the result of the fit, and the points are
affected by errors and intrinsic dispersion so may be above or below the fit. In the bottom
plot the lines are Ks = A logP+B [Fe/H]+C for the full range of metallicity with logP taken
from each star.
It is worth noting that we find a very small dependence of the Ks magnitude on the
metallicity. However, the metal abundance range spanned by our RR Lyrae stars does not
86
CHAPTER 5. RR LYRAE STARS IN THE VMC TILE LMC 5_5
Figure 5.3 Projections of the PLKsZ relation (given in Eq. 5.3) on the Log(P) versus Ks
(top panel) and Ks versus [Fe/H] (bottom panel) planes. Grey lines represent lines of equalmetallicities (top panel) and periods (bottom panel).
reach the highest values (up to solar and supersolar) observed in the MW bulge and disk RR
Lyrae populations.
5.2.2 Zero-point of the PLKsZ relation
To use the derived PLKsZ relation for determining distances it is necessary to calibrate
its zero-point. This can be done in a number of different ways. In this study we follow
two different approaches: the first one is based on adopting a value for the distance of the
LMC; in the second approach we use the absolute magnitudes of Galactic RR Lyrae stars
for which trigonometric parallaxes have been measured with the HST/FGS (Benedict et al.,
2011). Both approaches have their advantages and disadvantages, we discuss them in the
following sections.
87
5.2. PLKSZ RELATION OF RR LYRAE STARS IN THE LMC
Zero-point based on the LMC distance
The measure of the distance to the LMC has been the subject of many studies (see Sec-
tion 2.3). A recent determination of direct distances to eight long-period EBs in the LMC
was presented by Pietrzynski et al. (2013) and claimed to be accurate to ∼ 2%: DLMC =
49.97 ±0.19 (stat) ± 1.11 (syst) kpc, corresponding to the distance modulus (m−M)0 =
18.494 ± 0.049 mag.
The RR Lyrae stars in our sample are located in a relatively small area close to the
center of the LMC bar. Neglecting depth/projection effects they can be considered as being
all at the same distance from us and close to late-type EBs (Pietrzynski et al., 2013), which
are all located relatively close to the barycentre of the LMC. In the following analysis we
adopted for the distance modulus of the LMC the value published by Pietrzynski et al.
(2013) and subtracted this value from the dereddened mean Ks apparent magnitudes of
our 71 RR Lyrae stars to derive absolute Ks magnitudes (MK ). Then by applying the
technique described in Section 5.2.1 we derived the relation between absolute magnitudes,
periods and metallicities obtaining for the zero-point the value of: −1.05 ± 0.05 mag (see
column 2 of Table 5.2). In using the late-type EBs to calibrate the RR Lyrae PLKsZ
relation we have implicitly assumed that RR Lyrae stars and EBs are at same distance from
us. However, when pushing for distance comparisons at a few percent level the effects
of sample size, spatial distribution, depth and geometric projection become important and
properly accounting for the internal structure of the LMC may become necessary (see e.g.
Fig. 2.1 for different features of the LMC structure traced by CCs, RR Lyrae stars and
HEBs).
Zero-point based on trigonometric parallaxes of Galactic RR Lyrae stars
In order to obtain an estimate of the PLKsZ relation zero-point which is independent from
the distance to the LMC and, in turn, be able to measure the distance to this galaxy from the
PLKsZ relation, it is necessary to know the RR Lyrae absolute magnitude with reasonable
accuracy. Trigonometric parallaxes remain the only direct method to measure distances and
hence derive absolute magnitudes (see Section 1.1). Benedict et al. (2011) derived absolute
trigonometric parallaxes for five Galactic RR Lyrae stars (RZ Cep, XZ Cyg, SU Dra, RR
Lyr and UV Oct) with the HST/FGS. With these parallaxes the authors estimated absolute
magnitudes in the K and V passbands, corrected for interstellar extinction and Lutz-Kelker-
Hanson bias (hereinafter LKH, Lutz & Kelker 1973, Hanson 1979). Absolute magnitudes
88
CHAPTER 5. RR LYRAE STARS IN THE VMC TILE LMC 5_5
Relation ZP from DLMC ZP from Benedict et al. (2011)MK = (−2.70± 0.22)logP + (0.03 ± 0.06)[Fe/H]Har + ZP (−1.05 ± 0.05) (−1.27± 0.08)
Table 5.2 Absolute calibration of the new PLKsZ relation.
in the Ks-band, periods and metallicities from Benedict et al. (2011), and the slopes of
the relation derived in Eq. 5.3 were used in order to determine a zero-point from each
of these five MW RR Lyrae stars. The metallicities in Benedict et al. (2011) are in the
Zinn & West metallicity scale and were converted to the metallicity scale in Gratton et
al. (2004) by adding 0.06 dex. The logarithm of the period of the RRc star RZ Cep was
"fundamentalized" by adding 0.127. Then we calculated the weighted mean of the five
zero-points, this corresponds to: −1.27 ± 0.08 mag (see column 3 of Table 5.2).
There is a difference of ∼ 0.2 mag between the two zero-points. In fact, if we apply our
PLKsZ relation with zero-point calibrated on Benedict et al. (2011) parallaxes to determine
the absolute magnitudes of the 71 RR Lyrae stars in our sample, we obtain a distance mod-
ulus for the LMC, determined as the weighted average of the distance moduli of these 71
RR Lyrae stars, of (m−M)0 = 18.71 ± 0.01 mag with σ = 0.09. This distance modulus
is about 0.2 mag longer than the widely adopted value of (m−M)0 = 18.5 mag.
There are a number of possible explanations for this discrepancy. First of all, we as-
sumed that all RR Lyrae stars in our sample are located at the same distance from us, equal
to the distance derived from the LMC EBs analysed by Pietrzynski et al. (2013). However,
the RR Lyrae stars could in fact be distributed along the whole depth of the LMC. Fur-
thermore, RR Lyrae stars and EBs from Pietrzynski et al. (2013) could reside in different
sub-structures of the LMC, which could be the reason for the systematic error in the deter-
mination of the zero-point. On the other hand, when calibrating the zero-point by applying
the parallaxes of the MW RR Lyrae stars by Benedict et al. (2011) we implicitly assume
that the PLKsZ relation is the same in the MW and in the LMC, which may not be true. It
is well known, in fact, that the LMC is in general more metal-poor than our Galaxy. The
difference in metal abundances could affect the PLKsZ relation of RR Lyrae stars. Indeed,
as mentioned above, the derived low metallicity dependence of our PLKsZ relation could
be due to the smaller metallicity range covered by the LMC RR Lyrae stars, that does not
reach the highest values of the Galactic variables.
We may also wonder whether there might be unknown systematic errors affecting Bene-
dict et al.’s parallaxes. These come from HST fields, which provide relative and not absolute
89
5.3. GAIA OBSERVATION OF RR LYRAE STARS IN THE MILKY WAY
trigonometric parallaxes. Absolute parallaxes of the reference stars in each field are esti-
mated via a complex procedure of fitting the spectral type and luminosity class of each star.
A general formal error of 0.5 mas is applied to the absolute parallax of the reference stars,
equal for all stars in all fields, and without justification. This could result in miscalculated
estimates of the precision of the final absolute parallax measurements of the five RR Lyrae
stars. The Lutz-Kelker bias is corrected a posteriori. In this respect it is worth of notice
that, according to van Leeuwen (2007), Hipparcos parallax of RR Lyrae itself, the only RR
Lyrae variable for which the satellite could measure the parallax with some precision (±
0.64 mas), is about 0.31 mas smaller than (Benedict et al., 2011)’s parallax for this star,
although consistent with it within the errors, hence, the corresponding distance modulus is
about 0.17 mag longer. In any case, a great contribution to the determination of the zero-
point of the RR Lyrae PLKsZ relation is expected from the ESA astrometric satellite Gaia.
We discuss this topic in Section 5.3.
We compared our new PLKsZ relation (Table 5.2) with the relations in the literature
(see Section 1.5.2). The slope in period of the RR Lyrae PLKsZ relation differs signifi-
cantly in different studies. The value derived in the present study is in excellent agreement
with that derived by Del Principe et al. (2006). Metallicities in all studies, but Sollima et al.
(2008) one, are on the Zinn & West scale, while in the current study are on a scale, which
is systematically 0.06 dex higher than the Zinn & West one. Since the difference between
two scales is small, this should not affect significantly the results of this comparison. The
dependence on metallicity of the PLKsZ relation also varies significantly among the dif-
ferent studies. Our slope in metallicity is the smallest among all previous studies and it is
closer to that found by Borissova et al. (2009).
5.3 Gaia observation of RR Lyrae stars in the Milky Way
The Gaia astrometric satellite will revolutionise many fields of astronomy (Perryman et al.,
2001). Of particular importance will be its catalogue of trigonometric parallaxes for more
than one billion stars, with astrometric precision to the µas level (see Section 1.2). Due
to Gaia’s constant observation of the sky over the five-year nominal mission, the satellite
will repeatedly observe all stars brighter than its limiting magnitude, with an average of 80
observations per star. This will also make it possible for Gaia to discover and characterise
many types of variables, including RR Lyrae stars and Cepheids.
90
CHAPTER 5. RR LYRAE STARS IN THE VMC TILE LMC 5_5
Gaia is observing in the broad visual band G (Jordi et al., 2010) for its astrometric mea-
surements, and is therefore not ideal for characterising the RR Lyrae PLZ relation, which
exists only in the infrared passbands. However, since Gaia will provide accurate parallaxes
for an expected tens of thousands of MW RR Lyrae stars, it could serve as a perfect tool for
the determination of the zero-point of the PLKsZ relation through the combination with
external datasets. Moreover, Gaia will contribute significantly to the determination of the
luminosity-metallicity relation of RR Lyrae stars in the visual passband. The current largest
limiting factor in the zero-point calibration of the PLKsZ and MV − [Fe/H] relations is the
lack of a reliable and statistically significant sample of parallax measurements. The current
state of the art is the sample of five RR Lyrae parallaxes from Benedict et al. (2011) using
the HST. Gaia will improve this situation by several orders of magnitude in both precision
and numbers of objects.
In order to study the impact of Gaia in the determination of the PMKsZ and MV −
[Fe/H] relations we have selected a sample of 25 bright Galactic fundamental-mode RR
Lyrae stars with known metallicities and photometry in the Ks and V bands. We estimated
distances to the selected variables by comparing apparent and absolute magnitudes deter-
mined on the basis of the PMKsZ relation derived in this thesis work (Table 5.2) and the
MV − [Fe/H] relation (Eq. 14) in Benedict et al. (2011). Then we simulated parallaxes
along with their errors for the selected RR Lyrae stars, assuming nominal Gaia mission
performance. The simulation of Gaia parallaxes was performed by M. Palmer, using the
Gaia Object Generator (GOG; Luri et al. 2014, see Subsection 5.3.1). By using simulated
parallaxes including observational errors we recalculated the PMKsZ and MV − [Fe/H]
relations and compare them with those used for the estimate of parallaxes. This exercise
is designed to show if parallaxes determined with Gaia will allow us to derive the "true"
PMKsZ and MV − [Fe/H] relations.
Information about the 25 RRab stars in the MW, for which we simulate Gaia parallaxes,
is presented in Table 5.3. Stars listed in this table were selected because they are close and
bright enough (V<11.5 mag) to have Gaia parallaxes determined better than 2-3%. More-
over, these objects have spectroscopically derived metallicities and are the least reddened of
the nearby RR Lyrae stars. Many of them have been analysed in radial velocities and Baade-
Wesselink studies, and they do not exhibit a strong Blazko effect (Blazko, 1907). Three of
these stars are part of the sample used in this thesis work to calibrate the zero-point of the
PLKsZ relation (see Subsection 5.2.2).
91
5.3. GAIA OBSERVATION OF RR LYRAE STARS IN THE MILKY WAY
Feast et al. (2008) derived mean Ks magnitudes of these RR Lyrae stars, by using single-
epoch Ks photometry from 2MASS (Cutri et al. 2003), ephemerides of the stars, amplitudes
in the visual passband and template fitting of the Ks light curves. Feast et al. (2008) com-
pared the derived mean Ks magnitudes with those obtained by Fernley et al. (1993), and
declare that the difference is 0.008 ± 0.0015 mag. For comparison, the average error of
the dereddened mean Ks magnitudes of our sample of 71 RR Lyrae stars in the LMC (Ta-
ble 5.1), derived by applying templates, is 0.009 mag. Since Feast et al. (2008) did not
provide the errors for the mean Ks magnitudes of the individual RR Lyrae stars in their
sample, we assumed a worse case scenario with an error of ∼ 0.01 mag and consider this
value in the determination of absolute magnitudes in the Ks passband. Feast et al. (2008)
also provided information about the reddening of the 25 RR Lyrae stars. We used these val-
ues of reddening, but since these RR Lyrae stars have small values of reddening, especially
in the Ks passband, we consider the errors in the reddening to be negligible.
We performed the transformation from the 2MASS system to the VISTA system, by
using mean Ks and J magnitudes (Feast et al., 2008) and applying the empirical relations
provided by the Cambridge Astronomy Survey Unit (CASU)1:
Ks(V ISTA) = Ks(2MASS) + 0.010 × (J −Ks)(2MASS) (5.4)
Metallicities for the 25 RR Lyrae stars, calibrated to the Zinn & West metallicity scale, were
determined spectroscopically by Layden (1994). We converted them to the metallicity scale
of our sample of 71 RR Lyrae stars by adding 0.06 dex (Gratton et al., 2004). The periods
of the RR Lyrae variables are taken from Feast et al. (2008), and coordinates are from the
SIMBAD database.
5.3.1 Simulated Gaia data
GOG (Luri et al., 2014) is designed to simulate both individual Gaia observations and the
full contents of the end-of-mission catalogue (see Section 1.2). GOG is capable of deter-
mining the expected precision in astrometric, photometric and spectroscopic observations
of Gaia. In general, the precision depends on the apparent magnitude of the star, its colour,
and its sky position, which affects the number and type of observations made (due to the
Gaia scanning law).
1http://casu.ast.cam.ac.uk/surveys-projects/vista/technical/photometric-properties
92
CHAPTER 5. RR LYRAE STARS IN THE VMC TILE LMC 5_5
To obtain an absolute magnitude for each RR Lyrae star in our sample of 25 bright MW
variables, we used:
MKs = −2.70logP + 0.03[Fe/H] − 1.05 (5.5)
as determined in Table 5.2 and the zero-point fixed by the distance to the LMC. We then
obtained a distance by combining this absolute magnitude with the apparent magnitude and
extinction as defined above. Colour information as (V-I) was obtained from the Hipparcos
catalogue (Perryman and ESA, 1997) where available. The apparent magnitude, position,
colour, period, and metallicity data form the basis of a synthetic catalogue of RR Lyrae
stars, along with the distance obtained from the PMKsZ relation, and is used as the input
catalogue of ‘true’ parameters for GOG. GOG then creates simulated Gaia observations for
our sample. We take the PMKsZ relation (Eq. 5.5) as true, as a study of the possible
precision in PLKsZ calibration after the Gaia data will become available.Table 5.3 gives
the MKs magnitudes and parallaxes of the 25 MW RR Lyrae stars.
Using the fitting method described in Sect. 5.2.1 to the data including the simulated par-
allax observations and simulated errors applied to parallax, metallicity and apparent magni-
tude, we find a PMKsZ relation of:
MKs = (−2.70 ± 0.07)logP + (0.028 ± 0.008)[Fe/H]
+ (−1.01 ± 0.03) (5.6)
Comparison of these results to the input PLKsZ relation shows very good agreement.
This shows that the capabilities of fitting the absolute PLKsZ relation using Gaia parallaxes
for the 25 selected MW RR Lyrae stars will allow a precision in the zero-point of around
0.03 mag. Moreover, this is an additional test that the fitting procedure given in Sect. 5.2.1
is accurate and unbiased.
93
5.3. GAIA OBSERVATION OF RR LYRAE STARS IN THE MILKY WAY
Star
RA
DEC
πH
ipparcos
σH
ipparcos
πGaia
σGaia
E(B
-V)
P[F
e/H
]σ[F
e/H]
Ks,VIS
TA
MK
σM
KM
VσM
V
(deg
)(d
eg)
(mas
)(m
as)
(mas
)(m
as)
(mag
)(d
ay)
(dex
)(d
ex)
(mag
)(m
ag)
(mag
)(m
ag)
(mag
)R
RLy
r29
1.36
630
42.7
8436
3.46
0.64
4.15
10.
007
0.03
00.
5668
39-1
.31
0.08
6.49
2-0
.428
0.01
10.
494
0.01
1X
Ari
47.1
2869
10.4
4590
0.88
1.32
1.96
10.
019
0.18
00.
6511
54-2
.34
0.09
7.94
5-0
.655
0.02
30.
308
0.02
7R
XEr
i72
.434
55-1
5.74
118
1.50
1.12
1.68
50.
020
0.05
80.
5872
46-1
.24
0.16
8.43
2-0
.455
0.02
70.
502
0.01
3SW
And
5.92
954
29.4
0101
1.48
1.21
1.90
70.
021
0.03
80.
4422
62-0
.32
0.17
8.50
8-0
.103
0.02
60.
709
0.01
3SV
Eri
47.9
6711
-11.
3539
11.
481.
671.
370
0.00
60.
085
0.71
3865
-1.9
80.
078.
645
-0.7
010.
014
0.33
90.
014
RR
Cet
23.0
3405
1.34
173
-1.2
91.
351.
627
0.02
30.
022
0.55
3030
-1.4
60.
128.
523
-0.4
280.
032
0.47
30.
014
DX
Del
311.
8681
512
.464
080.
771.
381.
695
0.00
50.
092
0.47
2619
-0.5
00.
128.
689
-0.1
980.
012
0.65
70.
012
SUD
ra17
4.48
586
67.3
2974
0.20
1.13
1.42
50.
005
0.01
00.
6604
18-1
.68
0.14
8.62
2-0
.613
0.01
20.
413
0.01
3X
ZC
yg29
3.12
211
56.3
8819
2.29
0.84
1.67
00.
021
0.09
60.
4666
10-1
.46
0.11
8.72
5-0
.195
0.02
90.
456
0.01
2V
YSe
r23
2.75
803
1.68
382
-1.2
81.
571.
235
0.00
70.
040
0.71
4101
-1.7
60.
238.
830
-0.7
250.
016
0.40
80.
017
VIn
d31
7.87
460
-45.
0745
51.
571.
471.
440
0.00
70.
043
0.47
9604
-1.4
40.
118.
988
-0.2
350.
014
0.46
90.
015
XZ
Dra
287.
4275
464
.858
932.
260.
881.
361
0.00
70.
062
0.47
6497
-0.8
10.
099.
150
-0.2
020.
015
0.59
00.
016
BH
Peg
343.
2543
215
.787
940.
311.
821.
194
0.00
80.
077
0.64
0991
-1.3
20.
219.
070
-0.5
720.
018
0.49
80.
016
SWD
ra18
4.44
429
69.5
1062
-0.4
61.
291.
131
0.00
70.
014
0.56
9671
-1.1
80.
079.
322
-0.4
160.
016
0.51
20.
015
SVH
ya18
7.62
710
-26.
0475
44.
491.
761.
226
0.00
80.
080
0.47
8542
-1.6
40.
279.
369
-0.2
160.
018
0.42
30.
017
RUSc
l0.
7004
6-2
4.94
530
-0.1
11.
421.
275
0.00
70.
018
0.49
3347
-1.1
90.
139.
231
-0.2
470.
016
0.52
20.
017
AVPe
g32
8.01
164
22.5
7483
2.28
1.72
1.39
70.
006
0.06
70.
3903
78-0
.08
0.22
9.34
90.
051
0.01
40.
755
0.01
4X
XA
nd19
.364
2338
.950
562.
541.
900.
953
0.00
60.
039
0.72
2755
-1.9
50.
079.
412
-0.7
050.
016
0.37
20.
017
RVO
ct20
6.63
230
-84.
4017
71.
321.
321.
057
0.00
60.
180
0.57
1169
-1.2
80.
259.
530
-0.4
130.
016
0.50
70.
017
RS
Boo
218.
3883
931
.754
620.
111.
401.
298
0.00
50.
012
0.37
7339
-0.2
60.
319.
509
0.07
10.
013
0.71
60.
012
WY
Ant
154.
0206
1-2
9.72
845
-0.2
41.
610.
956
0.00
60.
059
0.57
4341
-1.6
00.
209.
677
-0.4
410.
017
0.42
30.
018
UY
Boo
209.
6930
712
.951
791.
001.
800.
866
0.00
60.
033
0.65
0889
-2.4
30.
169.
726
-0.5
970.
018
0.27
00.
022
RYC
ol78
.782
42-4
1.62
824
1.36
1.34
1.05
30.
006
0.02
60.
4788
32-1
.05
0.17
9.70
5-0
.193
0.01
60.
536
0.01
9D
NA
qr34
9.82
168
-24.
2163
31.
822.
110.
809
0.00
80.
025
0.63
3757
-1.5
70.
159.
903
-0.5
660.
024
0.43
10.
022
AN
Ser
238.
3793
812
.961
15-1
.71
2.93
0.94
90.
007
0.04
00.
5220
690.
020.
219.
845
-0.2
830.
019
0.78
80.
018
Tabl
e5.
3:Pr
oper
tieso
f25
brig
htfu
ndam
enta
l-mod
eR
RLy
rae
star
sin
the
MW
(Col
umn
1:N
ame
ofth
est
ar;C
olum
n2:
Rig
htA
scen
sion
(J20
00)f
rom
SIM
BAD
data
base
;Col
umn
3:D
eclin
atio
n(J
2000
)fro
mSI
MBA
Dda
taba
se;C
olum
n4:
Para
llaxe
sfr
omth
ere
vise
dH
ip-
parc
osca
talo
gue
(van
Leeu
wen
,200
7);
Col
umn
5:Er
rors
ofpa
ralla
xes
from
Hip
parc
osca
talo
gue
(van
Leeu
wen
,200
7);C
olum
n6:
Gai
apa
ralla
xes
sim
ulat
edus
ing
Eq.5
.5;C
ol-
umn
7:Si
mul
ated
erro
rsof
Gai
apa
ralla
xes;
Col
umn
8:R
edde
ning
from
Feas
teta
l.(2
008)
;C
olum
n9:
Perio
dsfr
omFe
aste
tal.
(200
8);C
olum
n10
:M
etal
licity
from
Layd
en(1
994)
calib
rate
dto
the
met
allic
itysc
ale
ofth
e71
LMC
RR
Lyra
est
ars
byad
ding
0.06
dex;
Col
-um
n11
:Err
orsi
nm
etal
licity
from
Layd
en(1
994)
;Col
umn
12:K
sap
pare
ntm
agni
tude
inth
eV
ISTA
syst
em;C
olum
n13
:C
alcu
late
dab
solu
tem
agni
tude
inth
eK
spa
ssba
nd;C
ol-
umn
14:E
rror
sin
the
abso
luteK
sm
agni
tude
;Col
umn
15:C
alcu
late
dab
solu
tem
agni
tude
inth
eVJ
pass
band
;Col
umn
16:E
rror
sin
the
abso
luteVJ
mag
nitu
de).
94
CHAPTER 5. RR LYRAE STARS IN THE VMC TILE LMC 5_5
5.3.2 Simulation of the MV − [Fe/H] relation of RR Lyrae stars in the MilkyWay
We applied the same approach in order to check if it will be possible to derive the MV −
[Fe/H] relation of RR Lyrae stars by using Gaia data. We used metallicities from Layden
(1994) and apparent V magnitudes from Fernley et al. (1998b). Fernley et al. (1998b) mean
V magnitudes were derived from the Hipparcos photometry and compared with mean V
magnitudes for 11 RRab and 2 RRc stars from Liu & Janes (1990). The mean difference
was found to be 0.003 mag with an rms scatter of 0.007 mag (Fernley et al., 1998b). We
assume a conservative error on the apparent mean magnitudes of ∼ 0.01 mag and consider
this value in the determination of absolute magnitudes in the V passband. We applied the
values of reddening E(B-V) from Feast et al. (2008) and determined the extinction using the
relation:
AV = 3.1E(B − V ) (5.7)
In order to obtain absolute MV magnitudes for the 25 RR Lyrae stars we applied the
relation in Benedict et al. (2011):
MV = (0.214 ± 0.047)([Fe/H] + 1.5) + (0.45 ± 0.05), (5.8)
where the metallicity is in the Zinn & West scale. Eq. 5.8 was derived using the slope
obtained by Gratton et al. (2004) and the zero-point determined from the HST parallaxes
of the five MW RR Lyrae stars measured by Benedict et al. (2011). Applying the proce-
dure described in Section 5.3.1 we simulated Gaia parallaxes and related errors of the 25
RR Lyrae stars. To fit the relation we used the method developed by M. Palmer for two
dimensions and determined a new MV − [Fe/H] relation:
MV = (0.208 ± 0.003)([Fe/H] + (0.779 ± 0.005) (5.9)
As it could be seen using Gaia parallaxes for only 25 RR Lyrae variables will allow us
to recover the slope of the relation within 3%, and to recover the zero-point to within 1%.
Obviously a larger sample of RR Lyrae stars with Gaia parallaxes will allow us to determine
the MV − [Fe/H] and PLKsZ relations with much greater precision. The main issues in
95
5.3. GAIA OBSERVATION OF RR LYRAE STARS IN THE MILKY WAY
the future will be concerned with the accurate estimate of metallicities, mean Ks and V
magnitudes, and reddening.
96
Chapter 6
RR Lyrae stars in the VMC tile LMC8_3
6.1 Classification of EROS-2 candidate RR Lyrae stars
The EROS-2 survey provided light curves in the BEROS and REROS passbands for 16337
candidate RR Lyrae stars in the LMC, selected from EROS-2 catalogue of candidate vari-
ables on the basis of the BEROS , BEROS − REROS CMD (see left panel of Figure 2.3).
We crossmatched the EROS-2 catalogue of candidate RR Lyrae stars against the VMC cat-
alogue (internal VMC release from 5 August 2013) and found 5570 sources in common.
Among them we selected objects which are located in the tile LMC 8_3 (291 stars in total).
After discarding objects with periods longer than 4.1 days1, we obtained a sample of 268
candidate RR Lyrae stars which have a counterpart in the VMC catalogue. This sample in-
cludes also star lm0303n13977 which according to EROS-2 should have a period PEROS =
918.06335 days. However, in the OGLE III catalogue this star is listed among the RR Lyrae
stars with a period around half a day. We visually inspected the EROS-2 light curve of the
star with GRATIS and derived a new period P = 0.499556 days which in excellent agreement
with OGLE III’s. By applying Eqs. 2.1 and 2.2 we transformed the BEROS and the REROS
magnitudes to Johnson V magnitudes and analysed the light curves of the 268 candidate
RR Lyrae stars in the BEROS and V passbands with GRATIS. We corrected the period
provided by the EROS-2 survey for four stars, namely: lm0303n13977, lm0434l20435,
lm0301l25140 and lm0291l26545. Through the visual inspection of the light curves we
performed a preliminary classification of RRab, RRc, RRd stars and misclassified objects,
which light curves do not have the characteristic shape of a RR Lyrae star. According to the
1This limit in period was chosen as to include typical periods of RR Lyrae stars and their most frequentaliases.
97
6.1. CLASSIFICATION OF EROS-2 CANDIDATE RR LYRAE STARS
visual inspection of the light curves, our sample includes 252 confirmed RR Lyrae stars and
16 misclassified sources which mainly are EBs.
To classify the 268 candidate RR Lyrae stars we also plotted them on the LogP versus
AmpV diagram, (see Fig. 6.1). In this figure one can distinguish three main groups of
objects:
• LogP < −0.7 and LogP > −0.05: misclassified objects
• −0.7 ≤ LogP ≤ −0.3 and Amp(V ) ≤ 0.8 mag: RRc stars
• −0.4 ≤ LogP ≤ −0.3 and Amp(V ) > 0.8 mag or −0.3 ≤ LogP ≤ 0.05: RRab
stars
Twelve sources lie outside both the RRab and the RRc regions. All of them but one were
classified as non-RR Lyrae stars by the visual inspection of the light curves with GRATIS.
One object among these 12 stars (lm0291n13464) was classified as RRc after analysis of the
light curve. However, the star is located outside the regions of RR Lyrae stars in the period-
amplitude diagram (Figure 6.1), hence, we discarded it. Five objects (lm0434m21890,
lm0300n19430, lm0303k15709, lm0303n10802, lm0303l25724) were classified as RRab
with the period-amplitude diagram, but after the analysis with GRATIS they all were dis-
carded, since they are misclassified sources. Similarly, ten stars were classified as c-type
RR Lyrae stars with the period-amplitude diagram, but the analysis with GRATIS showed
that they are in fact RRd stars. Information about these RRd stars and the comparison with
the OGLE III catalogue, for those which were observed also by the OGLE III survey, is
presented in Table 6.1.
The final catalogue of confirmed RR Lyrae stars in tile LMC 8_3, for which EROS-2 and
VMC data are available contains 251 sources. The sample includes 167 RRab, 74 RRc and
10 RRd stars. For each star we derived mean magnitudes, amplitudes, epochs of maximum
light in the BEROS and V passbands. Some of these parameters and the classification in
type of the 251 RR Lyrae stars are presented in Table 6.2.
98
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3
EROS-2 id P1 P0 P1/P0 OGLE III P1 OGLE III P0 OGLE III P1/P0
lm0293k.30764 0.353758 0.475592 0.7438 0.3537438 0.4755950 0.7438lm0435k.8479 0.365147 0.490433 0.7445 - - -lm0444l.8138 0.354920 0.476967 0.7441 - - -lm0293n.14230 0.362863 0.487836 0.7438 0.3629116 0.4878202 0.7440lm0310l.12653 0.362132 0.486196 0.7448 0.3621078 0.4861951 0.7448lm0303m.23391 0.385532 0.516902 0.7459 0.3855124 0.5168991 0.7458lm0303k.24363 0.391872 0.524815 0.7467 0.3918820 0.5247920 0.7467lm0301n.13911 0.357182 0.479980 0.7442 - - -lm0291n.25922 0.365509 0.490849 0.7446 - - -lm0301l.26933 0.360587 0.484494 0.7443 0.3605884 0.4844985 0.7443
Table 6.1 RRd stars in tile LMC 8_3. (Column 1: EROS-2 identification number; Column 2:First-overtone period derived with GRATIS; Column 3: Fundamental mode period derivedwith GRATIS; Column 4: Ratio of the periods; Column 5: First-overtone period from theOGLE III catalogue; Column 6: Fundamental mode period from the OGLE III catalogue ;Column 7: Ratio of the periods from the OGLE III catalogue).
Figure 6.1 Period-amplitude diagram of the 268 candidate RR Lyrae stars in tile LMC 8_3.Misclassified objects discarded from the following analysis include: short period variables(crosses) and EBs (squares).
99
6.1. CLASSIFICATION OF EROS-2 CANDIDATE RR LYRAE STARS
ERO
S-2
idR
AD
ECPe
riod
⟨BEROS⟩
Amp(B)
⟨V⟩
Amp(V)
Epoc
h(m
ax)
Type
(deg
)(d
eg)
(day
s)(m
ag)
(mag
)(m
ag)
(mag
)V
lm03
01n1
6576
77.0
3389
-66.
4998
20.
2366
4518
.75
0.21
18.8
70.
2624
5216
4.74
65c
lm03
05m
3332
76.8
9820
-66.
9698
10.
2493
1119
.51
0.36
19.6
70.
4524
5119
3.58
67c
lm03
00l1
5247
75.8
0446
-66.
5037
00.
2709
2019
.35
0.35
19.4
50.
4424
5158
9.65
12c
lm04
36l1
7456
76.2
2323
-66.
1816
90.
2773
1919
.55
0.61
19.6
00.
7124
5192
2.67
09c
lm02
93l1
8421
74.7
9358
-66.
8607
20.
2787
5919
.07
0.33
19.1
60.
3924
5229
8.65
45c
lm04
37m
2212
677
.398
74-6
6.06
973
0.28
0684
19.4
20.
4719
.52
0.58
2451
745.
8545
clm
0425
l243
8975
.464
57-6
5.86
768
0.28
1388
19.0
50.
3919
.12
0.47
2451
593.
6165
clm
0427
m19
332
75.9
2683
-66.
0407
30.
2865
4619
.11
0.36
19.1
60.
4324
5190
6.90
71c
lm04
35m
1088
877
.488
19-6
5.61
824
0.28
9555
19.1
60.
3719
.24
0.46
2451
927.
6789
clm
0425
l205
1375
.501
09-6
5.84
096
0.28
9973
18.8
20.
4718
.87
0.59
2450
508.
6286
clm
0423
l200
6975
.597
47-6
5.49
339
0.29
1086
19.0
80.
5119
.13
0.60
2451
467.
6728
clm
0302
n485
876
.137
49-6
6.78
444
0.29
2002
19.0
00.
4519
.05
0.56
2451
493.
6596
clm
0291
k248
6275
.000
92-6
6.40
342
0.29
3334
19.6
80.
4220
.02
0.56
2451
128.
6539
clm
0435
m91
0977
.321
64-6
5.60
798
0.29
5152
18.9
20.
4819
.02
0.56
2450
706.
7920
clm
0434
n143
1076
.706
55-6
5.80
327
0.29
6573
19.2
00.
4019
.28
0.52
2451
905.
5749
clm
0291
l119
4074
.899
17-6
6.47
166
0.30
3318
19.2
00.
4819
.31
0.57
2451
886.
5948
clm
0424
m19
442
75.1
0627
-65.
6782
00.
3046
0519
.29
0.44
19.4
10.
6124
5118
2.68
72c
lm04
25n1
5519
75.7
8383
-65.
8018
40.
3075
0719
.00
0.43
19.0
80.
4824
5183
0.71
42c
lm02
91n2
5551
75.1
1817
-66.
5556
60.
3083
2218
.90
0.45
19.0
30.
5324
5188
5.60
54c
lm04
25n1
8680
75.9
2700
-65.
8217
30.
3103
6619
.24
0.54
19.2
70.
7124
5159
1.62
72c
lm03
04m
2952
75.9
4720
-66.
9718
50.
3119
4419
.08
0.41
19.2
10.
5224
5120
7.61
61c
lm03
03n3
1583
77.1
4986
-66.
9305
00.
3141
8019
.15
0.45
19.1
90.
5324
5230
7.63
81c
lm03
01n7
929
76.8
9016
-66.
4461
00.
3142
7119
.14
0.47
19.2
40.
5524
5087
1.57
79c
lm04
25k9
319
75.4
7239
-65.
6096
70.
3196
9719
.55
0.55
19.7
50.
6924
5147
8.61
92c
lm04
34l2
3190
76.2
3528
-65.
8782
70.
3225
9519
.27
0.46
19.3
30.
5124
5202
0.51
10c
lm03
03m
2250
477
.154
98-6
6.72
917
0.32
3404
19.4
50.
4419
.46
0.51
2452
204.
7726
clm
0425
n137
5375
.738
00-6
5.79
020
0.32
4285
19.5
10.
4619
.56
0.59
2451
125.
6205
clm
0303
n168
4177
.102
76-6
6.84
558
0.32
7493
19.2
30.
3819
.33
0.46
2451
078.
7631
clm
0291
n154
1275
.414
71-6
6.49
017
0.32
8223
19.3
10.
4119
.46
0.50
2451
124.
7292
clm
0300
m68
0876
.005
54-6
6.28
864
0.32
9139
19.1
80.
3719
.26
0.46
2451
491.
6430
c
100
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3lm
0301
m15
847
77.1
2213
-66.
3411
20.
3300
7719
.11
0.54
19.2
10.
6424
5119
9.56
39c
lm04
36m
8308
76.7
2609
-65.
9659
90.
3316
1919
.11
0.45
19.3
90.
5424
5177
4.83
16c
lm03
12l1
5193
77.4
2594
-66.
8571
60.
3317
8019
.36
0.47
19.5
10.
5124
5156
5.63
91c
lm04
25k4
625
75.5
5453
-65.
5751
80.
3355
3719
.18
0.36
19.3
00.
4324
5162
3.54
79c
lm04
23l1
7670
75.3
4933
-65.
5021
00.
3375
9419
.05
0.42
19.1
80.
5024
5224
9.80
13c
lm02
93m
1980
375
.410
86-6
6.71
085
0.33
8538
19.1
60.
4619
.21
0.56
2451
838.
7084
clm
0303
l865
576
.693
37-6
6.80
070
0.33
9125
18.4
80.
2118
.54
0.24
2451
563.
6306
clm
0310
n115
8577
.668
64-6
6.49
466
0.34
0596
19.0
60.
1819
.23
0.32
2451
271.
5430
clm
0300
l675
375
.824
56-6
6.44
405
0.34
0936
18.7
70.
3518
.89
0.41
2451
383.
8448
clm
0436
l159
9376
.372
96-6
6.17
058
0.34
3821
19.2
10.
3719
.31
0.41
2451
886.
6258
clm
0302
l163
9575
.662
04-6
6.86
281
0.34
4601
19.1
40.
3819
.28
0.42
2452
239.
5837
clm
0303
m10
773
76.9
4934
-66.
6602
70.
3449
4219
.09
0.42
19.1
40.
5024
5106
7.75
97c
lm04
25l6
481
75.3
1167
-65.
7437
10.
3449
9718
.95
0.41
19.0
70.
4824
5223
7.57
30c
lm04
35m
1828
077
.563
86-6
5.66
690
0.34
5305
19.0
80.
3119
.20
0.39
2450
840.
7622
clm
0425
l106
5675
.558
37-6
5.77
181
0.34
5737
19.2
90.
4619
.39
0.55
2450
383.
7849
clm
0436
n100
2476
.585
57-6
6.12
169
0.34
6597
19.4
70.
3819
.65
0.44
2451
556.
6837
clm
0300
l889
075
.818
90-6
6.45
933
0.34
8701
18.8
90.
5218
.99
0.56
2452
345.
5449
clm
0310
l124
4077
.326
74-6
6.48
791
0.34
8783
19.2
40.
3919
.36
0.45
2451
997.
5510
clm
0436
n142
8576
.663
42-6
6.15
315
0.34
9850
19.2
90.
3419
.47
0.45
2452
018.
5169
clm
0302
k378
275
.738
02-6
6.63
133
0.35
2431
19.2
70.
3219
.46
0.36
2451
117.
6421
clm
0434
l201
6876
.335
03-6
5.85
612
0.35
3452
19.4
70.
3919
.66
0.43
2451
575.
6684
clm
0293
k307
6474
.953
75-6
6.77
676
0.35
3740
19.3
60.
3119
.52
0.40
2451
424.
8113
dlm
0291
l971
674
.901
31-6
6.45
757
0.35
4199
19.7
30.
3919
.94
0.44
2451
190.
6306
clm
0435
m13
533
77.3
3903
-65.
6372
40.
3542
7419
.01
0.35
19.1
50.
4324
5150
4.64
54c
lm04
44l8
138
77.7
6094
-65.
7585
50.
3549
2619
.04
0.35
19.1
80.
4224
5122
6.60
81d
lm03
01n1
3911
77.0
3367
-66.
4830
20.
3571
8819
.10
0.38
19.2
60.
4424
5175
0.92
05d
lm02
91l2
3359
74.6
0627
-66.
5434
70.
3580
9319
.22
0.36
19.4
00.
4224
5194
7.67
18c
lm04
27k1
0785
75.2
9491
-65.
9845
40.
3583
7019
.06
0.36
19.1
90.
4124
5224
2.79
08c
lm04
25m
3355
75.9
4157
-65.
5620
90.
3588
6419
.12
0.40
19.2
30.
4824
5146
2.66
46c
lm03
01l2
6933
76.3
9115
-66.
5790
50.
3605
8419
.06
0.32
19.2
60.
3824
5159
9.60
39d
lm04
22n1
6993
75.0
7383
-65.
4696
30.
3607
2619
.12
0.38
19.2
80.
4624
5146
9.63
48c
lm03
10l1
2653
77.4
2654
-66.
5918
80.
3621
0219
.17
0.35
19.3
20.
4824
5073
1.87
95d
lm02
93n1
4230
75.4
5233
-66.
8319
70.
3628
9718
.91
0.32
18.9
50.
3724
5179
1.73
70d
101
6.1. CLASSIFICATION OF EROS-2 CANDIDATE RR LYRAE STARSlm
0435
k847
977
.119
71-6
5.60
672
0.36
5160
19.0
10.
2919
.15
0.39
2451
886.
6258
dlm
0291
n259
2275
.170
50-6
6.55
760
0.36
5493
19.1
30.
3519
.30
0.43
2451
920.
6770
dlm
0293
m10
988
75.0
7649
-66.
6611
90.
3661
2119
.15
0.40
19.2
70.
4624
5249
6.80
02c
lm03
05m
6294
76.9
7324
-66.
9874
90.
3666
8318
.84
0.40
18.9
30.
5024
5148
2.64
07c
lm03
10k9
300
77.6
1115
-66.
3112
10.
3702
8819
.15
0.52
19.2
30.
5924
5198
2.57
26c
lm04
34m
2207
876
.476
51-6
5.70
050
0.37
2157
19.3
80.
4119
.58
0.50
2450
379.
8638
clm
0444
l927
077
.748
04-6
5.76
665
0.37
4023
19.0
30.
3119
.13
0.34
2451
997.
5565
clm
0425
m81
4475
.798
79-6
5.59
725
0.37
6376
19.0
60.
4019
.17
0.50
2451
653.
5187
clm
0300
n249
0476
.123
96-6
6.56
460
0.37
6841
18.9
90.
3819
.16
0.44
2451
388.
9318
clm
0434
l198
1076
.385
78-6
5.88
519
0.37
9506
18.7
50.
3718
.85
0.43
2451
768.
8205
clm
0427
l173
4675
.487
75-6
6.18
771
0.38
0922
19.3
10.
4619
.42
0.53
2451
966.
5759
clm
0436
m11
977
76.6
5728
-65.
9963
70.
3821
0319
.24
0.37
19.4
30.
4124
5146
0.66
05c
lm04
25k8
207
75.3
9793
-65.
6024
90.
3821
1118
.80
0.40
18.9
40.
4724
5218
3.68
22c
lm03
03m
2339
176
.805
10-6
6.73
721
0.38
5510
19.2
50.
4019
.39
0.45
2451
173.
6461
dlm
0427
l450
775
.530
04-6
6.08
408
0.38
7359
18.6
60.
3118
.74
0.36
2451
659.
4931
clm
0303
k243
6376
.731
34-6
6.74
087
0.39
1884
18.8
10.
4218
.91
0.46
2451
872.
6528
dlm
0424
m22
887
75.1
3167
-65.
7016
40.
3981
2519
.49
1.09
19.6
01.
3124
5118
3.64
80ab
lm03
02k5
022
75.7
5683
-66.
6424
90.
4042
0219
.28
0.41
19.4
10.
4724
5186
0.58
16c
lm03
02l1
2678
75.8
5530
-66.
8375
00.
4249
4519
.09
1.03
19.1
71.
1924
5043
2.75
73ab
lm03
03m
2298
977
.032
43-6
6.73
305
0.42
7324
18.5
30.
3718
.53
0.42
2451
253.
5588
clm
0436
n111
7276
.754
15-6
6.12
991
0.43
1733
19.3
41.
2619
.46
1.51
2451
618.
5691
ablm
0300
l146
4775
.546
89-6
6.59
292
0.43
3620
19.3
80.
4819
.48
0.60
2451
383.
8448
clm
0293
n310
8075
.156
16-6
6.93
208
0.43
6530
19.2
20.
5019
.24
0.57
2451
090.
6690
clm
0434
l791
276
.438
11-6
5.76
134
0.45
5709
19.5
30.
3819
.68
0.56
2451
581.
6628
clm
0312
k211
1177
.393
36-6
6.76
995
0.46
0600
19.1
81.
0919
.36
1.33
2451
595.
7083
ablm
0293
k392
874
.849
21-6
6.62
125
0.47
1742
19.2
90.
9119
.41
1.06
2451
629.
5964
ablm
0293
n307
9575
.454
01-6
6.92
786
0.47
4027
18.9
80.
7419
.07
0.92
2451
828.
6830
ablm
0432
l124
2076
.186
33-6
5.53
826
0.47
8439
19.4
60.
6819
.63
0.87
2452
021.
5603
ablm
0427
n774
175
.788
08-6
6.11
239
0.48
2840
19.0
21.
1419
.13
1.36
2451
393.
8494
ablm
0300
m99
3576
.002
53-6
6.31
022
0.48
5127
19.2
11.
0519
.33
1.26
2451
300.
5041
ablm
0437
k157
7277
.001
70-6
6.01
396
0.48
8322
19.2
21.
1319
.36
1.30
2451
620.
5741
ablm
0434
l204
35a
76.3
3615
-65.
8581
10.
4888
1019
.11
1.06
19.2
71.
3324
5047
6.72
360
ablm
0437
k226
5477
.012
47-6
6.06
322
0.49
1312
19.2
10.
8719
.36
1.07
2451
349.
9377
ab
102
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3lm
0436
n206
2876
.770
19-6
6.20
120
0.49
3107
19.1
01.
0819
.20
1.28
2452
191.
6897
ablm
0302
n235
2376
.210
95-6
6.89
987
0.49
7153
18.9
90.
8819
.06
1.17
2452
388.
4745
ablm
0293
k283
5274
.723
41-6
6.76
451
0.49
7779
19.1
11.
1419
.25
1.33
2451
875.
5967
ablm
0303
n139
77a
76.9
3426
-66.
8301
20.
4995
5619
.20
1.07
19.3
21.
2424
5175
6.86
03ab
lm03
03n1
5322
76.8
2352
-66.
8388
20.
5057
3318
.97
0.97
19.0
51.
1324
5124
6.61
59ab
lm02
93m
1437
575
.199
99-6
6.68
054
0.50
7995
18.7
60.
8618
.83
1.02
2451
653.
5100
ablm
0301
l242
5576
.597
98-6
6.55
346
0.51
0580
19.0
50.
8719
.25
1.03
2451
203.
5589
ablm
0436
l204
5076
.404
91-6
6.20
527
0.51
1395
19.0
20.
9219
.13
1.12
2451
966.
6073
ablm
0437
m20
444
77.7
0208
-66.
0452
10.
5114
2319
.38
0.77
19.5
31.
0024
5187
0.61
93ab
lm03
02l2
3297
75.8
7528
-66.
9081
10.
5114
7319
.21
1.04
19.3
61.
2324
5157
9.66
40ab
lm02
91m
8710
75.2
9738
-66.
2954
20.
5117
4519
.52
0.98
19.6
81.
1024
5077
6.73
63ab
lm04
35k2
0062
77.0
8979
-65.
6861
60.
5141
2519
.25
0.95
19.4
01.
0824
5155
6.68
37ab
lm02
91n2
0101
75.4
1745
-66.
5200
10.
5172
5419
.17
1.13
19.3
91.
4424
5157
7.63
93ab
lm03
00m
1717
876
.020
68-6
6.35
996
0.51
8967
19.3
50.
9119
.56
1.11
2451
960.
6609
ablm
0302
m22
487
76.3
0911
-66.
7632
90.
5205
6219
.73
0.99
19.9
31.
4124
5221
9.58
92ab
lm03
03m
1715
276
.983
50-6
6.69
861
0.52
4201
18.8
70.
7318
.92
0.85
2451
353.
9049
ablm
0300
k121
8475
.780
71-6
6.32
998
0.52
4813
19.0
40.
6919
.18
0.95
2451
918.
6675
ablm
0303
k252
1076
.702
20-6
6.74
596
0.52
4918
19.3
90.
6219
.54
0.77
2451
563.
6306
ablm
0435
m17
793
77.4
4960
-65.
6647
20.
5249
5619
.04
0.94
19.1
91.
1324
5193
4.67
02ab
lm04
35m
2356
377
.512
67-6
5.70
218
0.52
5048
19.0
40.
7019
.14
0.82
2451
868.
6062
ablm
0425
n232
5076
.043
45-6
5.87
922
0.52
5191
19.3
30.
9419
.43
0.99
2452
214.
8489
ablm
0300
m19
324
76.2
7787
-66.
4292
70.
5253
1219
.15
0.88
19.2
31.
0324
5123
3.71
63ab
lm03
00l1
3312
75.7
6052
-66.
5944
60.
5274
5218
.85
0.90
18.9
91.
0124
5183
3.72
64ab
lm02
91n6
040
75.2
0907
-66.
4317
50.
5276
1919
.27
1.03
19.3
91.
2124
5188
8.59
97ab
lm03
01n1
6814
77.1
1029
-66.
5006
50.
5282
6219
.05
0.80
19.1
90.
9924
5158
9.65
12ab
lm04
26n1
2018
75.0
9864
-66.
1325
90.
5294
6019
.63
1.16
19.8
71.
4024
5180
4.76
60ab
lm02
91n2
0061
75.0
6329
-66.
5227
20.
5297
5619
.51
0.92
19.6
91.
1024
5197
3.57
02ab
lm03
01n2
1605
76.8
7595
-66.
5331
90.
5325
4519
.26
1.05
19.4
31.
2024
5117
5.69
07ab
lm03
01m
2278
077
.190
99-6
6.38
563
0.53
5459
18.9
51.
1019
.16
1.33
2451
459.
7352
ablm
0301
k175
5476
.377
39-6
6.36
031
0.53
5567
19.4
50.
9419
.64
1.08
2451
573.
6131
ablm
0425
l148
5275
.332
57-6
5.80
227
0.53
6054
19.3
71.
1819
.53
1.36
2451
892.
8354
ablm
0437
m17
477
77.5
9584
-66.
0738
20.
5361
3419
.47
0.73
19.5
50.
9324
5220
0.66
93ab
lm03
10k1
1253
77.2
5582
-66.
3252
30.
5371
4919
.04
0.84
19.1
61.
0024
5119
1.68
07ab
103
6.1. CLASSIFICATION OF EROS-2 CANDIDATE RR LYRAE STARSlm
0434
k220
9576
.397
10-6
5.73
215
0.53
9682
19.1
10.
8719
.30
1.06
2450
736.
7900
ablm
0425
k115
0075
.330
82-6
5.62
627
0.54
0233
18.7
20.
4718
.84
0.65
2450
880.
5798
ablm
0434
m61
3976
.658
53-6
5.58
909
0.54
0358
19.1
41.
0719
.27
1.25
2451
602.
5686
ablm
0301
m15
584
76.9
6520
-66.
3405
60.
5413
4019
.43
1.09
19.6
01.
3424
5150
2.62
55ab
lm04
46k2
0706
77.7
4377
-66.
0537
20.
5435
6919
.36
0.55
19.5
60.
8224
5158
9.67
90ab
lm04
27m
1475
375
.893
61-6
6.00
800
0.54
4010
18.8
70.
7418
.99
0.90
2451
573.
6030
ablm
0437
n147
9477
.716
65-6
6.16
543
0.54
4769
19.2
40.
9919
.33
1.04
2450
806.
8093
ablm
0300
m23
701
75.9
6552
-66.
4039
20.
5461
0219
.00
0.75
19.1
60.
8724
5229
7.67
31ab
lm04
25m
1262
475
.717
20-6
5.62
945
0.54
7065
18.8
90.
8019
.00
1.00
2451
587.
6229
ablm
0300
m23
266
76.3
2789
-66.
3997
30.
5488
6818
.92
0.55
19.0
20.
6824
5086
4.71
09ab
lm03
01n1
4847
76.9
3447
-66.
4895
80.
5495
3519
.21
0.60
19.3
80.
8624
5194
5.68
03ab
lm04
35m
9334
77.3
7913
-65.
6089
60.
5508
5018
.87
0.67
19.0
40.
8024
5185
4.61
76ab
lm04
23l1
1740
75.4
0143
-65.
5192
50.
5543
3719
.15
0.49
19.2
90.
6124
5191
2.69
47ab
lm02
91k1
0561
74.7
7965
-66.
3105
80.
5571
0018
.96
0.82
19.1
60.
9824
5203
8.49
30ab
lm02
91m
1193
375
.417
18-6
6.31
573
0.55
8102
18.9
60.
5819
.09
0.69
2452
190.
6718
ablm
0423
n262
2475
.759
80-6
5.52
229
0.55
9366
19.4
00.
8219
.55
0.98
2452
210.
7725
ablm
0302
k147
9675
.622
13-6
6.74
150
0.55
9635
19.2
30.
7819
.40
0.90
2451
997.
5382
ablm
0300
m11
839
75.9
2208
-66.
3239
20.
5597
3319
.10
0.93
19.2
61.
1524
5131
7.48
64ab
lm03
03l1
7671
76.7
3167
-66.
8534
40.
5605
8818
.95
0.87
19.0
81.
0324
5082
0.60
03ab
lm04
23l7
926
75.5
4610
-65.
5305
60.
5618
1819
.28
0.89
19.4
31.
0424
5181
3.75
76ab
lm04
27l1
8856
75.6
4163
-66.
1973
40.
5626
9819
.17
0.78
19.3
80.
9724
5162
5.53
32ab
lm03
03m
1781
277
.067
91-6
6.70
197
0.56
5556
19.2
00.
8919
.28
1.08
2450
398.
7132
ablm
0302
n123
5175
.940
97-6
6.83
188
0.56
6134
19.6
30.
5819
.80
0.82
2452
516.
7872
ablm
0300
k143
3575
.659
71-6
6.34
538
0.56
6157
19.0
20.
7319
.18
0.91
2451
870.
6089
ablm
0300
n272
8675
.944
49-6
6.58
057
0.56
6301
18.9
20.
9119
.07
1.08
2451
623.
5582
ablm
0302
l129
6075
.732
62-6
6.83
949
0.56
7341
18.9
80.
7519
.14
0.77
2452
223.
8058
ablm
0300
n210
9176
.329
09-6
6.53
946
0.56
7460
19.3
91.
0119
.57
1.23
2451
253.
5588
ablm
0434
k900
876
.391
64-6
5.61
437
0.56
7635
18.9
20.
9219
.08
1.08
2451
927.
6789
ablm
0301
l116
3076
.570
24-6
6.47
409
0.56
8156
19.1
20.
8219
.29
1.01
2451
791.
7477
ablm
0300
k176
6575
.748
62-6
6.36
812
0.56
8997
18.8
60.
5519
.07
0.69
2452
232.
8191
ablm
0291
l107
7574
.692
80-6
6.46
539
0.57
0992
19.8
70.
4320
.17
0.49
2451
623.
5424
ablm
0300
m11
600
76.1
4728
-66.
3216
60.
5709
9518
.69
0.58
18.7
70.
6824
5218
5.64
85ab
lm04
37n1
5049
77.4
9507
-66.
1695
10.
5710
1419
.24
0.77
19.4
20.
8924
5144
0.84
55ab
104
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3lm
0434
n137
0476
.726
55-6
5.79
908
0.57
1166
19.4
00.
8219
.57
1.03
2451
745.
8545
ablm
0427
l124
6275
.381
09-6
6.15
291
0.57
1194
19.1
00.
6419
.28
0.84
2451
961.
7336
ablm
0435
l524
776
.922
13-6
5.73
542
0.57
1823
18.9
50.
6019
.12
0.77
2452
227.
6073
ablm
0434
m21
424
76.7
5130
-65.
6951
90.
5738
2019
.36
0.40
19.5
70.
5124
5194
3.73
60ab
lm04
37n8
455
77.7
3625
-66.
1133
30.
5749
9919
.10
0.90
19.2
31.
0024
5076
3.79
60ab
lm04
44l2
0033
77.7
6182
-65.
8942
70.
5750
9218
.57
0.26
18.6
20.
3024
5149
0.69
19ab
lm02
93n2
0870
75.3
6086
-66.
8714
70.
5781
9018
.52
0.73
18.6
80.
8624
5183
0.70
52ab
lm04
37m
2088
377
.607
90-6
6.04
953
0.58
0287
19.3
30.
7219
.52
0.87
2451
821.
7638
ablm
0293
m19
628
75.2
9061
-66.
7109
90.
5811
4119
.06
0.73
19.2
00.
8724
5158
9.62
91ab
lm03
03n1
2799
76.9
1560
-66.
8231
00.
5818
4819
.06
0.64
19.2
10.
7424
5219
9.80
86ab
lm04
34l1
7031
76.3
4705
-65.
8327
10.
5829
3719
.29
0.68
19.5
30.
8024
5202
8.50
12ab
lm02
93m
1900
375
.261
69-6
6.70
727
0.58
3546
19.2
80.
6819
.44
0.85
2450
820.
6936
ablm
0437
k153
2876
.981
54-6
6.01
065
0.58
4568
19.2
80.
7619
.53
0.99
2451
870.
8183
ablm
0291
k100
4774
.824
01-6
6.30
667
0.58
5024
19.4
30.
7919
.66
0.92
2451
894.
5925
ablm
0293
k252
2674
.876
83-6
6.74
562
0.58
6479
19.1
30.
7919
.31
0.95
2451
976.
5671
ablm
0303
n273
0277
.211
28-6
6.90
501
0.58
6637
19.2
40.
5719
.34
0.68
2452
471.
9041
ablm
0435
n113
2177
.350
12-6
5.77
656
0.58
7183
18.8
90.
4919
.18
0.61
2451
530.
6598
ablm
0437
k868
176
.964
96-6
5.96
417
0.58
9055
19.0
40.
4719
.21
0.63
2450
440.
8116
ablm
0300
l207
3975
.685
50-6
6.54
657
0.58
9066
18.9
10.
7319
.13
0.86
2451
478.
6339
ablm
0310
l181
4777
.452
44-6
6.53
289
0.59
0217
18.7
50.
5618
.91
0.64
2451
623.
5755
ablm
0302
l264
1775
.704
71-6
6.93
057
0.59
0296
19.3
40.
6919
.54
0.89
2451
953.
6490
ablm
0310
k180
1077
.556
57-6
6.40
282
0.59
0299
19.2
70.
8819
.42
0.97
2452
316.
6514
ablm
0300
k165
6375
.877
14-6
6.36
044
0.59
2704
19.1
80.
6519
.38
0.78
2451
120.
6248
ablm
0303
m21
245
77.0
1340
-66.
7231
10.
5935
5118
.85
0.64
18.9
30.
7424
5230
5.65
37ab
lm04
37k1
3906
77.3
0504
-65.
9985
10.
5943
3219
.15
0.63
19.3
20.
7124
5188
5.63
14ab
lm02
93m
1700
075
.185
43-6
6.69
597
0.59
5224
19.1
10.
7019
.27
0.84
2452
231.
7729
ablm
0435
m70
5877
.570
13-6
5.59
222
0.59
7486
19.0
30.
4519
.19
0.53
2450
404.
7845
ablm
0425
m42
8875
.858
96-6
5.56
967
0.59
7504
19.0
40.
5719
.17
0.71
2451
929.
6322
ablm
0435
n139
1377
.440
01-6
5.79
393
0.59
7578
19.3
30.
4519
.54
0.59
2451
746.
6642
ablm
0426
m24
414
74.8
5054
-66.
0706
40.
6068
6919
.21
0.55
19.4
00.
6024
5193
8.64
25ab
lm04
25l1
0247
75.2
6573
-65.
7706
80.
6074
6118
.92
0.85
19.0
71.
0724
5158
7.62
29ab
lm03
10k1
5738
77.4
2775
-66.
4095
80.
6085
3419
.16
0.42
19.3
70.
5324
5220
1.79
70ab
lm04
35k1
2309
77.1
0144
-65.
6330
70.
6089
9219
.15
0.70
19.3
50.
8224
5150
2.63
58ab
105
6.1. CLASSIFICATION OF EROS-2 CANDIDATE RR LYRAE STARSlm
0435
l985
876
.918
47-6
5.76
707
0.60
9462
19.1
50.
5819
.34
0.70
2451
890.
6303
ablm
0434
k730
276
.147
62-6
5.60
166
0.61
0192
19.3
00.
5919
.53
0.69
2451
994.
5443
ablm
0293
l126
3174
.806
25-6
6.82
752
0.61
0866
19.2
40.
6019
.46
0.74
2452
177.
6975
ablm
0435
k175
8977
.227
23-6
5.66
834
0.61
2635
19.2
80.
5719
.46
0.65
2451
861.
6691
ablm
0293
l525
274
.964
58-6
6.78
360
0.61
2908
19.2
30.
6019
.43
0.73
2451
220.
6303
ablm
0312
k450
377
.380
73-6
6.62
996
0.61
3847
19.4
90.
5019
.79
0.74
2450
430.
6813
ablm
0436
k158
5576
.164
15-6
6.02
233
0.61
4185
18.9
80.
4319
.17
0.49
2451
764.
8463
ablm
0425
l210
4875
.439
03-6
5.84
525
0.61
5813
18.8
00.
7918
.99
0.94
2451
861.
6474
ablm
0427
m20
466
75.9
9099
-66.
0483
40.
6166
2619
.63
0.82
19.8
21.
0724
5157
7.64
81ab
lm04
35k1
2002
76.9
6857
-65.
6316
70.
6187
7419
.37
0.74
19.5
90.
8724
5220
2.65
19ab
lm04
24n5
227
75.1
1837
-65.
7359
10.
6199
8318
.58
0.65
18.7
40.
8524
5090
7.53
66ab
lm04
37m
9713
77.5
3209
-65.
9678
20.
6200
1118
.93
0.75
19.0
70.
9324
5183
0.74
54ab
lm03
03l2
6148
76.4
5407
-66.
9038
70.
6206
4718
.83
0.45
18.9
70.
5024
5224
0.56
97ab
lm03
02k1
3534
75.9
0035
-66.
7316
60.
6208
8019
.03
0.64
19.2
00.
7624
5222
9.59
83ab
lm03
05k5
704
76.5
3880
-66.
9874
80.
6216
0019
.26
0.45
19.4
90.
5024
5148
2.64
07ab
lm04
37l1
5735
77.0
6524
-66.
1793
40.
6225
5319
.29
0.42
19.5
10.
5124
5050
3.65
41ab
lm04
34m
1964
876
.560
45-6
5.68
376
0.62
2604
19.0
90.
5619
.30
0.66
2451
183.
6623
ablm
0300
n139
6176
.238
93-6
6.49
314
0.62
3548
18.9
11.
1419
.04
1.35
2452
297.
6731
ablm
0303
l276
1076
.593
94-6
6.91
158
0.62
3747
18.9
60.
4419
.13
0.53
2452
257.
6065
ablm
0292
n226
1274
.510
12-6
6.89
940
0.62
4068
19.1
00.
3919
.24
0.49
2452
206.
5991
ablm
0293
n182
2975
.168
69-6
6.85
795
0.62
8127
19.0
10.
3919
.16
0.46
2452
231.
7729
ablm
0303
n974
577
.018
68-6
6.80
425
0.62
8757
19.2
10.
3419
.35
0.44
2451
266.
5201
ablm
0435
m18
273
77.6
6155
-65.
6659
20.
6314
7618
.98
0.39
19.1
50.
4824
5157
1.63
85ab
lm04
23l2
1178
75.5
9644
-65.
4893
70.
6321
2518
.95
0.47
19.1
40.
5324
5268
4.69
00ab
lm03
03n1
6102
76.8
8992
-66.
8429
60.
6324
2818
.85
0.89
18.9
61.
0424
5230
1.65
23ab
lm04
24n1
2543
74.9
0326
-65.
7908
30.
6353
1618
.99
0.89
19.1
61.
0724
5225
9.58
69ab
lm03
00n1
9927
76.2
4113
-66.
5324
20.
6371
2919
.16
0.32
19.3
30.
3724
5193
9.74
43ab
lm03
00l2
5566
75.6
7367
-66.
5796
90.
6381
5518
.98
0.46
19.1
80.
5224
5053
2.57
16ab
lm04
35k1
5816
76.9
2775
-65.
6577
40.
6387
9418
.86
0.68
19.0
50.
8424
5194
3.73
60ab
lm03
00k1
1860
75.5
1738
-66.
3279
60.
6437
5719
.05
0.53
19.1
70.
6724
5125
9.55
91ab
lm03
03m
1100
577
.149
24-6
6.65
987
0.64
3770
19.1
21.
0619
.15
1.23
2451
177.
8395
ablm
0301
n149
4376
.882
53-6
6.49
069
0.64
5196
19.1
00.
3119
.32
0.37
2451
233.
7163
ablm
0436
m17
011
76.5
6619
-66.
0376
50.
6459
9619
.13
0.72
19.3
50.
8824
5205
1.48
10ab
106
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3lm
0301
l227
8676
.443
74-6
6.54
541
0.64
8027
19.0
20.
6019
.24
0.69
2451
815.
7624
ablm
0436
n823
676
.820
37-6
6.10
734
0.65
0192
18.7
30.
8418
.88
1.03
2451
447.
7726
ablm
0300
m25
109
76.2
5662
-66.
4128
80.
6528
9119
.05
0.94
19.0
91.
0724
5043
0.57
53ab
lm03
10l1
6334
77.4
3882
-66.
5174
90.
6577
8818
.99
0.25
19.2
60.
3024
5044
5.76
95ab
lm02
93l2
5506
74.8
2889
-66.
9017
00.
6579
8218
.98
0.82
19.1
70.
9624
5217
2.72
36ab
lm03
10l1
4484
77.3
2418
-66.
5028
00.
6616
5218
.74
0.62
19.0
10.
7324
5193
9.75
06ab
lm03
01l2
5140
a76
.511
23-6
6.55
949
0.66
3184
18.5
70.
7018
.70
0.82
2451
296.
5118
ablm
0291
l265
45a
74.6
6819
-66.
5626
30.
6694
8819
.06
0.94
19.3
21.
1324
5162
3.54
24ab
lm04
34n8
413
76.7
4585
-65.
7618
20.
6708
7118
.94
0.64
19.0
90.
7724
5218
3.71
35ab
lm03
00n1
2088
76.1
6779
-66.
4811
10.
6723
5619
.30
0.65
19.5
00.
7924
5232
6.57
40ab
lm04
27k1
7452
75.3
5321
-66.
0749
40.
6754
9819
.13
0.43
19.3
20.
4924
5153
8.57
61ab
lm03
00n1
2109
76.1
1925
-66.
4814
00.
6834
5918
.88
0.60
19.0
40.
6924
5195
1.65
17ab
lm04
26n9
666
75.1
7663
-66.
1149
70.
6876
2519
.09
0.42
19.2
80.
4624
5203
0.49
39ab
lm04
34n2
2292
76.4
8691
-65.
8596
00.
6896
9319
.21
0.34
19.3
90.
4424
5203
2.49
50ab
lm03
03m
5651
77.1
3918
-66.
6270
50.
6925
4719
.04
0.52
19.1
40.
6424
5187
0.60
89ab
lm03
01m
1578
877
.019
23-6
6.34
154
0.71
0038
18.7
00.
3418
.85
0.38
2451
866.
6022
ablm
0305
m38
8276
.858
77-6
6.97
363
0.71
0488
19.0
30.
6519
.19
0.75
2451
533.
6272
ablm
0305
m78
5077
.223
90-6
6.99
474
0.71
3324
18.7
60.
2718
.88
0.32
2451
502.
6255
ablm
0427
m63
3875
.990
25-6
5.94
538
0.71
3501
19.1
60.
6319
.28
0.71
2452
395.
4980
ablm
0434
n173
8376
.513
44-6
5.89
259
0.72
4152
18.8
30.
3119
.04
0.39
2452
254.
5884
ablm
0301
l164
8776
.556
35-6
6.50
519
0.73
8143
18.9
80.
1819
.24
0.22
2452
008.
5249
ablm
0300
l234
6275
.602
95-6
6.58
330
0.74
4314
18.7
60.
5518
.97
0.64
2451
886.
6168
ablm
0310
l189
1177
.523
38-6
6.53
928
0.74
8431
19.0
40.
3819
.29
0.45
2452
213.
7774
abTa
ble
6.2:
Prop
ertie
sof
the
251
confi
rmed
RR
Lyra
est
ars
intil
eLM
C8_
3(C
olum
n1:
ERO
S-2
iden
tifica
tion
ofth
est
ar;C
olum
n2:
Rig
htas
-ce
nsio
nfr
omth
eER
OS-
2ca
talo
gue;
Col
umn
3:D
eclin
atio
nfr
omth
eER
OS-
2ca
talo
gue;
Col
umn
4:Pe
riod
from
the
ERO
S-2
cata
logu
e(a
-St
ars
for
whi
cha
new
perio
dw
ases
timat
edin
this
stud
y);
Col
umn
5:M
ean
mag
nitu
dein
theB
EROS
band
;C
olum
n6:
Am
plitu
dein
the
BEROS
band
;C
olum
n7:
Mea
nm
agni
tude
inth
eV
band
;C
olum
n8:
Am
plitu
dein
theV
band
;Col
umn
9:Ep
och
ofm
axim
umlig
htin
theV
band
;Col
umn
10:C
lass
ifica
tion
inty
pe).
107
6.2. COMPARISON WITH THE OGLE III CATALOGUE
6.2 Comparison with the OGLE III catalogue
We compared our classification of the RR Lyrae stars in tile LMC 8_3 with the classifica-
tion provided in the OGLE III catalogue. The OGLE III survey covered only part of the
tile LMC 8_3. We were able to make a comparison for 72 RR Lyrae stars which are in
common between the two catalogues. Information about these 72 objects is presented in
Table 6.3. For the majority of the RR Lyrae stars our classification is in agreement with the
classification provided by OGLE III, but there are some discrepancies.
According to the OGLE III classification the source lm0305m3332 is an RRab star, but
we classified it as RRc star. Also the period of this star, determined by the EROS-2 survey
(P=0.249311 day), differs from the period provided by the OGLE III survey (P=0.4986339
day). After analysis of the light curve with GRATIS we concluded that OGLE III provided
an alias of the actual period. Star lm0293l18421 was classified as RRc by us and as RRe by
the OGLE III. Star lm0300l14647 is an RRd star according to the OGLE III classification,
but we analysed the light curve with GRATIS and did not confirm the existence of a second
periodicity, therefore, we classified the star as c-type RR Lyrae. Star lm0293n31080 is
RRab in the OGLE III classification and RRc in our classification.
108
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3
OG
LEII
Iid
ERO
S-2
idR
AD
ECTy
peI
VP
Epoc
h(m
ax)
(HH
:MM
:SS)
(DD
:MM
:SS)
(mag
)(m
ag)
(day
)(H
JD-2
4500
00)
OG
LE-L
MC
-RR
LYR
-024
65lm
0292
n226
124:
58:0
2.47
-66:
53:5
8.2
RR
ab18
.836
19.4
110.
6240
672
2166
.648
31O
GLE
-LM
C-R
RLY
R-0
2630
lm02
93k2
8352
4:58
:53.
66-6
6:45
:52.
4R
Rab
18.7
5219
.215
0.49
7780
021
66.8
0015
OG
LE-L
MC
-RR
LYR
-027
40lm
0293
l184
214:
59:1
0.51
-66:
51:3
9.0
RR
e18
.778
19.1
430.
2787
614
2166
.797
15O
GLE
-LM
C-R
RLY
R-0
2767
lm02
93l1
2631
4:59
:13.
54-6
6:49
:39.
4R
Rab
18.7
5019
.396
0.61
0866
021
66.7
2786
OG
LE-L
MC
-RR
LYR
-027
95lm
0293
l255
064:
59:1
8.97
-66:
54:0
6.6
RR
ab18
.582
19.1
810.
6579
816
2166
.798
64O
GLE
-LM
C-R
RLY
R-0
2814
lm02
93k3
928
4:59
:23.
82-6
6:37
:16.
8R
Rab
18.8
1119
.292
0.47
1742
321
72.5
6258
OG
LE-L
MC
-RR
LYR
-028
41lm
0293
k252
264:
59:3
0.49
-66:
44:4
4.4
RR
ab18
.707
19.2
900.
5864
819
2166
.593
34O
GLE
-LM
C-R
RLY
R-0
2913
lm02
93k3
0764
4:59
:48.
97-6
6:46
:36.
5R
Rd
19.1
2319
.625
0.35
3743
821
66.5
8727
OG
LE-L
MC
-RR
LYR
-029
28lm
0293
l525
24:
59:5
1.57
-66:
47:0
1.2
RR
ab18
.826
19.4
490.
6129
133
2166
.368
64O
GLE
-LM
C-R
RLY
R-0
3045
lm02
93m
1098
85:
00:1
8.38
-66:
39:4
0.5
RR
c18
.852
19.3
550.
3661
132
2166
.545
33O
GLE
-LM
C-R
RLY
R-0
3129
lm02
93n3
1080
5:00
:37.
50-6
6:55
:55.
6R
Rab
19.1
8419
.610
0.43
6512
321
66.7
3257
OG
LE-L
MC
-RR
LYR
-031
44lm
0293
n182
295:
00:4
0.54
-66:
51:2
8.8
RR
ab18
.718
19.3
220.
6281
261
2166
.469
07O
GLE
-LM
C-R
RLY
R-0
3159
lm02
93m
1700
05:
00:4
4.55
-66:
41:4
5.6
RR
ab18
.754
19.3
420.
5952
245
2166
.303
04O
GLE
-LM
C-R
RLY
R-0
3174
lm02
93m
1437
55:
00:4
8.01
-66:
40:5
0.0
RR
ab18
.712
19.2
120.
5079
962
2166
.587
39O
GLE
-LM
C-R
RLY
R-0
3227
lm02
93m
1900
35:
01:0
2.85
-66:
42:2
6.3
RR
ab18
.853
19.4
490.
5835
871
2166
.304
63O
GLE
-LM
C-R
RLY
R-0
3255
lm02
93m
1962
85:
01:0
9.79
-66:
42:3
9.7
RR
ab18
.681
19.2
440.
5811
319
2166
.723
46O
GLE
-LM
C-R
RLY
R-0
3330
lm02
93n2
0870
5:01
:26.
59-6
6:52
:17.
4R
Rab
18.5
7319
.099
0.57
8191
421
66.6
3326
OG
LE-L
MC
-RR
LYR
-033
82lm
0293
m19
803
5:01
:38.
65-6
6:42
:39.
2R
Rc
18.9
3819
.371
0.33
8544
921
66.7
3510
OG
LE-L
MC
-RR
LYR
-034
23lm
0293
n142
305:
01:4
8.55
-66:
49:5
4.7
RR
d18
.774
19.2
280.
3629
116
2166
.607
85O
GLE
-LM
C-R
RLY
R-0
3425
lm02
93n3
0795
5:01
:48.
98-6
6:55
:40.
0R
Rab
18.8
2119
.338
0.47
4009
821
66.6
9079
OG
LE-L
MC
-RR
LYR
-035
24lm
0300
l146
475:
02:1
1.22
-66:
35:3
4.9
RR
d18
.543
19.0
470.
4336
058
2166
.577
04O
GLE
-LM
C-R
RLY
R-0
3580
lm03
00l2
3462
5:02
:24.
69-6
6:35
:00.
3R
Rab
18.4
1218
.995
0.74
4310
121
66.4
9600
OG
LE-L
MC
-RR
LYR
-036
02lm
0302
k147
965:
02:2
9.31
-66:
44:2
9.6
RR
ab18
.831
19.4
100.
5596
368
2166
.543
48O
GLE
-LM
C-R
RLY
R-0
3637
lm03
02l1
6395
5:02
:38.
91-6
6:51
:46.
4R
Rc
18.8
3819
.278
0.34
4596
321
66.5
3368
OG
LE-L
MC
-RR
LYR
-036
54lm
0300
l255
665:
02:4
1.69
-66:
34:4
7.2
RR
ab18
.716
19.2
830.
6381
508
2172
.629
08O
GLE
-LM
C-R
RLY
R-0
3689
lm03
02l2
6417
5:02
:49.
15-6
6:55
:50.
3R
Rab
19.0
3619
.687
0.59
0301
821
66.7
5562
OG
LE-L
MC
-RR
LYR
-037
17lm
0302
l129
605:
02:5
5.86
-66:
50:2
2.4
RR
ab18
.646
19.1
960.
5673
193
2166
.529
92O
GLE
-LM
C-R
RLY
R-0
3722
lm03
02k3
782
5:02
:57.
11-6
6:37
:52.
8R
Rc
18.9
4119
.431
0.35
2435
321
66.8
2662
OG
LE-L
MC
-RR
LYR
-037
49lm
0302
k502
25:
03:0
1.62
-66:
38:3
3.1
RR
c18
.843
19.3
560.
4042
293
2166
.551
34O
GLE
-LM
C-R
RLY
R-0
3757
lm03
00l1
3312
5:03
:02.
53-6
6:35
:40.
6R
Rab
18.7
3019
.244
0.52
7450
621
66.5
5412
109
6.2. COMPARISON WITH THE OGLE III CATALOGUEO
GLE
-LM
C-R
RLY
R-0
3858
lm03
02l1
2678
5:03
:25.
28-6
6:50
:15.
2R
Rab
19.0
4019
.470
0.42
4944
821
66.5
2539
OG
LE-L
MC
-RR
LYR
-038
81lm
0302
l232
975:
03:3
0.11
-66:
54:2
9.5
RR
ab18
.909
19.4
910.
5114
616
2166
.332
40O
GLE
-LM
C-R
RLY
R-0
3902
lm03
02k1
3534
5:03
:36.
12-6
6:43
:54.
3R
Rab
18.6
2219
.256
0.62
0880
921
66.2
5905
OG
LE-L
MC
-RR
LYR
-039
56lm
0302
n123
515:
03:4
5.85
-66:
49:5
5.3
RR
ab19
.107
19.7
970.
5661
573
2166
.290
86O
GLE
-LM
C-R
RLY
R-0
3960
lm03
00n2
7286
5:03
:46.
69-6
6:34
:50.
3R
Rab
18.6
4919
.185
0.56
6303
321
66.6
4361
OG
LE-L
MC
-RR
LYR
-039
65lm
0304
m29
525:
03:4
7.34
-66:
58:1
8.9
RR
c18
.835
19.2
210.
3119
118
2166
.721
70O
GLE
-LM
C-R
RLY
R-0
4196
lm03
02n4
858
5:04
:33.
01-6
6:47
:04.
3R
Rc
18.8
5719
.200
0.29
2003
821
66.7
3196
OG
LE-L
MC
-RR
LYR
-042
99lm
0302
n235
235:
04:5
0.69
-66:
53:5
9.9
RR
ab18
.710
19.1
310.
4971
214
2166
.768
38O
GLE
-LM
C-R
RLY
R-0
4522
lm03
02m
2248
75:
05:1
4.23
-66:
45:4
8.0
RR
ab19
.106
19.6
420.
5204
521
2166
.599
96O
GLE
-LM
C-R
RLY
R-0
4643
lm03
01l2
6933
5:05
:33.
87-6
6:34
:44.
9R
Rd
18.7
02-9
9.99
00.
3605
884
2166
.804
71O
GLE
-LM
C-R
RLY
R-0
4736
lm03
03l2
6148
5:05
:49.
03-6
6:54
:14.
3R
Rab
18.6
4219
.235
0.62
0648
421
66.7
0892
OG
LE-L
MC
-RR
LYR
-048
53lm
0305
k570
45:
06:0
9.35
-66:
59:1
5.3
RR
ab18
.861
19.5
200.
6215
964
2166
.416
11O
GLE
-LM
C-R
RLY
R-0
4942
lm03
03l2
7610
5:06
:22.
59-6
6:54
:42.
0R
Rab
18.6
1019
.211
0.62
3747
921
66.5
6503
OG
LE-L
MC
-RR
LYR
-050
88lm
0303
l865
55:
06:4
6.46
-66:
48:0
2.7
RR
c18
.608
18.9
800.
3391
250
2166
.605
45O
GLE
-LM
C-R
RLY
R-0
5094
lm03
03k2
5210
5:06
:48.
56-6
6:44
:45.
7R
Rab
18.9
5419
.530
0.52
4921
021
66.7
6883
OG
LE-L
MC
-RR
LYR
-051
43lm
0303
k243
635:
06:5
5.56
-66:
44:2
7.3
RR
d18
.507
18.9
820.
3918
820
2166
.542
81O
GLE
-LM
C-R
RLY
R-0
5144
lm03
03l1
7671
5:06
:55.
64-6
6:51
:12.
7R
Rab
18.6
6319
.150
0.56
0584
921
66.5
6231
OG
LE-L
MC
-RR
LYR
-052
38lm
0303
m23
391
5:07
:13.
26-6
6:44
:14.
2R
Rd
18.8
7719
.533
0.38
5512
421
66.7
4170
OG
LE-L
MC
-RR
LYR
-052
63lm
0303
n153
225:
07:1
7.67
-66:
50:2
0.1
RR
ab18
.844
19.3
690.
5057
311
2166
.552
55O
GLE
-LM
C-R
RLY
R-0
5317
lm03
05m
3882
5:07
:26.
13-6
6:58
:25.
3R
Rab
18.6
2919
.242
0.71
0487
521
66.6
6993
OG
LE-L
MC
-RR
LYR
-053
60lm
0303
n161
025:
07:3
3.62
-66:
50:3
5.1
RR
ab18
.609
19.1
210.
6324
295
2166
.329
94O
GLE
-LM
C-R
RLY
R-0
5375
lm03
05m
3332
5:07
:35.
60-6
6:58
:11.
5R
Rab
19.1
7719
.677
0.49
8633
921
66.8
7261
OG
LE-L
MC
-RR
LYR
-054
05lm
0303
n127
995:
07:3
9.77
-66:
49:2
3.6
RR
ab18
.816
19.4
230.
5818
589
2166
.637
84O
GLE
-LM
C-R
RLY
R-0
5426
lm03
03n1
3977
5:07
:44.
26-6
6:49
:48.
9R
Rab
18.9
7819
.472
0.49
9565
521
66.5
0195
OG
LE-L
MC
-RR
LYR
-054
46lm
0303
m10
773
5:07
:47.
87-6
6:39
:37.
1R
Rc
18.7
4019
.213
0.34
4941
421
66.7
8490
OG
LE-L
MC
-RR
LYR
-054
76lm
0305
m62
945:
07:5
3.60
-66:
59:1
5.2
RR
c18
.650
19.0
950.
3666
785
2166
.876
90O
GLE
-LM
C-R
RLY
R-0
5490
lm03
03m
1715
25:
07:5
6.06
-66:
41:5
5.2
RR
ab18
.735
19.2
400.
5242
037
2166
.412
07O
GLE
-LM
C-R
RLY
R-0
5539
lm03
03m
2124
55:
08:0
3.26
-66:
43:2
3.3
RR
ab18
.659
19.2
370.
5935
504
2166
.768
82O
GLE
-LM
C-R
RLY
R-0
5551
lm03
03n9
745
5:08
:04.
51-6
6:48
:15.
8R
Rab
18.8
2419
.455
0.62
8778
721
66.3
2230
OG
LE-L
MC
-RR
LYR
-055
76lm
0303
m22
989
5:08
:07.
85-6
6:43
:59.
3R
Rc
18.4
3518
.937
0.42
7377
821
66.6
7659
OG
LE-L
MC
-RR
LYR
-056
17lm
0303
m17
812
5:08
:16.
34-6
6:42
:07.
3R
Rab
18.8
0319
.414
0.56
5554
521
66.6
4750
OG
LE-L
MC
-RR
LYR
-056
72lm
0303
n168
415:
08:2
4.70
-66:
50:4
4.4
RR
c19
.013
19.5
200.
3274
989
2166
.704
72O
GLE
-LM
C-R
RLY
R-0
5721
lm03
03m
5651
5:08
:33.
42-6
6:37
:37.
5R
Rab
18.7
0219
.331
0.69
2535
521
66.3
3100
110
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3O
GLE
-LM
C-R
RLY
R-0
5732
lm03
03m
1100
55:
08:3
5.84
-66:
39:3
5.7
RR
ab18
.641
19.2
520.
6437
728
2166
.677
16O
GLE
-LM
C-R
RLY
R-0
5734
lm03
03n3
1583
5:08
:36.
01-6
6:55
:50.
0R
Rc
18.9
7519
.395
0.31
4178
321
66.8
7421
OG
LE-L
MC
-RR
LYR
-057
40lm
0303
m22
504
5:08
:37.
25-6
6:43
:45.
2R
Rc
19.0
77-9
9.99
00.
3234
019
2223
.823
37O
GLE
-LM
C-R
RLY
R-0
5815
lm03
03n2
7302
5:08
:50.
73-6
6:54
:18.
2R
Rab
18.8
7819
.513
0.58
6639
921
66.8
5939
OG
LE-L
MC
-RR
LYR
-058
42lm
0305
m78
505:
08:5
3.76
-66:
59:4
1.2
RR
ab18
.620
19.2
860.
7133
254
2166
.735
15O
GLE
-LM
C-R
RLY
R-0
6089
lm03
12k4
503
5:09
:31.
40-6
6:37
:48.
1R
Rab
18.8
4119
.474
0.61
3850
321
66.6
6862
OG
LE-L
MC
-RR
LYR
-061
13lm
0312
k211
115:
09:3
4.39
-66:
46:1
2.1
RR
ab18
.920
19.3
550.
4605
988
2166
.859
45O
GLE
-LM
C-R
RLY
R-0
6171
lm03
12l1
5193
5:09
:42.
24-6
6:51
:26.
1R
Rc
19.0
4819
.534
0.33
1782
321
66.8
3342
OG
LE-L
MC
-RR
LYR
-061
73lm
0310
l126
535:
09:4
2.36
-66:
35:3
1.1
RR
d18
.935
19.4
240.
3621
078
2166
.559
86Ta
ble
6.3:
Prop
ertie
sof
RR
Lyra
est
ars
intil
eLM
C8_
3,w
hich
have
aco
unte
rpar
tin
the
OG
LEII
Ica
talo
gue
(Col
umn
1:O
GLE
III
iden
ti-fic
atio
nof
the
star
;C
olum
n2:
ERO
S-2
iden
tifica
tion
ofth
est
ar;
Col
-um
n3:
Rig
htas
cens
ion
from
the
OG
LEII
Icat
alog
ue;C
olum
n4:
Dec
-lin
atio
nfr
omth
eO
GLE
III
cata
logu
e;C
olum
n5:
Type
acco
rdin
gto
the
OG
LEII
Icl
assi
ficat
ion;
Col
umn
6:O
GLE
IIII
mea
nm
agni
tude
;C
olum
n7:
OG
LEII
IV
mea
nm
agni
tude
;Col
umn
8:Pe
riod
from
the
OG
LEII
Ica
talo
gue;
Col
umn
9:Ep
och
ofm
axim
umlig
htfr
omth
eO
GLE
IIIc
atal
ogue
).
111
6.3. FOURIER ANALYSIS OF THE RR LYRAE STARS IN TILE LMC 8_3
6.3 Fourier analysis of the RR Lyrae stars in tile LMC 8_3
The Fourier decomposition of the light curves was also used to check the classification of
the RR Lyrae stars in tile LMC 8_3 and to infer their metallicity (see Section 1.5.1). In order
to perform the Fourier analysis we first transformed the light curves in the EROS passbands
to the V -band using Eqs. 2.1 and 2.2, and then cleaned the V -band light curves of the 251
confirmed RR Lyrae stars from the possible outliers, according to the following iterative
procedure:
• we discarded all data-points with residuals > 0.200 mag from GRATIS best fit model
of the light curve;
• we checked the standard deviation σ of the distribution of residuals:
– if σ < 0.070 mag we stopped the cleaning procedure;
– if σ > 0.070 mag we discarded also data points with residual ∈ (0.150, 0.200)
mag from the best fit model.
• we again checked the standard deviation σ of the distribution of residuals:
– if σ < 0.070 mag we stopped the cleaning procedure;
– if σ > 0.070 mag we discarded also data points with residual ∈ (0.100, 0.150)
mag from the best fit model.
Note that all light curves still have more than 73 data points after this cleaning proce-
dure. We performed the sine Fourier decomposition of the light curves and derived normal-
ized Fourier parameters A21, A31, φ21, φ31 and the Dm values (see Section 1.5.1). Some of
these parameters are listed in Table 6.4.
Figure 6.2 shows the distribution of the 251 RR Lyrae stars in our sample on the A21
versus φ21 plane. The vast majority of the RR Lyrae stars are located in two well separated
regions which correspond to the RRab (upper-left region) and RRc (bottom-right region)
stars. Thus, the Fourier analysis generally confirms our classification based on the visual
inspection of the light curves and the period-amplitude diagram. A few deviating objects
in Figure 6.2 deserve further discussion. Star lm0427l17346 lies rather separated from
both groups. We visually inspected its light curve and analysed its position on the period-
amplitude diagram (Fig. 6.1), but did not find any peculiarities. Stars lm0293n31080 and
112
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3
Figure 6.2 A21 Fourier parameter versus φ21. Empty circles are RRab stars, filled circlesare RRc variables. Errors are omitted for clarifying, but they are provided in Table 6.4.
lm0434l7912 were classified as RRc, however they are both located in the region of the
fundamental-mode RR Lyrae stars in Figure 6.2. It should be noted that one of them (star
lm0293n31080) was classified as RRab also by the OGLE III survey. On the contrary, star
lm0426n9666, which we classified as RRab, is located in the region of the first-overtone
mode RR Lyrae stars. In the following, for these few objects we adopted the classification
based on the visual inspection of the light curves and the period-amplitude diagram.
Figure 6.3 shows the distribution of RR Lyrae stars on the φ31 versus logarithm of period
plane. There is a clear separation between RRab and RRc stars. Furthermore, for the RRab
stars there is a quite clear linear correlation of the φ31 parameter with Log(P), whereas the
correlation is definitely worse and errors are much larger for the RRc stars.
113
6.3. FOURIER ANALYSIS OF THE RR LYRAE STARS IN TILE LMC 8_3
Figure 6.3 φ31 parameter versus logarithm of the period. Empty circles are RRab stars,filled circles are RRc stars.
114
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3
ERO
S-2
idTy
peφ21
σφ21
φ31
σφ31
A21
σA
21
A31
σA
31
Dm
lm03
01n1
6576
c2.
582
0.44
87.
430.
497
0.08
10.
030.
067
0.02
855
.02
lm03
05m
3332
c2.
929
0.13
75.
286
0.46
30.
222
0.02
90.
070.
026
12.2
4lm
0300
l152
47c
2.97
40.
821
7.33
70.
954
0.03
70.
020.
027
0.01
877
.58
lm04
36l1
7456
c2.
780.
182
4.56
90.
467
0.13
0.02
30.
057
0.02
123
.75
lm02
93l1
8421
c2.
794
0.14
94.
851
0.59
50.
174
0.02
50.
051
0.02
27.
55lm
0437
m22
126
c3.
084
0.09
58.
061
0.27
70.
186
0.01
80.
065
0.01
680
.42
lm04
25l2
4389
c2.
970.
133
5.49
91.
467
0.23
10.
029
0.01
50.
019
29.7
7lm
0427
m19
332
c2.
987
0.12
66.
432
0.64
80.
201
0.02
40.
046
0.02
136
.99
lm04
35m
1088
8c
3.28
10.
179
4.73
10.
368
0.13
50.
024
0.07
30.
021
16.1
7lm
0425
l205
13c
2.99
50.
085.
482
0.37
20.
242
0.01
90.
057
0.01
79.
81lm
0423
l200
69c
3.05
30.
083
4.94
90.
316
0.22
20.
018
0.06
0.01
79.
68lm
0302
n485
8c
2.84
10.
108
5.35
40.
270.
206
0.02
10.
084
0.02
5.17
lm02
91k2
4862
c2.
553
0.19
35.
227
0.74
70.
104
0.01
90.
032
0.01
628
.52
lm04
35m
9109
c3.
012
0.09
5.15
80.
291
0.22
0.01
90.
071
0.01
722
.31
lm04
34n1
4310
c2.
715
0.09
65.
029
0.25
0.24
30.
022
0.09
60.
0215
.58
lm02
91l1
1940
c2.
975
0.07
26.
127
0.16
70.
234
0.01
60.
101
0.01
58.
36lm
0424
m19
442
c3.
365
0.12
2.58
20.
284
0.19
40.
023
0.08
20.
0234
.97
lm04
25n1
5519
c3.
010.
111
5.88
90.
311
0.19
60.
021
0.07
50.
019
10.6
5lm
0291
n255
51c
2.86
10.
075.
628
0.24
90.
256
0.01
70.
073
0.01
65.
39lm
0425
n186
80c
2.33
80.
099
4.33
90.
285
0.17
60.
017
0.06
40.
015
16.9
4lm
0304
m29
52c
2.92
50.
114
5.94
40.
409
0.20
20.
023
0.06
30.
021
7.39
lm03
03n3
1583
c3.
038
0.08
76.
288
0.19
80.
205
0.01
80.
087
0.01
79.
31lm
0301
n792
9c
3.06
50.
088
6.41
50.
314
0.22
10.
019
0.06
60.
017
33.8
1lm
0425
k931
9c
3.15
10.
063
5.66
40.
415
0.26
80.
017
0.04
40.
015
14.4
5lm
0434
l231
90c
2.67
30.
172
7.46
20.
811
0.12
40.
020.
029
0.01
860
.67
lm03
03m
2250
4c
2.89
20.
189
5.08
60.
841
0.10
10.
019
0.02
70.
015
6.07
lm04
25n1
3753
c3.
478
0.90
94.
959
0.20
40.
029
0.01
70.
111
0.02
35.2
6lm
0303
n168
41c
3.1
0.20
36.
969
0.74
40.
103
0.02
0.03
40.
018
64.1
1lm
0291
n154
12c
3.09
30.
177
6.55
30.
566
0.11
70.
020.
042
0.01
911
.61
lm03
00m
6808
c2.
557
0.11
76.
998
0.27
40.
157
0.01
80.
063
0.01
815
.81
115
6.3. FOURIER ANALYSIS OF THE RR LYRAE STARS IN TILE LMC 8_3lm
0301
m15
847
c2.
893
0.07
45.
838
0.20
60.
241
0.01
70.
088
0.01
612
.31
lm04
36m
8308
c3.
514
1.47
76.
572
0.64
60.
0090
0.01
30.
034
0.01
817
.32
lm03
12l1
5193
c2.
536
0.11
25.
699
0.22
40.
206
0.02
20.
104
0.02
18.
3lm
0425
k462
5c
3.44
20.
417.
988
0.57
60.
088
0.02
80.
055
0.02
671
.25
lm04
23l1
7670
c3.
157
0.14
36.
20.
656
0.14
10.
020.
037
0.01
89.
7lm
0293
m19
803
c2.
782
0.13
26.
773
0.94
30.
136
0.01
80.
022
0.01
558
.37
lm03
03l8
655
c3.
60.
238
2.64
11.
271
0.13
80.
031
0.02
30.
023
39.7
1lm
0310
n115
85c
3.50
60.
157
5.97
80.
666
0.23
60.
036
0.06
70.
0310
.46
lm03
00l6
753
c3.
104
0.15
56.
582
0.53
50.
143
0.02
20.
048
0.02
9.62
lm04
36l1
5993
c2.
905
0.51
27.
136
1.39
0.06
90.
028
0.01
70.
021
24.5
3lm
0302
l163
95c
3.60
70.
253
7.46
30.
558
0.11
80.
028
0.05
60.
026
63.4
9lm
0303
m10
773
c3.
372
0.13
66.
777
0.42
0.13
60.
018
0.04
90.
017
12.4
5lm
0425
l648
1c
3.11
30.
169
6.16
30.
281
0.13
60.
022
0.07
70.
022
9.2
lm04
35m
1828
0c
4.27
40.
629
7.67
30.
458
0.04
80.
022
0.05
60.
022
21.7
lm04
25l1
0656
c3.
045
0.11
17.
217
1.04
10.
169
0.01
90.
019
0.01
452
.65
lm04
36n1
0024
c3.
367
0.19
76.
560.
697
0.13
60.
026
0.04
50.
023
49.2
3lm
0300
l889
0c
2.55
40.
146
5.67
70.
149
0.11
40.
016
0.11
20.
016
12.2
lm03
10l1
2440
c2.
969
0.17
96.
243
0.62
60.
115
0.02
0.03
80.
018
25.6
5lm
0436
n142
85c
2.22
70.
154
4.76
50.
802
0.16
40.
024
0.03
70.
029.
08lm
0302
k378
2c
2.54
40.
251
7.29
50.
576
0.15
0.03
50.
067
0.03
155
.75
lm04
34l2
0168
c4.
188
0.34
67.
239
0.37
60.
074
0.02
30.
068
0.02
239
.83
lm02
93k3
0764
d2.
961
0.14
56.
973
0.51
20.
194
0.02
70.
058
0.02
563
.28
lm02
91l9
716
c3.
674
0.17
85.
350.
544
0.15
70.
027
0.05
90.
024
17.3
1lm
0435
m13
533
c3.
244
0.17
48.
143
0.91
80.
143
0.02
40.
029
0.02
46.4
7lm
0444
l813
8d
3.64
70.
185
3.91
41.
218
0.15
0.02
70.
023
0.01
928
.72
lm03
01n1
3911
d3.
127
0.13
25.
568
0.34
0.14
50.
018
0.06
10.
017
15.5
1lm
0291
l233
59c
3.31
90.
503
4.55
11.
199
0.08
10.
029
0.02
80.
023
44.4
7lm
0427
k107
85c
2.69
50.
175
6.27
70.
349
0.12
90.
022
0.07
50.
0214
.2lm
0425
m33
55c
2.62
20.
255
7.27
40.
397
0.15
60.
037
0.09
70.
034
72.2
9lm
0301
l269
33d
3.39
30.
203
6.64
60.
549
0.13
80.
027
0.05
70.
026
27.7
1lm
0422
n169
93c
2.87
40.
124
6.04
0.64
90.
194
0.02
30.
042
0.01
97.
54lm
0310
l126
53d
3.04
30.
135
3.99
30.
268
0.18
30.
024
0.08
90.
025
18.5
lm02
93n1
4230
d2.
847
0.17
45.
008
0.77
40.
165
0.02
80.
044
0.02
322
.6
116
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3lm
0435
k847
9d
2.89
10.
723.
443
0.63
70.
067
0.03
20.
072
0.03
226
.59
lm02
91n2
5922
d3.
194
0.15
47.
085
0.29
30.
140.
021
0.07
50.
021
32.7
6lm
0293
m10
988
c3.
236
0.18
86.
991
0.45
80.
111
0.02
0.04
40.
018
14.5
8lm
0305
m62
94c
3.00
30.
107
6.55
50.
216
0.17
20.
018
0.08
30.
018
27.4
7lm
0310
k930
0c
3.33
70.
108
5.30
20.
332
0.15
60.
017
0.05
70.
015
18.1
4lm
0434
m22
078
c2.
903
0.16
66.
653
1.15
60.
143
0.02
30.
020.
017
22.4
8lm
0444
l927
0c
2.94
0.22
17.
152
0.66
90.
141
0.02
90.
053
0.02
762
.54
lm04
25m
8144
c3.
775
0.17
87.
596
0.55
10.
123
0.02
10.
042
0.01
977
.87
lm03
00n2
4904
c3.
044
0.13
75.
612
0.6
0.16
30.
022
0.04
50.
019
34.3
1lm
0434
l198
10c
2.84
70.
252
6.94
61.
211
0.09
70.
023
0.01
80.
017
12.6
7lm
0427
l173
46c
4.99
80.
174
5.15
90.
326
0.12
40.
021
0.07
40.
0239
.84
lm04
36m
1197
7c
3.30
90.
162
5.65
10.
365
0.20
50.
032
0.09
70.
029
9.5
lm04
25k8
207
c3.
044
0.17
68.
203
0.33
20.
136
0.02
30.
072
0.02
318
.38
lm03
03m
2339
1d
2.83
30.
102
5.39
20.
238
0.23
80.
023
0.10
50.
021
6.93
lm04
27l4
507
c3.
979
0.63
56.
726
1.66
40.
061
0.02
80.
0040
0.02
117
.88
lm03
03k2
4363
d2.
792
0.11
45.
694
0.42
0.18
30.
020.
056
0.01
913
.77
lm04
24m
2288
7ab
2.19
0.04
4.57
80.
058
0.48
50.
017
0.29
50.
017
2.21
lm03
02k5
022
c4.
325
0.50
97.
250.
850.
060.
023
0.03
40.
021
15.1
2lm
0302
l126
78ab
2.06
80.
039
4.59
60.
055
0.49
60.
017
0.31
20.
017
2.41
lm03
03m
2298
9c
2.72
40.
703
7.35
0.20
40.
039
0.01
80.
106
0.02
147
.98
lm04
36n1
1172
ab2.
136
0.03
14.
731
0.04
20.
504
0.01
40.
333
0.01
41.
93lm
0300
l146
47c
3.45
60.
112
5.65
90.
249
0.24
60.
027
0.11
50.
024
10.8
1lm
0293
n310
80c
2.12
50.
062
4.33
10.
170.
335
0.01
90.
119
0.01
823
.27
lm04
34l7
912
c2.
195
0.08
44.
043
0.26
40.
446
0.03
40.
131
0.02
937
.59
lm03
12k2
1111
ab2.
101
0.03
24.
626
0.04
30.
506
0.01
40.
325
0.01
42.
16lm
0293
k392
8ab
2.07
30.
035
4.51
40.
058
0.41
50.
013
0.23
40.
012
9.58
lm02
93n3
0795
ab2.
222
0.03
64.
769
0.05
20.
50.
016
0.30
80.
016
2.31
lm04
32l1
2420
ab2.
122
0.08
34.
650.
390.
284
0.02
20.
063
0.01
942
.88
lm04
27n7
741
ab2.
256
0.02
64.
699
0.03
60.
474
0.01
10.
305
0.01
11.
2lm
0300
m99
35ab
2.29
70.
039
4.61
0.05
30.
397
0.01
40.
264
0.01
49.
15lm
0437
k157
72ab
2.23
30.
031
4.65
40.
043
0.49
50.
014
0.31
70.
014
1.88
lm04
34l2
0435
ab2.
171
0.03
44.
754
0.04
60.
491
0.01
50.
318
0.01
51.
49lm
0437
k226
54ab
2.27
50.
036
4.76
40.
053
0.51
0.01
70.
308
0.01
62.
39
117
6.3. FOURIER ANALYSIS OF THE RR LYRAE STARS IN TILE LMC 8_3lm
0436
n206
28ab
2.21
30.
041
4.47
30.
055
0.43
20.
016
0.28
90.
016
4.37
lm03
02n2
3523
ab2.
340.
043
4.55
0.06
90.
367
0.01
40.
211
0.01
410
.81
lm02
93k2
8352
ab2.
254
0.03
34.
534
0.04
20.
404
0.01
20.
291
0.01
26.
65lm
0303
n139
77ab
2.25
40.
031
4.52
40.
042
0.44
90.
013
0.30
10.
013
1.53
lm03
03n1
5322
ab2.
162
0.03
24.
710.
044
0.48
90.
014
0.31
50.
014
1.76
lm02
93m
1437
5ab
2.18
90.
029
4.67
80.
040.
510.
014
0.32
80.
013
2.55
lm03
01l2
4255
ab2.
201
0.03
44.
732
0.04
70.
510.
016
0.32
50.
015
2.32
lm04
36l2
0450
ab2.
246
0.04
34.
792
0.05
90.
564
0.02
20.
366
0.02
13.
12lm
0437
m20
444
ab2.
439
0.03
65.
141
0.05
70.
553
0.01
80.
312
0.01
62.
07lm
0302
l232
97ab
2.13
40.
036
4.67
60.
050.
547
0.01
70.
341
0.01
73.
26lm
0291
m87
10ab
2.29
40.
045
4.84
90.
073
0.43
40.
018
0.23
90.
017
1.8
lm04
35k2
0062
ab2.
142
0.03
94.
654
0.05
30.
511
0.01
80.
332
0.01
82.
55lm
0291
n201
01ab
2.30
20.
028
4.81
40.
039
0.46
70.
012
0.30
30.
012
1.67
lm03
00m
1717
8ab
2.25
90.
035
4.76
50.
048
0.51
90.
016
0.33
90.
016
2.19
lm03
02m
2248
7ab
2.44
30.
052
4.68
90.
060.
357
0.01
80.
297
0.01
86.
57lm
0303
m17
152
ab2.
312
0.03
94.
844
0.05
60.
535
0.01
90.
332
0.01
82.
93lm
0300
k121
84ab
2.29
40.
038
4.76
0.05
60.
396
0.01
40.
245
0.01
41.
69lm
0303
k252
10ab
2.59
60.
045
5.56
60.
073
0.51
60.
021
0.27
60.
019
0.87
lm04
35m
1779
3ab
2.23
50.
034
4.74
40.
048
0.47
30.
015
0.29
80.
014
1.3
lm04
35m
2356
3ab
2.38
30.
047
4.86
70.
091
0.35
90.
016
0.17
50.
015
4.13
lm04
25n2
3250
ab2.
093
0.04
54.
581
0.07
50.
468
0.01
90.
258
0.01
82.
73lm
0300
m19
324
ab2.
410.
033
4.87
10.
058
0.36
70.
011
0.19
30.
011
3.92
lm03
00l1
3312
ab2.
174
0.03
94.
439
0.05
60.
453
0.01
60.
281
0.01
62.
59lm
0291
n604
0ab
2.32
40.
034
4.67
70.
048
0.40
80.
013
0.26
60.
013
2.65
lm03
01n1
6814
ab2.
245
0.03
44.
629
0.06
40.
439
0.01
40.
210.
013
6.98
lm04
26n1
2018
ab2.
096
0.05
34.
590.
073
0.45
80.
022
0.29
70.
022
1.86
lm02
91n2
0061
ab2.
207
0.04
24.
582
0.07
0.39
90.
015
0.22
20.
015
6.67
lm03
01n2
1605
ab2.
063
0.03
34.
703
0.04
0.43
30.
013
0.33
70.
013
5.24
lm03
01m
2278
0ab
2.26
70.
037
4.75
90.
050.
495
0.01
60.
325
0.01
61.
26lm
0301
k175
54ab
2.29
90.
041
4.96
70.
060.
510.
019
0.30
40.
018
1.58
lm04
25l1
4852
ab2.
126
0.03
24.
753
0.04
40.
515
0.01
50.
325
0.01
52.
29lm
0437
m17
477
ab2.
062
0.05
94.
552
0.09
10.
336
0.01
80.
213
0.01
719
.77
lm03
10k1
1253
ab2.
233
0.04
54.
797
0.06
30.
515
0.02
10.
331
0.02
2.19
118
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3lm
0434
k220
95ab
2.28
30.
034
4.94
50.
050.
535
0.01
60.
327
0.01
62.
1lm
0425
k115
00ab
2.15
40.
064
4.44
10.
086
0.34
20.
020.
245
0.02
3.99
lm04
34m
6139
ab2.
156
0.03
74.
728
0.04
90.
528
0.01
70.
348
0.01
72.
26lm
0301
m15
584
ab2.
317
0.03
5.08
80.
043
0.53
90.
015
0.33
10.
014
1.67
lm04
46k2
0706
ab1.
910.
068
4.00
60.
122
0.45
50.
028
0.23
0.02
65.
62lm
0427
m14
753
ab2.
155
0.04
74.
681
0.06
40.
505
0.02
20.
330.
021
2.95
lm04
37n1
4794
ab2.
282
0.04
74.
968
0.07
50.
494
0.02
10.
271
0.01
91.
81lm
0300
m23
701
ab2.
187
0.04
14.
731
0.05
70.
507
0.01
90.
318
0.01
82.
72lm
0425
m12
624
ab2.
302
0.04
24.
922
0.07
0.48
10.
018
0.26
70.
017
1.57
lm03
00m
2326
6ab
2.17
60.
075
4.96
70.
116
0.57
20.
038
0.32
70.
034
3.57
lm03
01n1
4847
ab2.
295
0.05
34.
417
0.14
50.
380.
018
0.12
80.
017
12.9
1lm
0435
m93
34ab
2.19
80.
043
4.74
10.
058
0.52
10.
020.
335
0.01
93.
34lm
0423
l117
40ab
2.68
10.
087
5.21
40.
199
0.35
50.
029
0.15
10.
026
3.04
lm02
91k1
0561
ab2.
136
0.04
14.
631
0.05
50.
461
0.01
70.
314
0.01
71.
62lm
0291
m11
933
ab2.
197
0.05
14.
512
0.11
80.
391
0.01
80.
152
0.01
821
.22
lm04
23n2
6224
ab2.
297
0.03
94.
966
0.05
80.
548
0.01
90.
332
0.01
82.
39lm
0302
k147
96ab
2.40
50.
054.
811
0.06
90.
450.
020.
290.
022.
7lm
0300
m11
839
ab2.
191
0.03
44.
777
0.04
80.
487
0.01
50.
311
0.01
41.
46lm
0303
l176
71ab
2.22
50.
032
4.80
10.
046
0.49
80.
014
0.31
70.
013
1.85
lm04
23l7
926
ab2.
224
0.03
54.
773
0.05
50.
456
0.01
40.
260.
014
1.41
lm04
27l1
8856
ab2.
259
0.04
64.
812
0.06
40.
466
0.02
0.30
30.
019
1.15
lm03
03m
1781
2ab
2.31
80.
038
4.86
80.
052
0.46
70.
016
0.30
10.
016
1.24
lm03
02n1
2351
ab2.
448
0.06
74.
655
0.12
20.
408
0.02
50.
199
0.02
43.
26lm
0300
k143
35ab
2.19
10.
044.
529
0.05
40.
363
0.01
30.
253
0.01
31.
51lm
0300
n272
86ab
2.23
80.
028
4.78
20.
039
0.50
40.
013
0.31
40.
012
2.06
lm03
02l1
2960
ab2.
313
0.06
4.80
30.
103
0.39
90.
022
0.22
20.
027.
43lm
0300
n210
91ab
2.24
40.
048
4.89
50.
069
0.57
30.
024
0.35
0.02
33.
05lm
0434
k900
8ab
2.35
0.03
84.
505
0.06
0.34
40.
012
0.19
0.01
22.
78lm
0301
l116
30ab
2.44
10.
041
5.02
30.
075
0.39
60.
015
0.2
0.01
43.
16lm
0300
k176
65ab
2.35
70.
048
5.03
70.
070.
537
0.02
30.
325
0.02
22.
69lm
0291
l107
75ab
2.49
10.
041
5.35
20.
061
0.58
20.
021
0.34
60.
021.
43lm
0300
m11
600
ab2.
140.
044
4.6
0.05
90.
462
0.01
90.
307
0.01
83.
5lm
0437
n150
49ab
2.13
70.
044
4.78
60.
065
0.48
90.
019
0.29
70.
018
2.07
119
6.3. FOURIER ANALYSIS OF THE RR LYRAE STARS IN TILE LMC 8_3lm
0434
n137
04ab
2.27
70.
044
5.08
40.
064
0.54
30.
021
0.33
60.
021.
7lm
0427
l124
62ab
2.17
30.
072
4.46
20.
108
0.30
30.
020.
197
0.01
924
.7lm
0435
l524
7ab
2.33
20.
062
4.96
90.
150.
405
0.02
30.
155
0.02
13.
35lm
0434
m21
424
ab2.
526
0.09
94.
515
0.14
50.
295
0.02
80.
202
0.02
611
.26
lm04
37n8
455
ab2.
248
0.06
54.
503
0.07
30.
371
0.02
20.
309
0.02
39.
94lm
0444
l200
33ab
2.26
80.
131
4.81
80.
187
0.34
30.
041
0.24
10.
039
18.2
7lm
0293
n208
70ab
2.26
80.
039
4.81
0.04
90.
450.
016
0.33
10.
016
2.43
lm04
37m
2088
3ab
2.27
10.
039
4.89
30.
057
0.49
30.
017
0.29
70.
017
1.82
lm02
93m
1962
8ab
2.33
80.
039
5.18
20.
059
0.50
80.
018
0.29
30.
017
1.86
lm03
03n1
2799
ab2.
288
0.04
74.
902
0.07
70.
424
0.01
80.
235
0.01
70.
97lm
0434
l170
31ab
2.07
80.
051
4.72
10.
071
0.55
0.02
50.
343
0.02
53.
95lm
0293
m19
003
ab2.
328
0.04
64.
826
0.05
20.
366
0.01
50.
315
0.01
68.
53lm
0437
k153
28ab
2.28
90.
042
4.89
40.
061
0.56
20.
021
0.33
60.
023.
01lm
0291
k100
47ab
2.28
70.
046
4.97
10.
067
0.55
70.
022
0.33
30.
021
2.61
lm02
93k2
5226
ab2.
438
0.03
75.
113
0.05
30.
503
0.01
70.
310.
016
0.87
lm03
03n2
7302
ab2.
539
0.04
85.
322
0.08
0.46
80.
020.
254
0.01
91.
74lm
0435
n113
21ab
2.20
10.
057
4.74
80.
095
0.38
20.
020.
211
0.01
93.
81lm
0437
k868
1ab
2.15
80.
053
4.74
20.
092
0.40
70.
020.
215
0.01
91.
86lm
0300
l207
39ab
2.27
40.
038
5.03
0.05
60.
473
0.01
60.
281
0.01
61.
76lm
0310
l181
47ab
2.18
90.
055
4.85
0.08
0.49
40.
024
0.30
70.
024
3.06
lm03
02l2
6417
ab2.
304
0.05
34.
974
0.07
20.
548
0.02
60.
353
0.02
52.
64lm
0310
k180
10ab
2.28
60.
034
4.97
80.
050.
529
0.01
60.
311
0.01
52.
12lm
0300
k165
63ab
2.30
30.
037
5.04
10.
057
0.51
60.
017
0.29
20.
016
1.91
lm03
03m
2124
5ab
2.17
60.
044
4.84
30.
065
0.49
60.
020.
301
0.01
92.
53lm
0437
k139
06ab
2.50
80.
054
5.37
20.
090.
476
0.02
30.
264
0.02
10.
62lm
0293
m17
000
ab2.
356
0.03
95.
070.
058
0.47
80.
017
0.29
0.01
60.
86lm
0435
m70
58ab
2.16
60.
069
4.55
10.
110.
332
0.02
10.
184
0.02
27.
92lm
0425
m42
88ab
2.33
40.
061
4.95
50.
109
0.48
10.
026
0.24
50.
024
2.13
lm04
35n1
3913
ab2.
475
0.06
15.
398
0.12
80.
377
0.02
10.
171
0.01
921
.96
lm04
26m
2441
4ab
2.50
20.
071
5.44
70.
121
0.44
90.
029
0.25
10.
026
1.19
lm04
25l1
0247
ab2.
221
0.04
64.
869
0.06
90.
487
0.02
0.29
20.
019
1.63
lm03
10k1
5738
ab2.
216
0.08
14.
521
0.18
40.
270.
020.
117
0.02
17.1
3lm
0435
k123
09ab
2.29
10.
046
4.99
30.
069
0.45
90.
019
0.28
30.
019
1.05
120
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3lm
0435
l985
8ab
2.25
30.
068
4.94
10.
103
0.49
60.
030.
292
0.02
92.
21lm
0434
k730
2ab
2.66
70.
055
5.65
0.08
40.
536
0.02
70.
295
0.02
60.
59lm
0293
l126
31ab
2.41
30.
044
5.22
40.
069
0.49
80.
020.
290.
019
0.84
lm04
35k1
7589
ab2.
509
0.06
15.
342
0.09
80.
480.
026
0.27
80.
024
0.76
lm02
93l5
252
ab2.
340.
047
5.21
0.07
40.
471
0.02
0.27
20.
019
1.94
lm03
12k4
503
ab2.
686
0.07
45.
942
0.14
20.
498
0.03
30.
238
0.02
99.
81lm
0436
k158
55ab
2.15
50.
074
5.56
60.
182
0.50
30.
033
0.17
90.
028
7.97
lm04
25l2
1048
ab2.
228
0.03
94.
743
0.05
40.
492
0.01
70.
316
0.01
72.
05lm
0427
m20
466
ab2.
339
0.06
45.
102
0.13
50.
452
0.02
60.
195
0.02
34.
15lm
0435
k120
02ab
2.52
10.
046
5.40
90.
066
0.54
0.02
20.
326
0.02
10.
7lm
0424
n522
7ab
2.21
10.
048
4.78
10.
067
0.55
0.02
30.
349
0.02
23.
64lm
0437
m97
13ab
2.23
40.
039
4.77
20.
058
0.49
20.
017
0.29
40.
017
2.27
lm03
03l2
6148
ab2.
467
0.05
65.
202
0.09
50.
438
0.02
20.
240.
021
1.01
lm03
02k1
3534
ab2.
424
0.05
5.17
90.
082
0.48
10.
021
0.26
60.
020.
87lm
0305
k570
4ab
2.47
80.
065
5.33
40.
112
0.44
30.
026
0.23
40.
024
0.87
lm04
37l1
5735
ab2.
287
0.06
25.
199
0.10
80.
430.
025
0.21
10.
024
2.76
lm04
34m
1964
8ab
2.47
90.
054
5.24
80.
095
0.40
80.
020.
214
0.01
90.
98lm
0300
n139
61ab
2.32
70.
029
4.92
50.
041
0.51
0.01
30.
325
0.01
31.
03lm
0303
l276
10ab
2.38
90.
061
5.24
90.
101
0.41
70.
023
0.23
40.
022
1.37
lm02
92n2
2612
ab2.
614
0.08
25.
327
0.16
50.
432
0.03
20.
204
0.02
91.
71lm
0293
n182
29ab
2.38
10.
065
5.31
0.11
60.
437
0.02
60.
222
0.02
51.
85lm
0303
n974
5ab
2.65
20.
074
5.85
20.
233
0.48
20.
032
0.13
80.
028
37.0
3lm
0435
m18
273
ab2.
603
0.07
85.
695
0.38
60.
402
0.02
90.
080.
025
12.4
3lm
0423
l211
78ab
2.19
40.
067
5.05
70.
112
0.43
50.
026
0.24
50.
024
2.9
lm03
03n1
6102
ab2.
418
0.03
25.
128
0.04
50.
516
0.01
50.
315
0.01
40.
97lm
0424
n125
43ab
2.39
0.03
55.
115
0.05
10.
503
0.01
60.
306
0.01
60.
71lm
0300
n199
27ab
2.56
50.
083
5.37
80.
149
0.40
30.
031
0.19
80.
031
1.03
lm03
00l2
5566
ab2.
454
0.06
5.31
60.
10.
399
0.02
20.
226
0.02
11.
11lm
0435
k158
16ab
2.29
70.
045
5.02
30.
067
0.47
20.
019
0.28
90.
018
1.21
lm03
00k1
1860
ab2.
484
0.05
75.
302
0.12
10.
428
0.02
20.
184
0.02
1.94
lm03
03m
1100
5ab
2.37
40.
035.
249
0.04
40.
528
0.01
40.
320.
013
2.12
lm03
01n1
4943
ab2.
391
0.09
84.
398
0.32
60.
379
0.03
40.
111
0.03
8.01
lm04
36m
1701
1ab
2.53
70.
046
5.27
80.
078
0.50
20.
021
0.27
10.
019
1.03
121
6.3. FOURIER ANALYSIS OF THE RR LYRAE STARS IN TILE LMC 8_3lm
0301
l227
86ab
2.46
70.
048
5.26
60.
075
0.48
40.
021
0.27
70.
019
0.7
lm04
36n8
236
ab2.
313
0.05
74.
707
0.07
40.
458
0.02
40.
314
0.02
43.
22lm
0300
m25
109
ab2.
382
0.03
55.
290.
056
0.53
60.
017
0.29
10.
016
2.43
lm03
10l1
6334
ab2.
532
0.10
95.
045
0.65
40.
375
0.03
70.
066
0.03
119
.71
lm02
93l2
5506
ab2.
207
0.03
54.
869
0.04
90.
469
0.01
50.
30.
015
1.47
lm03
10l1
4484
ab2.
369
0.04
55.
118
0.06
30.
519
0.02
10.
321
0.02
1.76
lm03
01l2
5140
ab2.
371
0.03
45.
009
0.04
80.
552
0.01
70.
340.
016
2.65
lm02
91l2
6545
ab2.
413
0.03
35.
188
0.04
90.
545
0.01
60.
324
0.01
51.
38lm
0434
n841
3ab
2.58
0.04
85.
441
0.07
60.
521
0.02
20.
293
0.02
10.
64lm
0300
n120
88ab
2.40
50.
041
5.32
0.07
0.55
60.
020.
287
0.01
81.
74lm
0427
k174
52ab
2.31
70.
075
5.30
60.
142
0.44
40.
030.
221
0.02
74.
07lm
0300
n121
09ab
2.48
60.
043
5.29
70.
066
0.48
90.
019
0.27
50.
018
0.63
lm04
26n9
666
ab2.
435
0.19
4.89
70.
355
0.16
60.
030.
096
0.02
748
.54
lm04
34n2
2292
ab2.
656
0.08
65.
484
0.17
80.
501
0.03
90.
218
0.03
45.
84lm
0303
m56
51ab
2.59
50.
055
5.38
60.
107
0.46
70.
023
0.22
10.
022.
12lm
0301
m15
788
ab2.
339
0.08
65.
239
0.13
30.
452
0.03
50.
279
0.03
36.
1lm
0305
m38
82ab
2.54
0.05
5.33
0.07
80.
474
0.02
10.
277
0.02
0.78
lm03
05m
7850
ab2.
598
0.09
95.
338
0.19
90.
309
0.02
90.
151
0.02
616
.23
lm04
27m
6338
ab2.
543
0.05
25.
259
0.11
10.
479
0.02
30.
204
0.01
912
.2lm
0434
n173
83ab
2.40
40.
086
5.61
10.
224
0.37
30.
029
0.13
60.
026
5.61
lm03
01l1
6487
ab2.
667
0.14
96.
226
0.59
90.
322
0.04
40.
087
0.03
844
.37
lm03
00l2
3462
ab2.
440.
047
5.29
10.
073
0.49
90.
021
0.28
60.
020.
88lm
0310
l189
11ab
2.59
0.07
15.
605
0.18
80.
415
0.02
70.
145
0.02
44.
97Ta
ble
6.4:
Four
ierp
aram
eter
soft
he25
1co
nfirm
edR
RLy
rae
star
sin
tile
LMC
8_3.
122
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3
6.4 Metallicity of the RR Lyrae stars in tile LMC 8_3
Spectroscopically determined metallicities are not available for the RR Lyrae stars in tile
LMC 8_3, so we estimated individual photometric metal abundances from the Fourier pa-
rameters of the light curves (see Subsection 1.5.1). In particular, we applied Eqs. 1.11 and
1.13 to derive the metallicity of RRab and RRc stars, respectively, and Eq. 1.12 to obtain
the φ31 Fourier parameters in the Kepler magnitudes.
Following Cacciari et al. (2005) and Kapakos et al. (2011) we only considered RRab
stars for which Dm < 5 (132 RRab stars) and RRc stars for which σ(φ31) < 0.3 (20 RRc
stars). Among the RRc stars we also discarded:
• lm0437m22126, since it has a positive value of metallicity ([Fe/H] = 0.490±0.368
dex), out of the range of typical metallicities of RR Lyrae stars in the LMC;
• lm0300l14647. This star was classified as RRc by us, and as RRd by OGLE III.
• lm0293n31080 - RRc according to our classification, but RRab according to the
OGLE III catalogue. Since the classification of this star is doubtful we discarded
this star from the following analysis. However, it should be noted that if the star were
considered as an RRab its Dm value would be larger than 5, hence, its photometric
metallicity would not be reliable.
Individual photometric metallicities for the 132 RRab stars and 17 RRc stars are pre-
sented in Tables 6.5 and 6.6, respectively. They are all on the Carretta et al. (2009) metallic-
ity scale. The weighted mean metallicity of the RRab stars in tile LMC 8_3 is: ⟨[Fe/H]C09⟩ =
(−1.58 ± 0.01) dex , σ = 0.5, average on 132 stars. The weighted mean metallicity mean
of the RRc stars is: ⟨[Fe/H]C09⟩ = (−1.82 ± 0.04) dex, σ = 0.3, average on 17 stars.
There is a systematic difference of ∼ 0.25 dex between the two mean metallicities, with the
RRab stars being more metal rich. Nemec et al. (2013) calibrated Eq. 1.11 using accurate
pulsation periods, Fourier light curve parameters and spectroscopic metal abundances of 37
field RRab stars observed by the Kepler satellite. Instead the sample of Kepler-field RRc
stars contained only four objects, so it was not possible to derive independently a relation
similar to Eq. 1.11 for the RRc stars. Nemec et al. (2013) added the four Kepler-RRc stars
to the sample of 106 RRc stars in 12 globular clusters analysed by Morgan et al. (2007),
who derived the P − φ31 − [Fe/H] relation on the range of metallicities from -2.2 to -1.0
123
6.4. METALLICITY OF THE RR LYRAE STARS IN TILE LMC 8_3
dex. Nemec et al. (2013) obtained Eq. 1.13 by recalibrating Morgan et al. (2007)’s relation.
Some systematics in the calibration of the two different relations used to estimate the metal-
licity of the RRab and RRc stars could be the cause of the systematic offset of ∼ 0.25 dex
we find between the metallicity of RRab and RRc stars in tile LMC 8_3.
124
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3
ERO
S-2
idPe
riod
φ31(V
)φ31_k
epEr
rorφ
31_k
ep[F
e/H] C
09
Erro
r[Fe/H] C
09
Dm
(day
s)(d
ex)
dex
lm04
36n8
236
0.65
0192
4.70
74.
858
0.07
8-2
.97
0.24
93.
22lm
0434
k900
80.
5676
354.
505
4.65
60.
065
-2.7
110.
22.
78lm
0300
k143
350.
5661
574.
529
4.68
0.06
-2.6
280.
184
1.51
lm04
25k1
1500
0.54
0233
4.44
14.
592
0.09
-2.5
840.
254
3.99
lm02
93l2
5506
0.65
7982
4.86
95.
020.
055
-2.5
630.
177
1.47
lm04
25l2
1048
0.61
5813
4.74
34.
894
0.06
-2.5
370.
184
2.05
lm04
37m
9713
0.62
0011
4.77
24.
923
0.06
4-2
.496
0.19
22.
27lm
0300
m11
600
0.57
0995
4.6
4.75
10.
064
-2.4
850.
191
3.5
lm04
24n5
227
0.61
9983
4.78
14.
932
0.07
2-2
.471
0.21
13.
64lm
0300
l133
120.
5274
524.
439
4.59
0.06
2-2
.444
0.18
22.
59lm
0302
n123
510.
5661
344.
655
4.80
60.
125
-2.2
90.
323
3.26
lm04
37k8
681
0.58
9055
4.74
24.
893
0.09
6-2
.287
0.25
71.
86lm
0434
l170
310.
5829
374.
721
4.87
20.
076
-2.2
830.
213.
95lm
0291
k105
610.
5571
4.63
14.
782
0.06
1-2
.261
0.17
51.
62lm
0435
n113
210.
5871
834.
748
4.89
90.
098
-2.2
540.
262
3.81
lm03
01l2
5140
0.66
3184
5.00
95.
160.
055
-2.2
180.
167
2.65
lm04
25l1
0247
0.60
7461
4.86
95.
020.
074
-2.1
260.
202
1.63
lm03
00n1
3961
0.62
3548
4.92
55.
076
0.04
9-2
.12
0.14
91.
03lm
0426
n120
180.
5294
64.
594.
741
0.07
7-2
.08
0.20
41.
86lm
0303
m21
245
0.59
3551
4.84
34.
994
0.07
-2.0
70.
192.
53lm
0425
n232
500.
5251
914.
581
4.73
20.
079
-2.0
580.
207
2.73
lm03
10l1
8147
0.59
0217
4.85
5.00
10.
084
-2.0
240.
219
3.06
lm02
93n2
0870
0.57
819
4.81
4.96
10.
055
-2.0
150.
157
2.43
lm04
37n1
5049
0.57
1014
4.78
64.
937
0.07
-2.0
080.
187
2.07
lm04
27m
1475
30.
5440
14.
681
4.83
20.
069
-2.0
060.
184
2.95
lm03
00l2
3462
0.74
4314
5.29
15.
442
0.07
7-2
.004
0.22
80.
88lm
0435
k158
160.
6387
945.
023
5.17
40.
072
-1.9
930.
196
1.21
lm03
00n2
7286
0.56
6301
4.78
24.
933
0.04
7-1
.975
0.13
92.
06lm
0436
n206
280.
4931
074.
473
4.62
40.
061
-1.9
730.
166
4.37
lm04
35l9
858
0.60
9462
4.94
15.
092
0.10
6-1
.964
0.26
62.
21
125
6.4. METALLICITY OF THE RR LYRAE STARS IN TILE LMC 8_3lm
0423
l792
60.
5618
184.
773
4.92
40.
061
-1.9
550.
166
1.41
lm04
35m
9334
0.55
085
4.74
14.
892
0.06
4-1
.928
0.17
3.34
lm03
00m
1183
90.
5597
334.
777
4.92
80.
055
-1.9
260.
153
1.46
lm03
03n1
3977
0.49
9556
4.52
44.
675
0.04
9-1
.922
0.14
21.
53lm
0310
l144
840.
6616
525.
118
5.26
90.
068
-1.9
220.
188
1.76
lm03
00m
2370
10.
5461
024.
731
4.88
20.
063
-1.9
070.
167
2.72
lm03
03l1
7671
0.56
0588
4.80
14.
952
0.05
3-1
.877
0.14
81.
85lm
0427
l188
560.
5626
984.
812
4.96
30.
069
-1.8
710.
179
1.15
lm04
37k1
5328
0.58
4568
4.89
45.
045
0.06
6-1
.869
0.17
53.
01lm
0434
m61
390.
5403
584.
728
4.87
90.
055
-1.8
590.
152
2.26
lm04
23l2
1178
0.63
2125
5.05
75.
208
0.11
5-1
.858
0.28
22.
9lm
0291
n604
00.
5276
194.
677
4.82
80.
055
-1.8
540.
152.
65lm
0302
k147
960.
5596
354.
811
4.96
20.
074
-1.8
450.
187
2.7
lm04
35k1
2309
0.60
8992
4.99
35.
144
0.07
4-1
.835
0.19
1.05
lm04
37m
2088
30.
5802
874.
893
5.04
40.
063
-1.8
350.
166
1.82
lm04
25m
4288
0.59
7504
4.95
55.
106
0.11
2-1
.833
0.26
82.
13lm
0303
n127
990.
5818
484.
902
5.05
30.
081
-1.8
270.
203
0.97
lm02
91l2
6545
0.66
9488
5.18
85.
339
0.05
5-1
.801
0.15
91.
38lm
0435
k200
620.
5141
254.
654
4.80
50.
059
-1.7
730.
156
2.55
lm03
03m
1781
20.
5655
564.
868
5.01
90.
058
-1.7
660.
155
1.24
lm04
25l1
4852
0.53
6054
4.75
34.
904
0.05
1-1
.761
0.14
12.
29lm
0424
n125
430.
6353
165.
115
5.26
60.
057
-1.7
430.
157
0.71
lm03
01m
2278
00.
5354
594.
759
4.91
0.05
6-1
.742
0.15
1.26
lm03
02l2
6417
0.59
0296
4.97
45.
125
0.07
7-1
.731
0.19
2.64
lm03
00n2
1091
0.56
746
4.89
55.
046
0.07
4-1
.722
0.18
33.
05lm
0310
k180
100.
5902
994.
978
5.12
90.
056
-1.7
210.
151
2.12
lm03
05m
3882
0.71
0488
5.33
5.48
10.
082
-1.7
010.
219
0.78
lm03
02l2
3297
0.51
1473
4.67
64.
827
0.05
6-1
.697
0.14
93.
26lm
0291
k100
470.
5850
244.
971
5.12
20.
072
-1.6
950.
179
2.61
lm03
03n1
6102
0.63
2428
5.12
85.
279
0.05
2-1
.692
0.14
60.
97lm
0435
m17
793
0.52
4956
4.74
44.
895
0.05
5-1
.677
0.14
51.
3lm
0310
k112
530.
5371
494.
797
4.94
80.
068
-1.6
730.
169
2.19
lm02
93m
1437
50.
5079
954.
678
4.82
90.
048
-1.6
590.
133
2.55
126
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3lm
0300
k121
840.
5248
134.
764.
911
0.06
2-1
.641
0.15
61.
69lm
0427
m20
466
0.61
6626
5.10
25.
253
0.13
7-1
.639
0.30
94.
15lm
0300
n121
090.
6834
595.
297
5.44
80.
071
-1.6
240.
187
0.63
lm03
00k1
6563
0.59
2704
5.04
15.
192
0.06
3-1
.599
0.15
91.
91lm
0300
l207
390.
5890
665.
035.
181
0.06
2-1
.596
0.15
71.
76lm
0435
l524
70.
5718
234.
969
5.12
0.15
2-1
.594
0.32
53.
35lm
0300
m17
178
0.51
8967
4.76
54.
916
0.05
5-1
.576
0.14
22.
19lm
0303
n153
220.
5057
334.
714.
861
0.05
1-1
.568
0.13
61.
76lm
0301
l242
550.
5105
84.
732
4.88
30.
054
-1.5
670.
142.
32lm
0427
k174
520.
6754
985.
306
5.45
70.
144
-1.5
560.
333
4.07
lm02
93m
1700
00.
5952
245.
075.
221
0.06
4-1
.555
0.15
90.
86lm
0437
k157
720.
4883
224.
654
4.80
50.
05-1
.515
0.13
41.
88lm
0300
n120
880.
6723
565.
325.
471
0.07
5-1
.505
0.18
71.
74lm
0423
n262
240.
5593
664.
966
5.11
70.
064
-1.5
0.15
52.
39lm
0302
k135
340.
6208
85.
179
5.33
0.08
6-1
.498
0.2
0.87
lm03
03m
1100
50.
6437
75.
249
5.4
0.05
1-1
.492
0.14
2.12
lm04
25m
1262
40.
5470
654.
922
5.07
30.
075
-1.4
920.
173
1.57
lm03
01l2
2786
0.64
8027
5.26
65.
417
0.07
9-1
.481
0.19
10.
7lm
0437
l157
350.
6225
535.
199
5.35
0.11
1-1
.466
0.24
62.
76lm
0303
m56
510.
6925
475.
386
5.53
70.
11-1
.465
0.26
22.
12lm
0291
n201
010.
5172
544.
814
4.96
50.
047
-1.4
570.
127
1.67
lm03
00m
2510
90.
6528
915.
295.
441
0.06
2-1
.457
0.15
82.
43lm
0303
m17
152
0.52
4201
4.84
44.
995
0.06
2-1
.457
0.15
2.93
lm03
01l1
1630
0.56
8156
5.02
35.
174
0.07
9-1
.45
0.18
13.
16lm
0436
l204
500.
5113
954.
792
4.94
30.
064
-1.4
490.
154
3.12
lm03
03l2
6148
0.62
0647
5.20
25.
353
0.09
8-1
.447
0.22
11.
01lm
0436
m17
011
0.64
5996
5.27
85.
429
0.08
2-1
.442
0.19
41.
03lm
0300
k176
650.
5689
975.
037
5.18
80.
075
-1.4
280.
172
2.69
lm04
35m
2356
30.
5250
484.
867
5.01
80.
095
-1.4
180.
203
4.13
lm03
00m
2326
60.
5488
684.
967
5.11
80.
119
-1.4
140.
246
3.57
lm03
00m
1932
40.
5253
124.
871
5.02
20.
064
-1.4
120.
151
3.92
lm02
93k2
5226
0.58
6479
5.11
35.
264
0.05
9-1
.40.
146
0.87
lm04
34k2
2095
0.53
9682
4.94
55.
096
0.05
6-1
.384
0.13
92.
1
127
6.4. METALLICITY OF THE RR LYRAE STARS IN TILE LMC 8_3lm
0293
l525
20.
6129
085.
215.
361
0.07
8-1
.379
0.18
1.94
lm04
37n1
4794
0.54
4769
4.96
85.
119
0.07
9-1
.379
0.17
61.
81lm
0300
k118
600.
6437
575.
302
5.45
30.
124
-1.3
770.
268
1.94
lm04
27n7
741
0.48
284
4.69
94.
850.
044
-1.3
690.
121
1.2
lm03
03l2
7610
0.62
3747
5.24
95.
40.
104
-1.3
670.
227
1.37
lm04
34m
1964
80.
6226
045.
248
5.39
90.
098
-1.3
620.
216
0.98
lm04
34n1
3704
0.57
1166
5.08
45.
235
0.06
9-1
.349
0.15
91.
7lm
0291
m87
100.
5117
454.
849
5.0
0.07
7-1
.338
0.17
1.8
lm02
93l1
2631
0.61
0866
5.22
45.
375
0.07
4-1
.337
0.17
0.84
lm04
37k2
2654
0.49
1312
4.76
44.
915
0.05
9-1
.32
0.14
12.
39lm
0434
l204
350.
4888
14.
754
4.90
50.
053
-1.3
170.
132
1.49
lm03
00l2
5566
0.63
8155
5.31
65.
467
0.10
3-1
.314
0.22
41.
11lm
0301
k175
540.
5355
674.
967
5.11
80.
065
-1.3
070.
151.
58lm
0312
k211
110.
4606
4.62
64.
777
0.05
-1.2
930.
128
2.16
lm02
93n1
8229
0.62
8127
5.31
5.46
10.
119
-1.2
680.
246
1.85
lm04
34n8
413
0.67
0871
5.44
15.
592
0.08
-1.2
30.
185
0.64
lm02
93m
1962
80.
5811
415.
182
5.33
30.
064
-1.2
260.
147
1.86
lm03
10l1
8911
0.74
8431
5.60
55.
756
0.19
-1.2
150.
431
4.97
lm02
92n2
2612
0.62
4068
5.32
75.
478
0.16
7-1
.21
0.32
31.
71lm
0300
n199
270.
6371
295.
378
5.52
90.
151
-1.1
820.
297
1.03
lm03
05k5
704
0.62
165.
334
5.48
50.
115
-1.1
820.
232
0.87
lm02
93n3
0795
0.47
4027
4.76
94.
920.
058
-1.1
50.
134
2.31
lm03
01m
1558
40.
5413
45.
088
5.23
90.
05-1
.124
0.12
21.
67lm
0435
k175
890.
6126
355.
342
5.49
30.
101
-1.1
150.
203
0.76
lm04
35k1
2002
0.61
8774
5.40
95.
560.
071
-1.0
240.
152
0.7
lm03
03n2
7302
0.58
6637
5.32
25.
473
0.08
4-1
.003
0.16
61.
74lm
0423
l117
400.
5543
375.
214
5.36
50.
201
-0.9
910.
325
3.04
lm03
02l1
2678
0.42
4945
4.59
64.
747
0.06
1-0
.983
0.13
52.
41lm
0437
k139
060.
5943
325.
372
5.52
30.
094
-0.9
590.
177
0.62
lm04
26m
2441
40.
6068
695.
447
5.59
80.
124
-0.8
960.
217
1.19
lm02
91l1
0775
0.57
0992
5.35
25.
503
0.06
6-0
.863
0.13
41.
43lm
0437
m20
444
0.51
1423
5.14
15.
292
0.06
3-0
.822
0.12
62.
07lm
0436
n111
720.
4317
334.
731
4.88
20.
049
-0.8
190.
115
1.93
128
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3lm
0424
m22
887
0.39
8125
4.57
84.
729
0.06
4-0
.735
0.13
22.
21lm
0434
k730
20.
6101
925.
655.
801
0.08
8-0
.592
0.14
70.
59lm
0303
k252
100.
5249
185.
566
5.71
70.
077
-0.3
530.
112
0.87
Tabl
e6.
5:Ph
otom
etric
met
allic
ityof
132
RR
abst
ars
intil
eLM
C8_
3fo
rwhi
chD
m<
5(C
olum
n1:
ERO
S-2
iden
tifica
tion
ofth
est
ar;C
ol-
umn
2:Pe
riod
ofth
est
arfr
omth
eER
OS-
2ca
talo
gue;
Col
umn
3:Fo
urie
rpa
ram
eter
φ31
ofth
esi
neFo
urie
rde
com
posi
tion
oflig
htcu
rves
inth
eVJ
pass
band
;Col
umn
4:Fo
urie
rpar
amet
erφ31
ofth
esi
neFo
urie
rde-
com
posi
tion
inth
eK
eple
rmag
nitu
desd
eriv
edw
ithEq
.1.1
2;C
olum
n5:
Erro
rofφ
31
inth
eK
eple
rmag
nitu
des;
Col
umn
6:M
etal
licity
onth
eC
09m
etal
licity
scal
ede
rived
with
Eq.1
.11;
Col
umn
7:Er
roro
fm
etal
licity
onth
eC
09m
etal
licity
scal
e;C
olum
n8:
Dm
valu
e).
129
6.4. METALLICITY OF THE RR LYRAE STARS IN TILE LMC 8_3
ERO
S-2
idPe
riod
φc 31
errφ
c 31
[Fe/H] C
09
err[Fe/H] C
09
(day
s)(d
ex)
(dex
)lm
0300
l146
470.
4336
22.
517
0.24
9-2
.76
0.13
1lm
0293
n310
800.
4365
31.
189
0.17
-2.4
830.
148
lm04
34l7
912
0.45
5709
0.90
10.
264
-2.3
740.
194
lm03
03m
2298
90.
4273
244.
208
0.20
4-2
.191
0.18
4lm
0300
l889
00.
3487
012.
535
0.14
9-2
.106
0.13
5lm
0425
n137
530.
3242
851.
817
0.20
4-1
.984
0.13
1lm
0305
m62
940.
3666
833.
413
0.21
6-1
.979
0.17
1lm
0312
l151
930.
3317
82.
557
0.22
4-1
.939
0.14
7lm
0425
l648
10.
3449
973.
021
0.28
1-1
.92
0.18
lm03
01m
1584
70.
3300
772.
696
0.20
6-1
.881
0.14
9lm
0425
n186
800.
3103
661.
197
0.28
5-1
.842
0.13
3lm
0434
n143
100.
2965
731.
887
0.25
-1.7
30.
137
lm02
91n2
5551
0.30
8322
2.48
60.
249
-1.7
20.
156
lm04
35m
9109
0.29
5152
2.01
60.
291
-1.6
970.
145
lm03
02n4
858
0.29
2002
2.21
20.
27-1
.623
0.15
2lm
0303
n315
830.
3141
83.
146
0.19
8-1
.517
0.16
9lm
0291
l119
400.
3033
182.
985
0.16
7-1
.467
0.15
6lm
0300
m68
080.
3291
393.
856
0.27
4-1
.267
0.24
7lm
0424
m19
442
0.30
4605
-0.5
60.
284
-1.0
510.
232
lm04
37m
2212
60.
2806
844.
919
0.27
70.
490.
368
Tabl
e6.
6:Ph
otom
etric
met
allic
ityof
20R
Rc
star
sin
tile
LMC
8_3
(Col
-um
n1:
ERO
S-2
iden
tifica
tion
ofth
est
ar;C
olum
n2:
Perio
d;C
olum
n3:
Four
ierp
aram
eter
φc 31
ofth
eco
sine
Four
ierd
ecom
posi
tion;
Col
umn
4:Er
roro
fφc 31;C
olum
n5:
Met
allic
ityin
the
C09
met
allic
itysc
ale
deriv
edw
ithEq
.1.
13;
Col
umn
6:Er
ror
ofm
etal
licity
inth
eC
09m
etal
licity
scal
e).
130
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3
6.5 Ks magnitude of the RR Lyrae stars in tile LMC 8_3
We built the Ks-band light curves of the 251 confirmed RR Lyrae stars in tile LMC 8_3,
using the Ks aperture photometry of the VMC data provided by the VSA internal release
of 5 August 2013. In order to derive the mean ⟨Ks⟩ magnitudes we fitted the light curves
of the RR Lyrae stars with the templates from Jones et al. (1996). This method requires a
precise knowledge of the ephemerides and amplitudes in the VJ band, for which we used
the values derived in our analysis of the EROS-2 light curves with GRATIS (see Table 6.2).
We also corrected for any phase shift between templates and data points.
To correct the mean magnitudes for reddening we adopted the mean value of the ex-
tinction in the V band for tile LMC 8_3 derived by Rubele et al. (2012) and applied the
relation AK/AV = 0.114 from Cardelli et al. (1989). The absorption the K band is then
AK = 0.038± 0.006 mag. Dereddened mean Ks magnitudes of the 251 RR Lyrae stars are
presented in Table 6.7.
131
6.5. KS MAGNITUDE OF THE RR LYRAE STARS IN TILE LMC 8_3
VM
Cid
ERO
S-2
idR
AD
ECR
Rty
pePe
riod
Ks,0
σK
s,0
(deg
)(d
eg)
(day
s)(m
ag)
(mag
)V
MC
J050
223.
44-6
5293
6.47
lm04
23l2
0069
75.5
9747
-65.
4933
9c
0.29
1086
18.4
060.
019
VM
CJ0
5001
7.74
-652
810.
85lm
0422
n169
9375
.073
83-6
5.46
963
c0.
3607
2618
.06
0.02
1V
MC
J050
123.
87-6
5300
7.76
lm04
23l1
7670
75.3
4933
-65.
5021
c0.
3375
9418
.201
0.02
3V
MC
J050
917.
20-6
5362
8.82
lm04
35m
9109
77.3
2164
-65.
6079
8c
0.29
5152
18.2
450.
023
VM
CJ0
5095
7.20
-653
705.
78lm
0435
m10
888
77.4
8819
-65.
6182
4c
0.28
9555
18.5
060.
029
VM
CJ0
5034
6.01
-653
343.
72lm
0425
m33
5575
.941
57-6
5.56
209
c0.
3588
6418
.207
0.02
3V
MC
J050
921.
39-6
5381
4.14
lm04
35m
1353
377
.339
03-6
5.63
724
c0.
3542
7418
.118
0.02
1V
MC
J051
015.
38-6
5400
0.96
lm04
35m
1828
077
.563
86-6
5.66
69c
0.34
5305
18.1
490.
021
VM
CJ0
5021
3.12
-653
430.
92lm
0425
k462
575
.554
53-6
5.57
518
c0.
3355
3718
.285
0.02
4V
MC
J050
311.
74-6
5355
0.23
lm04
25m
8144
75.7
9879
-65.
5972
5c
0.37
6376
18.1
240.
021
VM
CJ0
5013
5.53
-653
609.
22lm
0425
k820
775
.397
93-6
5.60
249
c0.
3821
1117
.834
0.01
7V
MC
J050
153.
40-6
5363
5.13
lm04
25k9
319
75.4
7239
-65.
6096
7c
0.31
9697
18.4
180.
027
VM
CJ0
5055
4.38
-654
202.
05lm
0434
m22
078
76.4
7651
-65.
7005
c0.
3721
5718
.17
0.02
1V
MC
J051
059.
57-6
5460
0.06
lm04
44l9
270
77.7
4804
-65.
7666
5c
0.37
4023
18.0
920.
02V
MC
J050
025.
52-6
5404
1.56
lm04
24m
1944
275
.106
27-6
5.67
82c
0.30
4605
18.4
140.
028
VM
CJ0
5054
5.16
-654
541.
03lm
0434
l791
276
.438
11-6
5.76
134
c0.
4557
0918
.421
0.02
7V
MC
J050
649.
59-6
5481
1.93
lm04
34n1
4310
76.7
0655
-65.
8032
7c
0.29
6573
18.4
30.
027
VM
CJ0
5011
4.82
-654
437.
48lm
0425
l648
175
.311
67-6
5.74
371
c0.
3449
9718
.149
0.02
2V
MC
J050
214.
04-6
5461
8.69
lm04
25l1
0656
75.5
5837
-65.
7718
1c
0.34
5737
18.2
510.
024
VM
CJ0
5025
7.13
-654
724.
98lm
0425
n137
5375
.738
-65.
7902
c0.
3242
8518
.365
0.02
6V
MC
J050
308.
15-6
5480
6.87
lm04
25n1
5519
75.7
8383
-65.
8018
4c
0.30
7507
18.3
190.
024
VM
CJ0
5034
2.51
-654
918.
48lm
0425
n186
8075
.927
-65.
8217
3c
0.31
0366
18.3
960.
026
VM
CJ0
5052
0.41
-655
122.
21lm
0434
l201
6876
.335
03-6
5.85
612
c0.
3534
5218
.322
0.02
5V
MC
J050
532.
60-6
5530
6.83
lm04
34l1
9810
76.3
8578
-65.
8851
9c
0.37
9506
17.5
680.
013
VM
CJ0
5020
0.28
-655
027.
73lm
0425
l205
1375
.501
09-6
5.84
096
c0.
2899
7318
.142
0.02
2V
MC
J050
456.
47-6
5524
1.83
lm04
34l2
3190
76.2
3528
-65.
8782
7c
0.32
2595
18.2
410.
024
VM
CJ0
5015
1.53
-655
203.
97lm
0425
l243
8975
.464
57-6
5.86
768
c0.
2813
8818
.327
0.02
4V
MC
J050
654.
27-6
5575
7.68
lm04
36m
8308
76.7
2609
-65.
9659
9c
0.33
1619
18.2
530.
023
VM
CJ0
5063
7.75
-655
947.
19lm
0436
m11
977
76.6
5728
-65.
9963
7c
0.38
2103
18.1
920.
022
VM
CJ0
5093
5.73
-660
411.
25lm
0437
m22
126
77.3
9874
-66.
0697
3c
0.28
0684
18.5
330.
03
132
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3V
MC
J050
110.
80-6
5590
4.57
lm04
27k1
0785
75.2
9491
-65.
9845
4c
0.35
837
18.0
990.
02V
MC
J050
342.
45-6
6022
6.85
lm04
27m
1933
275
.926
83-6
6.04
073
c0.
2865
4618
.347
0.02
5V
MC
J050
620.
52-6
6071
8.45
lm04
36n1
0024
76.5
8557
-66.
1216
9c
0.34
6597
18.4
010.
026
VM
CJ0
5020
7.24
-660
502.
83lm
0427
l450
775
.530
04-6
6.08
408
c0.
3873
5917
.919
0.01
7V
MC
J050
639.
22-6
6091
1.85
lm04
36n1
4285
76.6
6342
-66.
1531
5c
0.34
985
18.1
810.
022
VM
CJ0
5052
9.49
-661
014.
55lm
0436
l159
9376
.372
96-6
6.17
058
c0.
3438
2118
.274
0.02
4V
MC
J050
453.
54-6
6105
4.45
lm04
36l1
7456
76.2
2323
-66.
1816
9c
0.27
7319
18.5
140.
029
VM
CJ0
5015
7.09
-661
115.
87lm
0427
l173
4675
.487
75-6
6.18
771
c0.
3809
2218
.116
0.02
VM
CJ0
5102
6.70
-661
840.
19lm
0310
k930
077
.611
15-6
6.31
121
c0.
3702
8818
.083
0.02
VM
CJ0
5040
1.37
-661
719.
33lm
0300
m68
0876
.005
54-6
6.28
864
c0.
3291
3918
.335
0.02
4V
MC
J050
829.
34-6
6202
7.95
lm03
01m
1584
777
.122
13-6
6.34
112
c0.
3300
7718
.137
0.02
1V
MC
J050
733.
67-6
6264
5.94
lm03
01n7
929
76.8
9016
-66.
4461
c0.
3142
7118
.272
0.02
4V
MC
J051
040.
41-6
6294
0.91
lm03
10n1
1585
77.6
6864
-66.
4946
6c
0.34
0596
18.2
940.
053
VM
CJ0
5091
8.46
-662
916.
88lm
0310
l124
4077
.326
74-6
6.48
791
c0.
3487
8318
.139
0.02
1V
MC
J050
808.
19-6
6295
9.33
lm03
01n1
6576
77.0
3389
-66.
4998
2c
0.23
6645
17.8
10.
016
VM
CJ0
5031
7.90
-662
638.
48lm
0300
l675
375
.824
56-6
6.44
405
c0.
3409
3618
.017
0.01
9V
MC
J050
000.
27-6
6241
2.25
lm02
91k2
4862
75.0
0092
-66.
4034
2c
0.29
3334
18.5
880.
031
VM
CJ0
5031
6.54
-662
733.
42lm
0300
l889
075
.818
9-6
6.45
933
c0.
3487
0117
.786
0.01
6V
MC
J050
313.
07-6
6301
3.26
lm03
00l1
5247
75.8
0446
-66.
5037
c0.
2709
218
.628
0.03
1V
MC
J045
936.
35-6
6272
7.30
lm02
91l9
716
74.9
0131
-66.
4575
7c
0.35
4199
18.2
990.
024
VM
CJ0
5013
9.58
-662
924.
71lm
0291
n154
1275
.414
71-6
6.49
017
c0.
3282
2318
.239
0.02
2V
MC
J045
935.
83-6
6281
8.01
lm02
91l1
1940
74.8
9917
-66.
4716
6c
0.30
3318
18.3
780.
026
VM
CJ0
5042
9.77
-663
352.
58lm
0300
n249
0476
.123
96-6
6.56
46c
0.37
6841
17.9
290.
018
VM
CJ0
5002
8.40
-663
320.
76lm
0291
n255
5175
.118
17-6
6.55
566
c0.
3083
2218
.151
0.02
1V
MC
J050
747.
88-6
6393
7.12
lm03
03m
1077
376
.949
34-6
6.66
027
c0.
3449
4218
.216
0.02
3V
MC
J050
211.
22-6
6353
4.89
lm03
00l1
4647
75.5
4689
-66.
5929
2c
0.43
362
17.8
070.
017
VM
CJ0
4582
5.50
-663
236.
72lm
0291
l233
5974
.606
27-6
6.54
347
c0.
3580
9318
.234
0.02
4V
MC
J050
257.
12-6
6375
3.02
lm03
02k3
782
75.7
3802
-66.
6313
3c
0.35
2431
18.0
230.
019
VM
CJ0
5030
1.63
-663
833.
15lm
0302
k502
275
.756
83-6
6.64
249
c0.
4042
0218
.191
0.02
2V
MC
J050
837.
23-6
6434
5.17
lm03
03m
2250
477
.154
98-6
6.72
917
c0.
3234
0418
.471
0.02
8V
MC
J050
807.
83-6
6435
9.20
lm03
03m
2298
977
.032
43-6
6.73
305
c0.
4273
2417
.811
0.01
7V
MC
J050
018.
38-6
6394
0.46
lm02
93m
1098
875
.076
49-6
6.66
119
c0.
3661
2118
.212
0.02
3V
MC
J050
138.
64-6
6423
9.19
lm02
93m
1980
375
.410
86-6
6.71
085
c0.
3385
3818
.358
0.02
6
133
6.5. KS MAGNITUDE OF THE RR LYRAE STARS IN TILE LMC 8_3V
MC
J050
646.
44-6
6480
2.84
lm03
03l8
655
76.6
9337
-66.
8007
c0.
3391
2517
.994
0.02
VM
CJ0
5043
3.03
-664
704.
30lm
0302
n485
876
.137
49-6
6.78
444
c0.
2920
0218
.357
0.02
5V
MC
J050
942.
23-6
6512
6.02
lm03
12l1
5193
77.4
2594
-66.
8571
6c
0.33
178
18.3
860.
027
VM
CJ0
5082
4.66
-665
044.
50lm
0303
n168
4177
.102
76-6
6.84
558
c0.
3274
9318
.178
0.03
6V
MC
J050
836.
01-6
6555
0.04
lm03
03n3
1583
77.1
4986
-66.
9305
c0.
3141
818
.412
0.02
7V
MC
J050
238.
91-6
6514
6.42
lm03
02l1
6395
75.6
6204
-66.
8628
1c
0.34
4601
18.1
640.
022
VM
CJ0
4591
0.51
-665
138.
98lm
0293
l184
2174
.793
58-6
6.86
072
c0.
2787
5918
.33
0.02
5V
MC
J050
735.
59-6
6581
1.53
lm03
05m
3332
76.8
982
-66.
9698
1c
0.24
9311
18.1
410.
022
VM
CJ0
5075
3.60
-665
915.
19lm
0305
m62
9476
.973
24-6
6.98
749
c0.
3666
8318
.028
0.02
VM
CJ0
5003
7.51
-665
555.
71lm
0293
n310
8075
.156
16-6
6.93
208
c0.
4365
318
.527
0.02
4V
MC
J050
347.
33-6
6581
9.01
lm03
04m
2952
75.9
472
-66.
9718
5c
0.31
1944
18.3
040.
018
VM
CJ0
5101
6.85
-653
532.
02lm
0435
m70
5877
.570
13-6
5.59
222
ab0.
5974
8617
.908
0.01
3V
MC
J050
302.
40-6
5312
0.51
lm04
23n2
6224
75.7
598
-65.
5222
9ab
0.55
9366
18.1
740.
022
VM
CJ0
5093
1.00
-653
632.
31lm
0435
m93
3477
.379
13-6
5.60
896
ab0.
5508
517
.895
0.01
7V
MC
J050
136.
39-6
5310
9.44
lm04
23l1
1740
75.4
0143
-65.
5192
5ab
0.55
4337
17.9
590.
021
VM
CJ0
5021
1.10
-653
150.
27lm
0423
l792
675
.546
1-6
5.53
056
ab0.
5618
1818
.082
0.02
1V
MC
J050
638.
07-6
5352
0.91
lm04
34m
6139
76.6
5853
-65.
5890
9ab
0.54
0358
18.0
590.
02V
MC
J050
326.
18-6
5341
0.97
lm04
25m
4288
75.8
5896
-65.
5696
7ab
0.59
7504
17.9
730.
019
VM
CJ0
5082
4.37
-653
759.
21lm
0435
k123
0977
.101
44-6
5.63
307
ab0.
6089
9217
.965
0.01
9V
MC
J050
752.
49-6
5375
4.29
lm04
35k1
2002
76.9
6857
-65.
6316
7ab
0.61
8774
18.1
170.
021
VM
CJ0
5103
8.81
-653
957.
41lm
0435
m18
273
77.6
6155
-65.
6659
2ab
0.63
1476
17.7
560.
015
VM
CJ0
5043
5.44
-653
606.
07lm
0434
k730
276
.147
62-6
5.60
166
ab0.
6101
9217
.978
0.01
8V
MC
J050
534.
00-6
5365
1.80
lm04
34k9
008
76.3
9164
-65.
6143
7ab
0.56
7635
17.7
70.
016
VM
CJ0
5094
7.94
-653
953.
14lm
0435
m17
793
77.4
496
-65.
6647
2ab
0.52
4956
18.0
710.
021
VM
CJ0
5085
4.55
-654
006.
09lm
0435
k175
8977
.227
23-6
5.66
834
ab0.
6126
3518
.045
0.02
VM
CJ0
5074
2.69
-653
928.
17lm
0435
k158
1676
.927
75-6
5.65
774
ab0.
6387
9417
.69
0.01
4V
MC
J051
003.
09-6
5420
8.05
lm04
35m
2356
377
.512
67-6
5.70
218
ab0.
5250
4817
.972
0.01
8V
MC
J050
821.
58-6
5411
0.34
lm04
35k2
0062
77.0
8979
-65.
6861
6ab
0.51
4125
18.1
950.
022
VM
CJ0
5025
2.15
-653
746.
20lm
0425
m12
624
75.7
172
-65.
6294
5ab
0.54
7065
17.9
670.
019
VM
CJ0
5061
4.54
-654
101.
80lm
0434
m19
648
76.5
6045
-65.
6837
6ab
0.62
2604
17.8
380.
017
VM
CJ0
5070
0.34
-654
142.
90lm
0434
m21
424
76.7
513
-65.
6951
9ab
0.57
382
18.0
690.
02V
MC
J050
119.
43-6
5373
4.91
lm04
25k1
1500
75.3
3082
-65.
6262
7ab
0.54
0233
17.8
580.
017
VM
CJ0
5074
1.32
-654
407.
60lm
0435
l524
776
.922
13-6
5.73
542
ab0.
5718
2317
.953
0.01
9
134
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3V
MC
J050
535.
32-6
5435
5.85
lm04
34k2
2095
76.3
971
-65.
7321
5ab
0.53
9682
18.0
880.
02V
MC
J050
924.
06-6
5463
5.78
lm04
35n1
1321
77.3
5012
-65.
7765
6ab
0.58
7183
17.4
910.
013
VM
CJ0
5074
0.45
-654
601.
59lm
0435
l985
876
.918
47-6
5.76
707
ab0.
6094
6218
.026
0.02
VM
CJ0
5065
9.03
-654
542.
60lm
0434
n841
376
.745
85-6
5.76
182
ab0.
6708
7117
.786
0.01
6V
MC
J050
945.
64-6
5473
8.28
lm04
35n1
3913
77.4
4001
-65.
7939
3ab
0.59
7578
18.1
40.
021
VM
CJ0
5003
1.62
-654
206.
12lm
0424
m22
887
75.1
3167
-65.
7016
4ab
0.39
8125
18.6
320.
034
VM
CJ0
5065
4.39
-654
756.
81lm
0434
n137
0476
.726
55-6
5.79
908
ab0.
5711
6618
.165
0.02
2V
MC
J050
028.
44-6
5440
9.42
lm04
24n5
227
75.1
1837
-65.
7359
1ab
0.61
9983
17.3
40.
012
VM
CJ0
5010
3.78
-654
614.
63lm
0425
l102
4775
.265
73-6
5.77
068
ab0.
6074
6117
.90.
018
VM
CJ0
5110
2.96
-655
339.
53lm
0444
l200
3377
.761
82-6
5.89
427
ab0.
5750
9217
.793
0.01
6V
MC
J050
523.
30-6
5495
7.92
lm04
34l1
7031
76.3
4705
-65.
8327
1ab
0.58
2937
17.9
790.
019
VM
CJ0
5055
6.87
-655
134.
75lm
0434
n222
9276
.486
91-6
5.85
96ab
0.68
9693
17.8
860.
017
VM
CJ0
5011
9.83
-654
808.
40lm
0425
l148
5275
.332
57-6
5.80
227
ab0.
5360
5418
.191
0.02
2V
MC
J050
520.
68-6
5512
9.43
lm04
34l2
0435
76.3
3615
-65.
8581
1ab
0.48
8809
518
.024
0.01
9V
MC
J045
936.
81-6
5472
7.16
lm04
24n1
2543
74.9
0326
-65.
7908
3ab
0.63
5316
17.8
210.
017
VM
CJ0
5060
3.24
-655
333.
47lm
0434
n173
8376
.513
44-6
5.89
259
ab0.
7241
5217
.55
0.01
3V
MC
J050
145.
38-6
5504
2.88
lm04
25l2
1048
75.4
3903
-65.
8452
5ab
0.61
5813
17.5
760.
014
VM
CJ0
5041
0.43
-655
245.
19lm
0425
n232
5076
.043
45-6
5.87
922
ab0.
5251
9118
.056
0.01
9V
MC
J051
007.
73-6
5580
4.30
lm04
37m
9713
77.5
3209
-65.
9678
2ab
0.62
0011
17.8
060.
016
VM
CJ0
5075
1.59
-655
751.
27lm
0437
k868
176
.964
96-6
5.96
417
ab0.
5890
5517
.949
0.01
8V
MC
J050
913.
23-6
5595
4.52
lm04
37k1
3906
77.3
0504
-65.
9985
1ab
0.59
4332
17.9
380.
018
VM
CJ0
5035
7.69
-655
643.
65lm
0427
m63
3875
.990
25-6
5.94
538
ab0.
7135
0117
.778
0.01
6V
MC
J050
755.
57-6
6003
8.96
lm04
37k1
5328
76.9
8154
-66.
0106
5ab
0.58
4568
17.9
920.
019
VM
CJ0
5080
0.42
-660
050.
63lm
0437
k157
7277
.001
7-6
6.01
396
ab0.
4883
2218
.153
0.02
1V
MC
J051
048.
50-6
6024
2.86
lm04
37m
2044
477
.702
08-6
6.04
521
ab0.
5114
2318
.349
0.02
5V
MC
J051
058.
57-6
6031
3.36
lm04
46k2
0706
77.7
4377
-66.
0537
2ab
0.54
3569
18.0
760.
019
VM
CJ0
5102
5.89
-660
258.
51lm
0437
m20
883
77.6
079
-66.
0495
3ab
0.58
0287
18.1
880.
022
VM
CJ0
5102
3.01
-660
425.
80lm
0437
m17
477
77.5
9584
-66.
0738
2ab
0.53
6134
18.0
540.
02V
MC
J050
615.
88-6
6021
5.95
lm04
36m
1701
176
.566
19-6
6.03
765
ab0.
6459
9617
.914
0.01
7V
MC
J050
334.
48-6
6002
9.23
lm04
27m
1475
375
.893
61-6
6.00
8ab
0.54
401
17.9
530.
018
VM
CJ0
5080
3.01
-660
347.
82lm
0437
k226
5477
.012
47-6
6.06
322
ab0.
4913
1218
.203
0.02
2V
MC
J050
439.
43-6
6012
0.57
lm04
36k1
5855
76.1
6415
-66.
0223
3ab
0.61
4185
17.8
380.
016
VM
CJ0
5105
6.74
-660
648.
08lm
0437
n845
577
.736
25-6
6.11
333
ab0.
5749
9918
.042
0.01
9
135
6.5. KS MAGNITUDE OF THE RR LYRAE STARS IN TILE LMC 8_3V
MC
J050
357.
85-6
6025
4.64
lm04
27m
2046
675
.990
99-6
6.04
834
ab0.
6166
2617
.914
0.01
7V
MC
J050
716.
92-6
6062
6.56
lm04
36n8
236
76.8
2037
-66.
1073
4ab
0.65
0192
17.6
020.
013
VM
CJ0
5105
2.01
-660
955.
34lm
0437
n147
9477
.716
65-6
6.16
543
ab0.
5447
6917
.883
0.01
7V
MC
J050
701.
01-6
6074
8.02
lm04
36n1
1172
76.7
5415
-66.
1299
1ab
0.43
1733
18.3
850.
026
VM
CJ0
5095
8.87
-661
010.
55lm
0437
n150
4977
.495
07-6
6.16
951
ab0.
5710
1417
.991
0.01
9V
MC
J050
124.
80-6
6042
9.92
lm04
27k1
7452
75.3
5321
-66.
0749
4ab
0.67
5498
17.8
470.
017
VM
CJ0
5030
9.18
-660
645.
01lm
0427
n774
175
.788
08-6
6.11
239
ab0.
4828
418
.191
0.02
2V
MC
J050
815.
71-6
6104
6.07
lm04
37l1
5735
77.0
6524
-66.
1793
4ab
0.62
2553
17.9
120.
018
VM
CJ0
4592
4.15
-660
414.
72lm
0426
m24
414
74.8
5054
-66.
0706
4ab
0.60
6869
18.0
210.
019
VM
CJ0
5004
2.40
-660
654.
21lm
0426
n966
675
.176
63-6
6.11
497
ab0.
6876
2517
.859
0.01
7V
MC
J050
704.
87-6
6120
4.64
lm04
36n2
0628
76.7
7019
-66.
2012
ab0.
4931
0718
.032
0.01
9V
MC
J050
023.
70-6
6075
7.58
lm04
26n1
2018
75.0
9864
-66.
1325
9ab
0.52
946
18.1
770.
022
VM
CJ0
5013
1.48
-660
910.
93lm
0427
l124
6275
.381
09-6
6.15
291
ab0.
5711
9417
.851
0.01
7V
MC
J050
537.
17-6
6121
9.31
lm04
36l2
0450
76.4
0491
-66.
2052
7ab
0.51
1395
17.8
430.
016
VM
CJ0
5023
3.99
-661
150.
13lm
0427
l188
5675
.641
63-6
6.19
734
ab0.
5626
9818
.059
0.01
9V
MC
J050
901.
51-6
6193
1.25
lm03
10k1
1253
77.2
5582
-66.
3252
3ab
0.53
7149
17.9
370.
018
VM
CJ0
5075
1.68
-662
025.
78lm
0301
m15
584
76.9
652
-66.
3405
6ab
0.54
134
18.2
580.
023
VM
CJ0
5080
4.65
-662
029.
19lm
0301
m15
788
77.0
1923
-66.
3415
4ab
0.71
0038
17.6
620.
016
VM
CJ0
5040
0.65
-661
836.
81lm
0300
m99
3576
.002
53-6
6.31
022
ab0.
4851
2718
.118
0.02
VM
CJ0
5043
5.36
-661
917.
95lm
0300
m11
600
76.1
4728
-66.
3216
6ab
0.57
0995
17.7
650.
015
VM
CJ0
5034
1.33
-661
926.
07lm
0300
m11
839
75.9
2208
-66.
3239
2ab
0.55
9733
17.9
580.
018
VM
CJ0
5084
5.88
-662
308.
37lm
0301
m22
780
77.1
9099
-66.
3856
3ab
0.53
5459
18.1
040.
027
VM
CJ0
5101
3.61
-662
410.
19lm
0310
k180
1077
.556
57-6
6.40
282
ab0.
5902
9918
.048
0.02
VM
CJ0
5011
1.42
-661
743.
68lm
0291
m87
1075
.297
38-6
6.29
542
ab0.
5117
4518
.336
0.02
4V
MC
J050
530.
59-6
6213
7.18
lm03
01k1
7554
76.3
7739
-66.
3603
1ab
0.53
5567
18.2
230.
023
VM
CJ0
5030
7.36
-661
947.
80lm
0300
k121
8475
.780
71-6
6.32
998
ab0.
5248
1318
.068
0.02
VM
CJ0
5094
2.68
-662
434.
51lm
0310
k157
3877
.427
75-6
6.40
958
ab0.
6085
3417
.988
0.01
8V
MC
J050
140.
14-6
6185
6.66
lm02
91m
1193
375
.417
18-6
6.31
573
ab0.
5581
0217
.893
0.01
7V
MC
J050
204.
20-6
6194
0.86
lm03
00k1
1860
75.5
1738
-66.
3279
6ab
0.64
3757
17.7
920.
016
VM
CJ0
5040
5.00
-662
135.
69lm
0300
m17
178
76.0
2068
-66.
3599
6ab
0.51
8967
17.9
90.
018
VM
CJ0
5023
8.30
-662
042.
97lm
0300
k143
3575
.659
71-6
6.34
538
ab0.
5661
5717
.941
0.01
8V
MC
J050
330.
54-6
6213
7.49
lm03
00k1
6563
75.8
7714
-66.
3604
4ab
0.59
2704
18.0
80.
02V
MC
J045
917.
82-6
6182
4.09
lm02
91k1
0047
74.8
2401
-66.
3066
7ab
0.58
5024
18.1
210.
021
136
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3V
MC
J045
907.
17-6
6183
8.18
lm02
91k1
0561
74.7
7965
-66.
3105
8ab
0.55
7117
.909
0.01
8V
MC
J050
518.
74-6
6235
9.17
lm03
00m
2326
676
.327
89-6
6.39
973
ab0.
5488
6817
.899
0.01
8V
MC
J050
259.
67-6
6220
4.90
lm03
00k1
7665
75.7
4862
-66.
3681
2ab
0.56
8997
17.7
20.
016
VM
CJ0
5050
1.62
-662
446.
46lm
0300
m25
109
76.2
5662
-66.
4128
8ab
0.65
2891
17.6
460.
014
VM
CJ0
5035
1.73
-662
414.
02lm
0300
m23
701
75.9
6552
-66.
4039
2ab
0.54
6102
18.0
750.
019
VM
CJ0
5050
6.73
-662
545.
68lm
0300
m19
324
76.2
7787
-66.
4292
7ab
0.52
5312
18.1
110.
02V
MC
J050
917.
87-6
6301
0.23
lm03
10l1
4484
77.3
2418
-66.
5028
ab0.
6616
5217
.239
0.01
1V
MC
J050
744.
32-6
6292
2.45
lm03
01n1
4847
76.9
3447
-66.
4895
8ab
0.54
9535
18.1
160.
02V
MC
J050
616.
88-6
6282
6.74
lm03
01l1
1630
76.5
7024
-66.
4740
9ab
0.56
8156
18.0
280.
019
VM
CJ0
5082
6.52
-663
002.
34lm
0301
n168
1477
.110
29-6
6.50
065
ab0.
5282
6218
.126
0.02
3V
MC
J050
731.
84-6
6292
6.36
lm03
01n1
4943
76.8
8253
-66.
4906
9ab
0.64
5196
17.8
850.
017
VM
CJ0
5094
5.32
-663
103.
00lm
0310
l163
3477
.438
82-6
6.51
749
ab0.
6577
8817
.804
0.01
6V
MC
J050
948.
61-6
6315
8.65
lm03
10l1
8147
77.4
5244
-66.
5328
9ab
0.59
0217
17.8
460.
017
VM
CJ0
5100
5.62
-663
221.
50lm
0310
l189
1177
.523
38-6
6.53
928
ab0.
7484
3117
.728
0.01
5V
MC
J050
440.
29-6
6285
1.85
lm03
00n1
2088
76.1
6779
-66.
4811
1ab
0.67
2356
17.9
720.
018
VM
CJ0
5005
0.21
-662
554.
35lm
0291
n604
075
.209
07-6
6.43
175
ab0.
5276
1918
.092
0.02
VM
CJ0
5042
8.64
-662
852.
88lm
0300
n121
0976
.119
25-6
6.48
14ab
0.68
3459
17.7
870.
015
VM
CJ0
5061
3.56
-663
018.
70lm
0301
l164
8776
.556
35-6
6.50
519
ab0.
7381
4317
.412
0.01
3V
MC
J050
457.
37-6
6293
5.19
lm03
00n1
3961
76.2
3893
-66.
4931
4ab
0.62
3548
17.8
0.01
6V
MC
J050
730.
28-6
6315
9.48
lm03
01n2
1605
76.8
7595
-66.
5331
9ab
0.53
2545
18.1
250.
021
VM
CJ0
5045
7.89
-663
156.
79lm
0300
n199
2776
.241
13-6
6.53
242
ab0.
6371
2918
.012
0.01
9V
MC
J050
546.
52-6
6324
3.58
lm03
01l2
2786
76.4
4374
-66.
5454
1ab
0.64
8027
17.8
920.
017
VM
CJ0
5062
3.56
-663
312.
53lm
0301
l242
5576
.597
98-6
6.55
346
ab0.
5105
817
.799
0.01
5V
MC
J050
519.
02-6
6322
2.23
lm03
00n2
1091
76.3
2909
-66.
5394
6ab
0.56
746
18.0
640.
019
VM
CJ0
5060
2.75
-663
334.
37lm
0301
l251
4076
.511
23-6
6.55
949
ab0.
6631
835
17.7
550.
016
VM
CJ0
4584
6.28
-662
755.
50lm
0291
l107
7574
.692
8-6
6.46
539
ab0.
5709
9218
.345
0.02
5V
MC
J050
140.
25-6
6311
2.05
lm02
91n2
0101
75.4
1745
-66.
5200
1ab
0.51
7254
17.9
750.
019
VM
CJ0
5024
4.52
-663
247.
81lm
0300
l207
3975
.685
5-6
6.54
657
ab0.
5890
6617
.789
0.01
6V
MC
J050
931.
40-6
6374
8.14
lm03
12k4
503
77.3
8073
-66.
6299
6ab
0.61
3847
18.0
580.
02V
MC
J050
015.
23-6
6312
1.94
lm02
91n2
0061
75.0
6329
-66.
5227
2ab
0.52
9756
18.2
660.
023
VM
CJ0
5083
3.42
-663
737.
55lm
0303
m56
5177
.139
18-6
6.62
705
ab0.
6925
4717
.883
0.01
7V
MC
J050
346.
69-6
6345
0.22
lm03
00n2
7286
75.9
4449
-66.
5805
7ab
0.56
6301
17.9
360.
017
VM
CJ0
5024
1.69
-663
447.
20lm
0300
l255
6675
.673
67-6
6.57
969
ab0.
6381
5517
.898
0.01
7
137
6.5. KS MAGNITUDE OF THE RR LYRAE STARS IN TILE LMC 8_3V
MC
J050
224.
70-6
6350
0.23
lm03
00l2
3462
75.6
0295
-66.
5833
ab0.
7443
1417
.637
0.01
4V
MC
J050
835.
85-6
6393
5.74
lm03
03m
1100
577
.149
24-6
6.65
987
ab0.
6437
717
.907
0.01
7V
MC
J050
302.
54-6
6354
0.49
lm03
00l1
3312
75.7
6052
-66.
5944
6ab
0.52
7452
18.0
670.
019
VM
CJ0
4584
0.37
-663
345.
71lm
0291
l265
4574
.668
19-6
6.56
263
ab0.
6694
875
17.7
240.
016
VM
CJ0
5075
6.07
-664
155.
19lm
0303
m17
152
76.9
835
-66.
6986
1ab
0.52
4201
17.9
990.
02V
MC
J050
816.
34-6
6420
7.26
lm03
03m
1781
277
.067
91-6
6.70
197
ab0.
5655
5618
.005
0.02
VM
CJ0
5080
3.26
-664
323.
35lm
0303
m21
245
77.0
134
-66.
7231
1ab
0.59
3551
17.8
650.
018
VM
CJ0
4592
3.84
-663
716.
72lm
0293
k392
874
.849
21-6
6.62
125
ab0.
4717
4218
.15
0.02
3V
MC
J050
934.
40-6
6461
2.11
lm03
12k2
1111
77.3
9336
-66.
7699
5ab
0.46
0618
.26
0.02
3V
MC
J050
648.
56-6
6444
5.67
lm03
03k2
5210
76.7
022
-66.
7459
6ab
0.52
4918
18.2
740.
023
VM
CJ0
5004
8.02
-664
050.
02lm
0293
m14
375
75.1
9999
-66.
6805
4ab
0.50
7995
17.9
690.
019
VM
CJ0
5033
6.11
-664
354.
24lm
0302
k135
3475
.900
35-6
6.73
166
ab0.
6208
817
.904
0.01
7V
MC
J050
044.
55-6
6414
5.65
lm02
93m
1700
075
.185
43-6
6.69
597
ab0.
5952
2418
.00.
018
VM
CJ0
5010
2.85
-664
226.
34lm
0293
m19
003
75.2
6169
-66.
7072
7ab
0.58
3546
18.1
670.
022
VM
CJ0
5051
4.22
-664
547.
98lm
0302
m22
487
76.3
0911
-66.
7632
9ab
0.52
0562
18.3
320.
025
VM
CJ0
5010
9.79
-664
239.
69lm
0293
m19
628
75.2
9061
-66.
7109
9ab
0.58
1141
17.9
70.
019
VM
CJ0
5022
9.32
-664
429.
58lm
0302
k147
9675
.622
13-6
6.74
15ab
0.55
9635
18.0
810.
02V
MC
J050
804.
51-6
6481
5.72
lm03
03n9
745
77.0
1868
-66.
8042
5ab
0.62
8757
17.8
680.
018
VM
CJ0
5074
4.26
-664
948.
84lm
0303
n139
7776
.934
26-6
6.83
012
ab0.
4995
561
18.2
360.
024
VM
CJ0
5073
9.78
-664
923.
56lm
0303
n127
9976
.915
6-6
6.82
31ab
0.58
1848
17.9
870.
019
VM
CJ0
5071
7.67
-665
020.
16lm
0303
n153
2276
.823
52-6
6.83
882
ab0.
5057
3318
.042
0.01
9V
MC
J050
733.
61-6
6503
5.07
lm03
03n1
6102
76.8
8992
-66.
8429
6ab
0.63
2428
17.8
920.
017
VM
CJ0
4593
0.50
-664
444.
46lm
0293
k252
2674
.876
83-6
6.74
562
ab0.
5864
7917
.936
0.01
8V
MC
J050
655.
64-6
6511
2.73
lm03
03l1
7671
76.7
3167
-66.
8534
4ab
0.56
0588
17.9
350.
018
VM
CJ0
4585
3.67
-664
552.
45lm
0293
k283
5274
.723
41-6
6.76
451
ab0.
4977
7917
.932
0.01
9V
MC
J050
345.
85-6
6495
5.21
lm03
02n1
2351
75.9
4097
-66.
8318
8ab
0.56
6134
18.1
720.
022
VM
CJ0
4595
1.56
-664
701.
22lm
0293
l525
274
.964
58-6
6.78
36ab
0.61
2908
18.0
090.
02V
MC
J050
325.
29-6
6501
5.18
lm03
02l1
2678
75.8
553
-66.
8375
ab0.
4249
4518
.401
0.02
6V
MC
J050
850.
74-6
6541
8.25
lm03
03n2
7302
77.2
1128
-66.
9050
1ab
0.58
6637
18.1
150.
021
VM
CJ0
5025
5.86
-665
022.
40lm
0302
l129
6075
.732
62-6
6.83
949
ab0.
5673
4117
.929
0.01
8V
MC
J050
622.
59-6
6544
2.03
lm03
03l2
7610
76.5
9394
-66.
9115
8ab
0.62
3747
17.8
870.
017
VM
CJ0
5054
9.03
-665
414.
23lm
0303
l261
4876
.454
07-6
6.90
387
ab0.
6206
4717
.87
0.01
7V
MC
J050
450.
69-6
6535
9.87
lm03
02n2
3523
76.2
1095
-66.
8998
7ab
0.49
7153
18.1
040.
021
138
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3V
MC
J045
913.
55-6
6493
9.41
lm02
93l1
2631
74.8
0625
-66.
8275
2ab
0.61
0866
18.0
160.
02V
MC
J050
040.
53-6
6512
8.79
lm02
93n1
8229
75.1
6869
-66.
8579
5ab
0.62
8127
17.8
820.
018
VM
CJ0
5012
6.66
-665
217.
05lm
0293
n208
7075
.360
86-6
6.87
147
ab0.
5781
917
.201
0.01
1V
MC
J050
330.
10-6
6542
9.42
lm03
02l2
3297
75.8
7528
-66.
9081
1ab
0.51
1473
18.2
250.
023
VM
CJ0
5072
6.13
-665
825.
30lm
0305
m38
8276
.858
77-6
6.97
363
ab0.
7104
8817
.861
0.01
7V
MC
J050
853.
74-6
6594
1.23
lm03
05m
7850
77.2
239
-66.
9947
4ab
0.71
3324
17.6
60.
015
VM
CJ0
5024
9.16
-665
550.
35lm
0302
l264
1775
.704
71-6
6.93
057
ab0.
5902
9618
.113
0.02
2V
MC
J050
148.
97-6
6554
0.11
lm02
93n3
0795
75.4
5401
-66.
9278
6ab
0.47
4027
17.9
850.
019
VM
CJ0
4591
8.98
-665
406.
56lm
0293
l255
0674
.828
89-6
6.90
17ab
0.65
7982
17.8
30.
017
VM
CJ0
5060
9.35
-665
915.
29lm
0305
k570
476
.538
8-6
6.98
748
ab0.
6216
18.0
380.
02V
MC
J045
802.
46-6
6535
8.25
lm02
92n2
2612
74.5
1012
-66.
8994
ab0.
6240
6818
.086
0.01
6V
MC
J050
223.
18-6
5292
1.68
lm04
23l2
1178
75.5
9644
-65.
4893
7ab
0.63
2125
17.4
050.
013
VM
CJ0
5044
4.73
-653
217.
60lm
0432
l124
2076
.186
33-6
5.53
826
ab0.
4784
3918
.277
0.03
3V
MC
J050
828.
76-6
5362
4.37
lm04
35k8
479
77.1
1971
-65.
6067
2d
0.36
516
18.0
230.
019
VM
CJ0
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2.67
-654
530.
93lm
0444
l813
877
.760
94-6
5.75
855
d0.
3549
2618
.081
0.02
VM
CJ0
5080
8.12
-662
858.
86lm
0301
n139
1177
.033
67-6
6.48
302
d0.
3571
8818
.141
0.02
2V
MC
J050
942.
36-6
6353
1.04
lm03
10l1
2653
77.4
2654
-66.
5918
8d
0.36
2102
18.2
030.
022
VM
CJ0
5053
3.89
-663
444.
89lm
0301
l269
3376
.391
15-6
6.57
905
d0.
3605
8417
.969
0.01
8V
MC
J050
040.
98-6
6332
7.65
lm02
91n2
5922
75.1
705
-66.
5576
d0.
3654
9318
.191
0.02
2V
MC
J050
713.
26-6
6441
4.20
lm03
03m
2339
176
.805
1-6
6.73
721
d0.
3855
118
.176
0.02
2V
MC
J050
655.
56-6
6442
7.31
lm03
03k2
4363
76.7
3134
-66.
7408
7d
0.39
1884
17.8
680.
017
VM
CJ0
4594
8.97
-664
636.
55lm
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k307
6474
.953
75-6
6.77
676
d0.
3537
418
.457
0.02
8V
MC
J050
148.
56-6
6495
4.79
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93n1
4230
75.4
5233
-66.
8319
7d
0.36
2897
18.0
770.
02Ta
ble
6.7:
Prop
ertie
sof
the
RR
Lyra
est
ars
intil
eLM
C8_
3(C
olum
n1:
VM
Cid
entifi
catio
nof
the
star
;Col
umn
2:ER
OS-
2id
entifi
catio
nof
the
star
;Col
umn
3:R
ight
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nsio
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OS-
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4:D
eclin
atio
nfr
omth
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OS-
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Col
umn
5:R
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rae
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;Col
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n6:
Perio
dfr
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S-2
cata
logu
e;C
olum
n7:
Der
edde
ned
mea
nm
agni
tude
inth
eK
spa
ssba
nd;C
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Erro
rof
the
dere
dden
edK
s
mea
nm
agni
tude
s).
139
6.6. DISTANCE TO THE TILE LMC 8_3 FROM RR LYRAE STARS
6.6 Distance to the tile LMC 8_3 from RR Lyrae stars
In Chapter 5 we derived a new PLKsZ relation based on a sample of the 71 RR Lyrae stars
in tile LMC 5_5. We can apply the new relation, as well as other PLKsZ relations in the
literature, to estimate the distance to each VMC tile, separately. This will, in turn, allow us
to study the structure of the LMC.
In this section we describe preliminary results we have obtained from the application of
the PLKsZ relations to the RR Lyrae stars in the VMC tile LMC 8_3. Once we have period
and dereddened mean Ks magnitude for each RR Lyrae star (Table 6.7), we can immediately
plot the PL relation. This is shown in Figure 6.4, where filled and open circles are RRab
and RRc stars, respectively. We computed a weighted PLKs relation through the data by
progressively discarding objects which deviate more than 3σ from the linear regression:
Ks,0 = (−2.40 ± 0.13)logP + (17.38 ± 0.03) (6.1)
Figure 6.4 shows only objects that are located within 3σ from the best fit line. The slope
of Eq. 6.1 differs from the slope in logP derived for the 71 RR Lyrae stars in tile LMC 5_5
(Eq. 5.3), but is still consistent with it within the errors. The zero-points of Eqs. 6.1 and 5.3
are consistent within the errors, even if Eq. 6.1 does not take into account the metallicity.
A number of different PLKsZ relations exist in the literature (see Section 1.5.2): Bono
et al. (2003) (see Eq. 6.4), Dall’Ora et al. (2004) (see Eq. 6.5), Sollima et al. (2006) (see
Eq. 6.3), Sollima et al. (2008) (see Eq. 6.2), Del Principe et al. (2006) (see Eq. 6.6),
Borissova et al. (2009) (see Eq. 6.7). Benedict et al. (2011) have estimated zero-points for
all these PLKsZ relations, based on their HST trigonometric parallaxes for five Galactic
field RR Lyrae stars:
MK = (−2.38 ± 0.04)(logP + 0.28) + (0.08 ± 0.11)([Fe/H] + 1.58) + a1, (6.2)
MK = (−2.38 ± 0.04)(logP + 0.28) + a2, (6.3)
MK = −2.101(logP + 0.28) + (0.231 ± 0.012)([Fe/H] + 1.58) + a3, (6.4)
MK = (−2.16 ± 0.09)(logP + 0.28) + a4, (6.5)
MK = (−2.71 ± 0.12)(logP + 0.28) + (0.12 ± 0.04)([Fe/H] + 1.58) + a5 (6.6)
MK = (−2.11 ± 0.17)(logP + 0.28) + (0.05 ± 0.07)([Fe/H] + 1.58) + a6 (6.7)
140
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3
where the a1 - a6 values are: −0.56 ± 0.02, −0.57 ± 0.03, −0.58 ± 0.04, −0.56 ± 0.02,
−0.57 ± 0.02, and −0.56 ± 0.03, respectively. They were derived by fitting the Lutz-
Kelker-Hanson-corrected absolute magnitudes to the equations (Benedict et al., 2011). The
different PLKsZ relations are based on a number of different metallicity scales. In particu-
lar, Bono et al. (2003) and Del Principe et al. (2006) use the Zinn & West metallicity scale.
Sollima et al. (2008) use the Carretta & Gratton (1997) metallicity scale. The relations
from Dall’Ora et al. (2004) and Sollima et al. (2006) do not have metallicity terms. Finally,
Borissova et al. (2009) use the same metallicity scale adopted by Gratton et al. (2004).
We add to the above literature relations (Eqs. 6.2-6.7) our own PLKsZ relation derived
using the dereddened mean Ks magnitudes of the 71 RR Lyrae stars in tile LMC 5_5, spec-
troscopically determined metallicities from Gratton et al. (2004) and accurately estimated
periods from the OGLE III catalogue (see Chapter 5):
MK = (−2.70 ± 0.22)logP + (0.03 ± 0.06)[Fe/H] + (−1.27 ± 0.08) (6.8)
The zero-point of our relation is also calibrated on the Benedict et al. (2011)’s HST
trigonometric parallaxes for RR Lyrae stars and the metallicity is on Gratton et al. (2004)
scale, hence, on average, 0.06 dex higher than Zinn & West’s. To derive the distance to
tile LMC 8_3 we entered the above relations using: periods for the RR Lyrae stars taken
from the EROS-2 catalogue, mean ⟨Ks⟩ dereddened magnitudes estimated as described in
Section 6.5, and metallicities obtained by the Fourier analysis of the V band light curves
(see Section 6.4).
In order to take into account the systematic difference of ∼ 0.25 dex between the mean
metallicities of RRab and RRc stars, we used three different approaches:
• We used the mean metallicity derived by averaging the photometric metallicities of
both RRab and RRc stars. We associated to the mean value obtained in this way
an error corresponding to the standard deviation of the distribution ⟨[Fe/H]C09⟩ =
−1.61; σ[Fe/H]C09= 0.4. Then we used the whole sample of 241 RRab and RRc stars
in tile LMC 8_3 to estimate the distance.
• We used the mean metallicities determined by averaging the photometric metallicities
obtained only for RRab stars. We associate to this mean value an error corresponding
to the standard deviation of the average: ⟨[Fe/H]C09ab⟩ = −1.58; σ[Fe/H]C09ab= 0.5,
141
6.6. DISTANCE TO THE TILE LMC 8_3 FROM RR LYRAE STARS
and inferred distance moduli from the above PLKsZ relations for each of the 167
ab-type RR Lyrae stars.
• We used the mean metallicity derived by averaging the photometric metallicities ob-
tained only from the RRc stars. We associated to this mean value an error correspond-
ing to the standard deviation of the average: ⟨[Fe/H]C09c⟩ = −1.82; σ[Fe/H]C09c=
0.3, and inferred distance moduli from the above PLKsZ relations for each of the 74
c-type RR Lyrae stars.
The derived mean metallicities are on the Carretta et al. (2009) metallicity scale. To
transform them to the Zinn & West metallicity scale, used in the majority of the PLKsZ
relations listed above we applied the transformation equation provided by Carretta et al.
(2009):
[Fe/H]C09 = (1.105 ± 0.061)[Fe/H]ZW + 0.160 (6.9)
To transform the mean metallicities on the Zinn & West scale to the metallicity scale of
Eq. 6.8, we simply added 0.06 dex (Gratton et al., 2004). In order to determine the mean
metallicities on the Carretta & Gratton (1997) metallicity scale we applied the relation from
Carretta et al. (2009):
[Fe/H]C09 = (1.137 ± 0.060)[Fe/H]GC97 − 0.003 (6.10)
Each of the above PLKsZ relations (Eqs. 6.2-6.8) was used to infer the MK absolute
magnitude for each RR Lyrae star in tile LMC 8_3. The MK values were combined with
the dereddened apparent K magnitude providing a distance modulus estimate µ0 for each
individual star. Average µ0 values and related standard errors inferred from the different
PLKsZ relations are summarized in Table 6.8.
In Chapter 5 we applied our PLKsZ relation with zero-point based on the HST paral-
laxes for RR Lyrae stars by Benedict et al. (2011) to 71 RR Lyrae stars in tile LMC 5_5
and determined the mean distance µ0 = 18.71 ± 0.01 mag, which can now be compared
with the average distance to tile LMC 8_3 : µ0 = 18.615± 0.006 mag. Taken at face value
these results indicate that the external tile LMC 8_3 is located 0.1 mag closer to us than the
central tile LMC 5_5. These results are preliminary and need to be further confirmed, still
they are promising. Combining them with results obtained from the RR Lyrae stars in other
142
CHAPTER 6. RR LYRAE STARS IN THE VMC TILE LMC 8_3
PLK -relation µ0(< ab >) µ0(< c >) µ0(< ab+ c >)mag mag mag
Bono et al 2003 18.623 ± 0.164 18.696 ± 0.192 18.636 ± 0.173Dall’Ora et al. 2004 18.596 ± 0170 18.610 ± 0.193 18.600 ± 0.176Sollima et al. 2008 18.596 ± 0.165 18.596 ± 0.200 18.594 ± 0.174Sollima et al. 2006 18.622 ± 0.164 18.612 ± 0.197 18.619 ± 0.174Del Principe et al. 2006 18.632 ± 0.165 18.618 ± 0.195 18.624 ± 0.174Borissova et al. 2009 18.600 ± 0.165 18.632 ± 0.186 18.607 ± 0.171Relation from this study 18.634 ± 0.159 18.605 ± 0.195 18.625 ± 0.170average 18.615 ± 0.006 18.625 ± 0.013 18.615 ± 0.006
Table 6.8 Distance moduli of tile LMC 8_3 obtained applying different PLKsZ relations tothe RR Lyrae stars in this tile (Column 1: References for the PLKsZ relations; Column 2:Distance modulus obtained using only RRab stars; Column 3: Distance modulus obtainedusing only RRc stars; Column 4: Distance modulus obtained using all the ab and c-type RRLyrae stars in tile LMC 8_3. See text for details).
VMC tiles we will be able to map the internal structure of the LMC as traced by the old
population stars.
143
6.6. DISTANCE TO THE TILE LMC 8_3 FROM RR LYRAE STARS
Figure 6.4 Dereddened mean Ks magnitudes versus LogP for RR Lyrae stars in tile LMC
8_3. Empty and filled circles represent RRc and RRab stars, respectively. The periods of
RRc stars were fundamentalized by adding 0.127 to the LogP.
144
Conclusions
The main goal of this thesis was to study the geometric structure and the distance to the
Large Magellanic Cloud (LMC). To this purpose we have analysed three different types
of distance indicators: Classical Cepheids (CCs), “hot” eclipsing binaries (HEBs) and RR
Lyrae stars, which trace different sub-structures of the LMC.
Main results which we derived for the CCs are:
• We analysed 201 candidate CCs observed by the EROS-2 survey in the VMC tile
LMC 8_3. We classified the candidate CCs trough visual inspection of the light
curves. The sample was found to contain 124 bona-fide CCs, 2 candidate Anomalous
Cepheids, 58 eclipsing binaries, 13 small amplitude variables and 4 long period vari-
ables. Furthermore, in the sample of bona-fide CCs we found two double-mode CCs
and derived second periods for both of them.
• We determined main parameters (mean magnitudes, amplitudes and epochs of max-
imum light in the BEROS and REROS passbands) for all the 201 objects, checked
the periods provided by the EROS-2 survey and derived new periods for 16 of them.
The main parameters of the bona-fide CCs will be used in the future along with near-
infrared data from the VMC survey to measure the distance to the genuine CCs in this
tile.
• We developed a strategy for extracting bona-fide CCs from the EROS-2 sample of
candidate CCs which is based on the combination of colour-cuts in the CMD and
analysis of the scatter in the PL relations. This approach allowed us to extract a
sample of bona-fide CCs more than 97 % clean from contaminating sources. This
strategy will be applied in the analysis of all the external tiles of the LMC, for which
only the EROS-2 data are available.
The main results for HEBs are:
145
CONCLUSIONS
• We identified in the whole sample of the EROS-2 candidate CCs, 1768 EBs by com-
bining the colour-cut criterion and the visual inspection of the light curves. They are
composed by hot main sequence stars or blue giants, hence we classed them HEBs.
• We analysed the light curves of the 1768 HEBs and re-determined the previously
defined periods for 225 of them.
• We divided the sample of 1768 HEBs into contact-like (324) and non-contact (1444)
systems by visual inspection of their light curves and by analysis of the Fourier de-
composition parameters.
• We analysed the PL relation in the optical (REROS and I) and Ks passbands of the
contact-like HEBs in the EROS-2 sample. We did not confirm the existence of a PL
relation for contact-like HEBs.
• We found that contact EBs containing a red giant component from the OGLE III
catalogue do follow PL sequences in the I and Ks passbands. We computed the
weighted linear regression of the PL relation in the Ks passband:
Ks,0 = (−2.888 ± 0.096)log(P ) + (20.139 ± 0.171) (6.11)
with rms=0.406 mag.
There is a possible additional PL sequence located ∼ 1 mag fainter, but the number
of objects following it, is too small to allow a reliable fit.
Main results for the RR Lyrae stars in tile LMC 5_5 are:
• We analysed a sample of 71 RR Lyrae stars in this tile close to the bar of the LMC,
for which multi-epoch Ks photometry from the VMC survey, precise periods from
the OGLE III catalogue and spectroscopically determined metallicity are available.
We derived the mean Ks magnitudes of these stars by fitting templates from Jones et
al. (1996) to the VMC data.
• We derived a new PLKsZ relation for RR Lyrae stars by using a Bayesian fitting ap-
proach. The new PLKsZ relation has a number of advantages: (i) it uses multi-epoch
Ks photometry from the VMC survey to derive light curves and estimate mean Ks
magnitudes of the RR Lyrae stars, while in most studies single-epoch photometry is
146
CONCLUSIONS
used; (ii) it uses precisely determined periods from the OGLE III survey; (iii) the rela-
tion is based on a relatively large sample of the RR Lyrae stars with spectroscopically
determined metallicities in the range −2.06 < [Fe/H] < −0.63 dex (Gratton et al.,
2004); (iv) it is derived based on a Bayesian fitting approach developed specifically
for this study. This method takes into account: 1) the potentially significant intrinsic
dispersion of the data; 2) non-negligible errors in two dimensions; 3) the possibility
of inaccuracy in the formal error estimates.
• We calibrated the zero-point of our new PLKsZ relation by applying two different
techniques: (i) by using the distance to the LMC determined by Pietrzynski et al.
(2013); (ii) by applying the HST parallaxes of five MW RR Lyrae stars from Benedict
et al. (2011).
• We applied our PLKsZ relation with the zero-point calibrated from the HST paral-
laxes and derived the distance to tile LMC 5_5: (m − M)0 = 18.71 ± 0.09 mag.
This distance modulus is about 0.2 mag longer than the widely adopted value of
(m − M)0 = 18.5 mag. In future studies we suggest to use the relation with the
zero-point based on the precise distance to the LMC:
MK = (−2.70 ± 0.22)logP + (0.03 ± 0.06)[Fe/H]Har + (−1.05 ± 0.05) (6.12)
• We estimated the impact of Gaia on definition of the zero-point of the RR Lyrae
PLKsZ and MV − [Fe/H] relations. We selected 25 bright MW RR Lyrae stars and
simulated their Gaia parallaxes with observational errors. We applied a Bayesian fit-
ting approach specifically developed for this study to derive PLKsZ and MV −[Fe/H]
relations based on the simulated parallaxes. The final relations are very close to those
which were considered as "true" in the input and their zero-points have respectively
precisions of 0.03 mag and 0.005 mag.
Main results for the RR Lyrae stars in tile LMC 8_3 are:
• We analysed the sample of EROS-2 candidate RR Lyrae stars in tile LMC 8_3 and
extracted 251 bona-fide RR Lyrae variables that have a counterpart in the VMC cata-
logue.
• We classified the 251 bona-fide RR Lyrae stars based on both, the visual inspection
of the light curves and the analysis of the period-amplitude diagram. The sample
147
CONCLUSIONS
contains 167 RRab, 74 RRc and 10 RRd stars. For each star we derived mean magni-
tudes, amplitudes, epochs of maximum light in the BEROS and V passbands.
• We checked the periods provided by the EROS-survey and corrected them for four
objects. We determined the second periods for the 10 RRd stars.
• We performed the Fourier decomposition of the light curves of the 241 bona-fide
RRab and RRc variables and determined photometric metallicities from the Fourier
parameters of the light curves for 132 RRab stars and 17 RRc stars. The mean metal-
licity on the Carretta et al. (2009) metallicity scale, of the RRab stars in tile LMC
8_3 is ⟨[Fe/H]C09ab⟩ = −1.58; σ[Fe/H]C09ab= 0.5, whereas the mean metallicity
of the RRc stars is ⟨[Fe/H]C09c⟩ = −1.82; σ[Fe/H]C09c= 0.3. The mean metallic-
ity derived by averaging the photometric metallicities of both RRab and RRc stars is
⟨[Fe/H]C09⟩ = −1.61; σ[Fe/H]C09= 0.4. There is a shift of about 0.25 dex between
mean metallicities of RRab and RRc stars, the reason of which could be some sys-
tematics in the calibration of the relations used to derive the photometric metallicities.
• We fitted the Ks band light curves obtained by the VMC survey with templates from
Jones et al. (1996) and derived mean Ks magnitudes for 241 RR Lyrae stars. We
computed a weighted PLKs relation through the data:
Ks,0 = (−2.40± 0.13)logP + (17.38 ± 0.03) (6.13)
• We used the PLKsZ relations in the literature and our new PLKsZ relation computed
from 71 RR Lyrae stars in tile LMC 5_5 to determine individual distances to the 251
RR Lyrae stars in tile LMC 8_3 and derived the mean distance modulus: (m−M)0 =
18.615 ± 0.006 mag. These results show that the external tile LMC 8_3 seems to be
located 0.1 mag closer to us than the central tile LMC 5_5.
The comparison of the spatial distribution of the three different distance indicators re-
vealed the internal structure of the LMC. The RR Lyrae stars have a larger density in the
central region of the LMC, but in general they are distributed smoothly and likely trace
the halo of the galaxy. On the contrary, CCs and HEBs are strongly concentrated towards
the LMC bar and spiral arm, and almost disappear in the peripheral areas. HEBs are more
sharply concentrated toward regions of recent star formation such as 30 Doradus and Con-
stellation III, while CCs mostly follow the bar and spiral arm of the LMC.
148
CONCLUSIONS
From the analysis of the EBs we confirmed the existence of PL relations only for con-
tact EBs that contain a red giant component, while did not confirm the existence of a PL
relation for contact HEBs. The luminosity ratio of the components of the HEBs (main se-
quence stars and blue giants) can vary significantly. In contrast, in contact systems with a
red giant component, the giant dominates the luminosity while the contribution from the
secondary is usually negligible. As a consequence the PL relation of contact HEBs can be
much more scattered than the PL of contact EBs with a red giant component. In any case,
the scatter of the PL relation for EBs with a red giant component is too large to be used for
the determination of the distance.
The results from the RR Lyrae stars in tiles LMC 8_3 and 5_5 are puzzling and need
further investigation. The zero-point of the PLKsZ relation of RR Lyrae stars still remains
a controversial issue that cannot be solved with the present data. While this is not going to
affect our study of the structure of the LMC through the VMC data, for which we will use
differential distances, the absolute distance to the LMC from RR Lyrae stars can be derived
only when the RR Lyrae zero-point issue will be settled. A huge improvement in this topic is
expected with the astrometric mission Gaia which will measure the parallaxes of thousands
MW RR Lyrae stars. In this thesis we simulated Gaia parallaxes of only 25 bright Galactic
RR Lyrae stars and showed that using even a small sample of RR Lyrae stars with precisely
determined parallaxes we will be able to estimate the PLKsZ and MV − [Fe/H] relations
with a great precision, when combined with metallicity and photometry from other sources.
The zero-points of the CCs and EBs will also be recalibrated with Gaia, thus allowing a
direct and robust comparison of the the distance to the LMC as derived from independent
distance indicators.
149
Appendix A
Properties of the “hot” eclipsingbinaries in the LMC
Main properties and Fourier parameters of the light curves of 1768 HEBs in our sample are
presented in Table A.1. The table provides the EROS-2 identification numbers (column 1)
and coordinates (RA and DEC at J2000; columns 2 and 3) of the HEBs. Periods (column 4)
for the majority of stars are from the EROS-2 catalogue, while for 225 sources marked by an
asterisk, periods were recalculated in this study. Number of digits in the periods are the same
as originally listed in the EROS-2 catalogue. Mean ⟨BEROS⟩ and ⟨REROS⟩ magnitudes
are listed in columns 5 and 6, respectively. The EROS-2 team provided us values with three
digits as computed using all observations involved in the period determination (e.g. after
excluding outliers), however we rounded them to two digits to account for the typical errors
of the individual data-points which vary from 0.02 to 0.08 mag depending on magnitude.
Column 7 lists the epochs of minimum light in the REROS passband we calculated in this
study, they are listed with four digits, in agreement with the actual precision of EROS-2
HJDs (see below). Columns from 8 to 13 of Table A.1 present the parameters of the Fourier
decomposition in the REROS passband calculated in this study. HJDs provided by the
EROS-2 catalogue are accurate to within 10 s, hence, epochs of minimum light have four
digit accuracy.
Finally, Table A.2 provides information about the cross-identifications (EROS-2 and
VMC IDs) for 999 HEBs in common between the two catalogues, their periods and the Ks
and REROS magnitudes at maximum light.
151
ERO
S-2
idR
AD
ECPe
riod
⟨REROS⟩
⟨BEROS⟩
Epoc
h(m
in)
a0
a1
a2
a3
a4
a5
(J20
00)
(J20
00)
(HJD
−2,
450,
000)
(deg
)(d
eg)
(day
)(m
ag)
(mag
)lm
0555
k127
21*
76.2
287
-71.
2391
90.
8010
095
17.2
617
.08
2184
.700
90.
957
-0.0
37-0
.055
-0.0
070
-0.0
160.
0030
lm03
23n2
0546
80.4
206
-66.
8744
0.90
0708
17.2
417
.06
1851
.626
30.
879
-0.0
28-0
.167
-0.0
14-0
.062
-0.0
030
lm03
54n8
770
85.1
1371
-67.
1645
40.
9040
0317
.64
17.4
011
85.7
298
0.91
3-0
.03
-0.1
27-0
.008
0-0
.041
0.00
20lm
0193
k191
8279
.737
58-6
8.10
716
0.90
5358
17.0
516
.99
2213
.782
10.
958
-0.0
1-0
.047
-0.0
060
-0.0
240.
0060
lm03
41k8
979
83.6
6655
-66.
3030
70.
9117
2117
.00
16.7
511
73.7
244
0.88
2-0
.032
-0.1
73-0
.011
-0.0
740.
0lm
0285
n102
2973
.417
11-6
7.17
722
0.91
1792
17.0
716
.85
1532
.577
30.
973
-0.0
15-0
.02
-0.0
010
0.00
10-0
.002
0lm
0344
m26
510
83.0
365
-67.
1281
80.
9124
4517
.32
17.1
817
51.8
628
0.91
7-0
.01
-0.1
170.
0020
-0.0
520.
0060
lm00
23n1
1843
83.3
321
-69.
6220
90.
9125
6817
.46
17.3
917
01.4
807
0.85
4-0
.033
-0.1
41-0
.01
-0.0
320.
017
lm01
23m
1183
673
.493
11-6
9.46
511
0.91
9332
17.1
817
.29
2519
.731
90.
97-0
.014
-0.0
37-0
.005
0-0
.013
-0.0
010
lm01
22n1
3303
72.4
6236
-69.
6452
20.
9226
0417
.17
16.9
443
8.82
730.
947
-0.0
23-0
.08
-0.0
1-0
.018
0.00
40lm
0030
n213
9184
.323
19-6
9.38
179
0.92
2672
16.8
816
.77
2304
.768
60.
883
-0.0
43-0
.153
-0.0
18-0
.046
-0.0
010
lm02
26n2
0767
84.6
0396
-69.
0012
50.
9239
4117
.65
17.4
519
75.6
799
0.91
3-0
.013
-0.1
2-0
.005
0-0
.056
-0.0
lm01
06n1
3876
76.5
4384
-70.
3435
30.
9253
4417
.51
17.3
649
8.60
620.
892
-0.0
33-0
.133
-0.0
21-0
.043
-0.0
010
lm02
31k9
063
87.1
2851
-67.
7065
30.
9279
9917
.07
16.8
410
72.8
079
0.88
-0.0
2-0
.141
-0.0
050
-0.0
310.
0020
lm01
14k6
489
74.0
4547
-69.
7893
20.
9320
9717
.54
17.4
395
2.46
630.
982
-0.0
28-0
.025
0.0
-0.0
110.
0040
lm02
83n8
062
73.6
8666
-66.
7968
40.
9389
2317
.10
16.8
122
55.5
680
0.85
5-0
.034
-0.1
98-0
.014
-0.0
71-0
.005
0lm
0214
n104
5982
.863
71-6
8.57
040.
9389
7117
.76
17.7
216
59.5
486
0.95
-0.0
13-0
.084
-0.0
020
-0.0
50.
0050
lm01
71m
1673
3*76
.183
53-6
7.74
663
0.93
9001
15.9
115
.61
1915
.751
60.
948
-0.0
010
-0.0
71-0
.002
0-0
.028
-0.0
010
lm01
27k1
2134
73.2
6783
-70.
1808
40.
9394
5417
.47
17.5
122
25.5
710
0.98
1-0
.003
0-0
.046
-0.0
-0.0
29-0
.0lm
0215
l150
0483
.632
46-6
8.59
249
0.94
0678
17.2
417
.06
2200
.784
90.
912
-0.0
050
-0.1
41-0
.003
0-0
.08
-0.0
010
lm00
43k2
3371
86.9
9351
-69.
5312
0.94
1374
17.4
517
.43
1478
.771
70.
902
-0.0
31-0
.114
-0.0
11-0
.043
-0.0
010
lm03
42k1
8196
82.8
9531
-66.
7500
20.
9414
4717
.03
16.8
243
4.80
950.
911
-0.0
060
-0.1
11-0
.001
0-0
.045
-0.0
050
lm03
46l1
4981
82.7
9685
-67.
5609
0.94
1548
17.0
417
.07
1657
.518
40.
985
-0.0
25-0
.035
-0.0
11-0
.017
-0.0
lm04
66k2
3468
81.4
0389
-66.
0712
60.
9430
3217
.24
17.0
411
40.6
191
0.86
7-0
.04
-0.1
86-0
.018
-0.0
55-0
.007
0lm
0167
m21
114
74.7
5322
-68.
8346
70.
9431
8917
.76
17.5
933
6.87
080.
956
-0.0
2-0
.055
-0.0
060
-0.0
32-0
.002
0lm
0436
n210
3676
.816
2-6
6.20
443
0.94
4593
17.1
916
.93
1866
.612
50.
874
-0.0
31-0
.156
-0.0
12-0
.042
-0.0
040
lm03
41k1
8581
83.7
3331
-66.
3684
0.94
7627
17.3
717
.22
1981
.624
20.
985
-0.0
33-0
.006
0-0
.005
0-0
.005
00.
0030
lm03
41k4
660
83.6
1982
-66.
2723
10.
9533
7417
.34
17.0
918
69.6
179
0.93
2-0
.007
0-0
.107
-0.0
11-0
.069
-0.0
050
lm02
17m
1920
884
.090
04-6
8.82
472
0.95
4486
16.9
817
.01
2338
.661
70.
976
-0.0
24-0
.031
-0.0
040
-0.0
030
0.0
lm00
30n1
9548
84.4
7044
-69.
3371
10.
9552
6117
.09
16.9
321
67.8
026
0.94
2-0
.005
0-0
.077
-0.0
010
-0.0
31-0
.001
0lm
0090
n162
4378
.417
69-6
9.30
601
0.95
6439
16.9
216
.90
2198
.668
90.
953
-0.0
080
-0.0
7-0
.005
0-0
.04
-0.0
020
lm03
40m
1585
283
.069
71-6
6.35
575
0.95
8465
17.4
617
.28
2310
.712
70.
979
-0.0
62-0
.019
-0.0
17-0
.006
00.
0070
lm00
72n1
2336
92.5
0478
-69.
6507
50.
9593
17.6
117
.47
1784
.868
20.
91-0
.042
-0.1
28-0
.019
-0.0
580.
0010
lm01
02m
1044
176
.453
63-6
9.46
743
0.96
0451
17.2
216
.96
2496
.822
20.
859
-0.0
1-0
.226
0.00
50-0
.089
0.00
40lm
0015
k638
380
.934
04-6
9.79
310.
9641
5917
.16
16.9
777
2.83
830.
879
-0.0
090
-0.1
66-0
.007
0-0
.073
-0.0
010
lm05
42k2
0454
72.9
0434
-70.
9645
80.
9658
3817
.37
17.3
216
59.4
784
0.97
5-0
.048
-0.0
39-0
.032
-0.0
2-0
.004
0lm
0034
k102
3883
.799
16-6
9.82
040.
9689
8817
.19
17.2
821
60.7
476
0.92
-0.0
3-0
.122
-0.0
1-0
.056
0.00
10lm
0160
m26
440
73.5
2748
-67.
8170
20.
9691
5817
.74
17.7
314
93.6
251
0.96
1-0
.014
-0.0
360.
0020
-0.0
030
0.0
152
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0355
n118
6686
.035
32-6
7.17
845
0.96
9348
17.2
217
.08
1774
.920
30.
98-0
.056
-0.0
3-0
.02
-0.0
1-0
.008
0lm
0604
l157
3385
.467
77-7
1.41
346
0.97
6899
17.8
217
.67
1179
.844
70.
957
-0.0
26-0
.065
-0.0
17-0
.027
-0.0
090
lm00
93k1
6356
79.0
9752
-69.
4890
80.
9771
8617
.00
16.9
555
4.53
240.
926
-0.0
17-0
.105
-0.0
060
-0.0
32-0
.001
0lm
0321
l271
5880
.227
24-6
6.57
613
0.97
7509
17.2
817
.14
1236
.602
50.
937
-0.1
25-0
.086
-0.0
54-0
.025
0.00
10lm
0352
m18
009
85.0
8721
-66.
7491
90.
9789
6317
.81
17.6
111
42.7
253
0.96
6-0
.001
0-0
.05
-0.0
040
-0.0
320.
0020
lm02
23n2
6953
85.6
8687
-68.
3124
20.
9790
3417
.68
17.5
616
36.5
279
0.98
2-0
.017
-0.0
25-0
.001
0-0
.002
0-0
.0lm
0023
k200
2183
.115
16-6
9.51
038
1.01
1662
16.9
016
.89
1482
.731
10.
942
-0.0
12-0
.083
-0.0
050
-0.0
39-0
.002
0lm
0594
k127
0083
.460
81-7
1.23
035
1.01
9228
17.5
217
.56
2201
.644
30.
973
-0.0
12-0
.027
0.0
-0.0
040
0.00
20lm
0033
m10
429
85.3
568
-69.
4624
91.
0192
3217
.86
17.7
821
69.8
024
0.96
2-0
.02
-0.0
47-0
.003
0-0
.007
00.
0030
lm01
17l9
906
75.0
4975
-70.
3230
11.
0200
3417
.26
17.1
013
88.8
013
0.93
2-0
.019
-0.0
84-0
.009
0-0
.031
-0.0
060
lm00
30n2
2649
84.3
3989
-69.
3578
91.
0265
2816
.76
16.6
412
55.6
286
0.95
1-0
.007
0-0
.076
-0.0
020
-0.0
350.
0020
lm03
23l2
7434
79.9
3833
-66.
9190
21.
0272
0617
.34
17.2
217
76.8
380
0.90
9-0
.016
-0.1
21-0
.008
0-0
.055
0.00
20lm
0025
n170
9183
.559
48-6
9.99
927
1.02
8086
17.5
717
.71
1763
.812
10.
968
-0.0
15-0
.048
-0.0
11-0
.015
-0.0
010
lm01
66n2
4423
73.6
9688
-69.
0193
41.
0332
8517
.41
17.0
986
4.69
760.
952
-0.0
22-0
.038
-0.0
010
-0.0
0.0
lm04
15m
2190
274
.362
23-6
5.69
419
1.03
3457
17.6
217
.35
2241
.606
90.
957
-0.0
010
-0.0
73-0
.001
0-0
.048
-0.0
030
lm01
65n1
4065
74.7
7506
-68.
5824
31.
0380
7217
.52
17.3
448
0.76
380.
974
-0.0
23-0
.028
-0.0
010
-0.0
040
0.00
10lm
0157
l178
2172
.473
1-6
8.98
049
1.04
055
17.6
317
.47
2229
.566
00.
889
-0.0
46-0
.144
-0.0
23-0
.028
-0.0
010
lm00
91m
2706
479
.325
71-6
9.20
378
1.04
1214
17.3
216
.97
333.
8872
0.82
6-0
.048
-0.1
83-0
.013
-0.0
760.
0060
lm00
93n5
032
79.5
86-6
9.58
177
1.04
2603
16.8
416
.65
1549
.649
80.
918
-0.0
23-0
.09
-0.0
040
-0.0
22-0
.001
0lm
0405
n237
8694
.582
84-6
7.26
861
1.04
6324
16.3
916
.48
865.
7215
0.99
5-0
.02
-0.0
040
-0.0
040
-0.0
040
-0.0
020
lm01
73m
9757
76.2
3218
-68.
0513
91.
0468
816
.83
16.7
874
8.79
530.
94-0
.013
-0.0
83-0
.006
0-0
.037
-0.0
020
lm04
24n1
4561
74.9
1334
-65.
8054
51.
0472
3516
.78
16.5
320
57.4
711
0.93
3-0
.003
0-0
.093
-0.0
060
-0.0
510.
0010
lm03
17m
2435
178
.603
69-6
7.46
527
1.04
9265
17.2
417
.12
2185
.658
10.
987
-0.0
42-0
.03
-0.0
25-0
.018
-0.0
050
lm01
12n5
096
74.4
563
-69.
5837
11.
0502
2317
.77
17.6
523
27.5
878
0.87
8-0
.005
0-0
.195
0.00
40-0
.089
0.00
10lm
0493
n186
9287
.281
21-6
5.47
855
1.05
0931
17.6
317
.74
830.
8104
0.91
4-0
.041
-0.1
15-0
.018
-0.0
39-0
.003
0lm
0031
m96
5185
.603
44-6
9.10
275
1.05
1009
17.0
617
.15
2174
.803
10.
938
-0.0
060
-0.0
95-0
.001
0-0
.056
-0.0
020
lm00
11l5
712
80.9
5532
-69.
2395
11.
0512
3817
.18
16.8
922
14.6
057
0.84
5-0
.028
-0.1
86-0
.017
-0.0
57-0
.002
0lm
0244
k107
4887
.995
23-6
8.42
181.
0516
0817
.82
17.8
015
76.7
872
0.87
1-0
.039
-0.1
49-0
.018
-0.0
480.
0070
lm03
56m
2406
984
.996
3-6
7.46
769
1.05
1643
17.2
617
.11
1263
.623
40.
977
-0.0
83-0
.035
-0.0
23-0
.008
0-0
.012
lm05
40l1
5552
72.9
1439
-70.
7063
61.
0521
6517
.83
17.6
422
96.6
801
0.80
6-0
.046
-0.2
22-0
.022
-0.0
65-0
.007
0lm
0020
l855
381
.839
68-6
9.26
417
1.05
4358
17.1
516
.92
1835
.799
80.
893
-0.0
010
-0.1
61-0
.004
0-0
.087
0.00
10lm
0367
n188
0587
.432
52-6
7.60
061
1.05
5955
17.6
617
.47
2353
.670
90.
962
-0.0
35-0
.07
-0.0
18-0
.039
0.00
50lm
0311
l960
678
.420
94-6
6.46
266
1.05
9117
16.5
316
.32
1858
.840
90.
93-0
.021
-0.0
98-0
.008
0-0
.027
-0.0
lm03
56m
1026
484
.894
58-6
7.37
154
1.05
9355
17.1
717
.05
405.
8067
0.96
50.
0-0
.075
0.00
10-0
.052
-0.0
060
lm04
63m
8760
82.4
7922
-65.
2473
71.
0594
8317
.87
17.6
819
34.7
227
0.95
6-0
.02
-0.0
40.
0020
-0.0
040
0.00
50lm
0355
k172
1685
.564
42-6
7.06
382
1.06
0366
16.9
916
.83
1248
.615
50.
883
-0.0
45-0
.163
-0.0
2-0
.07
0.0
lm05
51m
9243
76.4
3002
-70.
5058
81.
0646
4916
.53
16.1
918
56.6
163
0.94
6-0
.014
-0.0
64-0
.002
0-0
.016
0.00
20lm
0184
n148
4477
.143
24-6
8.59
311
1.06
7386
17.0
216
.85
2020
.515
10.
968
-0.0
11-0
.051
-0.0
020
-0.0
270.
0lm
0585
m29
810
83.0
6159
-71.
3173
1.06
795
17.2
417
.05
1923
.685
40.
925
-0.0
23-0
.088
-0.0
080
-0.0
180.
0030
lm02
90k1
8569
74.0
2612
-66.
3812
91.
0683
9216
.21
16.0
119
25.5
978
0.94
8-0
.013
-0.0
58-0
.0-0
.009
0-0
.002
0lm
0341
n190
184
.046
94-6
6.42
796
1.06
9987
16.7
316
.43
1616
.587
10.
93-0
.022
-0.1
11-0
.01
-0.0
61-0
.0
153
lm05
70m
2030
179
.779
65-7
0.57
244
1.07
0216
16.2
416
.03
875.
6007
0.93
5-0
.021
-0.0
82-0
.005
0-0
.02
-0.0
020
lm03
36l2
1294
81.1
102
-67.
5991
61.
0708
4717
.81
17.5
535
3.83
580.
925
-0.0
060
-0.1
390.
0-0
.10.
0030
lm03
34l2
0690
80.8
7888
-67.
2388
71.
0713
3317
.05
16.8
814
95.8
507
0.95
3-0
.101
-0.0
7-0
.053
-0.0
26-0
.012
lm01
16m
1775
274
.319
9-7
0.21
411
1.07
1932
16.9
016
.68
1608
.557
00.
859
-0.0
4-0
.188
-0.0
19-0
.063
-0.0
020
lm01
23m
3222
73.4
2292
-69.
4153
81.
0726
3316
.94
16.8
516
18.5
335
0.93
1-0
.017
-0.0
86-0
.005
0-0
.028
-0.0
lm03
35l1
6808
81.8
1014
-67.
2113
21.
0737
0316
.19
15.9
618
67.6
534
0.95
5-0
.007
0-0
.061
-0.0
020
-0.0
250.
0lm
0337
k164
4281
.808
75-6
7.41
741
1.07
405
17.6
117
.48
2463
.880
30.
963
-0.0
090
-0.0
61-0
.004
0-0
.041
-0.0
030
lm02
95l1
9334
74.9
3114
-67.
2190
61.
0747
0216
.93
16.7
120
80.9
085
0.97
4-0
.011
-0.0
24-0
.002
00.
0010
0.00
10lm
0207
n197
6182
.231
04-6
8.99
163
1.07
4897
17.2
417
.07
2337
.617
50.
943
-0.0
19-0
.097
-0.0
13-0
.045
0.00
10lm
0335
n642
282
.476
19-6
7.13
888
1.07
6161
17.2
817
.00
802.
8039
0.97
6-0
.023
-0.0
27-0
.008
0-0
.012
-0.0
010
lm00
22k2
100
82.1
9138
-69.
4210
81.
0793
8916
.35
16.1
218
81.6
874
0.92
4-0
.021
-0.0
82-0
.001
0-0
.02
0.00
50lm
0184
k200
1576
.788
47-6
8.47
51.
0797
4117
.45
17.3
612
24.6
259
0.96
5-0
.043
-0.0
45-0
.015
-0.0
27-0
.002
0lm
0157
n980
372
.530
28-6
8.92
034
1.08
0202
17.4
317
.25
429.
7768
0.92
6-0
.035
-0.1
15-0
.016
-0.0
460.
0030
lm03
14n1
0220
77.8
5657
-67.
1738
51.
0805
6316
.37
16.1
522
34.5
971
0.94
8-0
.004
0-0
.066
-0.0
020
-0.0
28-0
.0lm
0326
l756
179
.197
04-6
7.49
735
1.08
1099
16.9
116
.86
440.
5993
0.97
7-0
.0-0
.034
0.00
20-0
.03
0.00
70lm
0120
n262
0672
.464
3-6
9.36
574
1.08
1433
16.7
816
.70
1531
.573
60.
964
-0.0
12-0
.054
-0.0
030
-0.0
21-0
.002
0lm
0040
k162
2585
.899
43-6
9.15
902
1.08
7516
17.4
517
.27
1900
.618
70.
920.
0010
-0.1
0.0
-0.0
42-0
.003
0lm
0044
m42
0386
.334
72-6
9.77
792
1.08
7685
16.3
416
.22
1585
.724
00.
917
-0.0
12-0
.131
-0.0
030
-0.0
77-0
.001
0lm
0311
l247
2578
.416
42-6
6.56
447
1.09
0105
17.9
217
.74
2234
.597
10.
9-0
.047
-0.1
43-0
.022
-0.0
67-0
.003
0lm
0374
n604
788
.328
48-6
7.14
495
1.09
0677
17.5
317
.37
1939
.782
70.
97-0
.012
-0.0
18-0
.002
00.
00.
0060
lm03
01m
2633
676
.876
21-6
6.41
165
1.09
0782
17.8
417
.66
1438
.819
80.
971
-0.0
3-0
.019
-0.0
16-0
.001
00.
014
lm04
25n2
6027
75.7
4082
-65.
8787
41.
0908
4917
.95
17.8
216
09.5
550
0.93
70.
045
-0.0
980.
022
-0.0
410.
0010
lm05
84l1
1571
81.6
8072
-71.
3754
31.
0919
8917
.78
17.7
718
28.7
310
0.93
4-0
.016
-0.0
8-0
.01
-0.0
20.
0030
lm04
66m
1201
981
.757
79-6
5.98
167
1.09
2537
16.9
216
.69
2142
.839
80.
972
-0.0
1-0
.029
-0.0
030
-0.0
130.
0020
lm03
43k8
884
83.7
1834
-66.
6522
91.
0926
4416
.74
16.5
417
64.8
820
0.91
1-0
.008
0-0
.117
-0.0
060
-0.0
40.
0010
lm05
93l2
4799
84.8
8857
-71.
0928
61.
0933
7517
.49
17.4
519
15.6
440
0.93
6-0
.004
0-0
.109
-0.0
-0.0
52-0
.004
0lm
0207
l996
581
.714
55-6
8.92
461.
0949
0416
.84
16.6
319
66.6
365
0.92
9-0
.026
-0.0
9-0
.004
0-0
.02
-0.0
020
lm03
60n1
1911
86.5
6384
-66.
4813
91.
0951
7917
.76
17.6
419
25.8
028
0.96
6-0
.033
-0.0
41-0
.005
0-0
.011
-0.0
020
lm02
07l1
1656
81.6
0031
-68.
9372
91.
0954
1917
.74
17.7
423
27.6
642
0.98
1-0
.037
-0.0
31-0
.011
-0.0
12-0
.001
0lm
0021
n128
9083
.331
13-6
9.39
681
1.09
5632
17.4
417
.39
537.
5088
0.85
6-0
.012
-0.1
61-0
.004
0-0
.06
-0.0
030
lm03
44m
1045
883
.335
15-6
7.02
379
1.09
8211
16.2
616
.04
1300
.563
40.
992
-0.0
1-0
.012
-0.0
020
-0.0
020
0.00
40lm
0093
n123
5079
.697
03-6
9.61
813
1.10
0478
17.7
217
.67
1463
.717
60.
983
-0.0
14-0
.066
-0.0
060
-0.0
42-0
.0lm
0550
k131
3775
.288
8-7
0.54
11.
1030
217
.13
16.9
415
91.6
349
0.96
7-0
.01
-0.0
550.
0-0
.027
-0.0
030
lm01
21l5
053
73.2
0473
-69.
2297
31.
1049
9116
.37
16.0
718
88.5
707
0.94
-0.0
050
-0.0
83-0
.001
0-0
.036
0.0
lm03
66k1
7409
86.0
5265
-67.
427
1.10
5186
16.4
916
.38
1627
.612
30.
979
-0.0
69-0
.039
-0.0
25-0
.01
-0.0
010
lm03
64l1
3690
86.2
1409
-67.
2048
91.
1056
1717
.08
16.8
715
79.7
251
0.97
7-0
.013
-0.0
47-0
.011
-0.0
310.
0030
lm03
43l2
4033
83.4
3983
-66.
9044
51.
1072
9517
.08
17.0
316
07.6
250
0.96
3-0
.074
-0.0
66-0
.049
-0.0
380.
0040
lm03
46l8
111
82.7
8009
-67.
5065
51.
1127
6117
.17
16.9
978
0.83
480.
931
0.00
80-0
.109
0.00
20-0
.07
0.0
lm02
43l1
6058
88.8
1548
-68.
2634
51.
1128
0717
.48
17.5
111
16.8
745
0.95
1-0
.025
-0.0
6-0
.001
0-0
.013
0.0
lm01
56n2
1172
71.7
8486
-68.
9931
21.
1139
917
.80
17.5
916
03.5
730
0.94
7-0
.021
-0.0
73-0
.016
-0.0
390.
0040
lm02
83k1
1461
73.2
1344
-66.
6709
61.
1146
2216
.97
16.8
418
48.7
862
0.92
-0.0
22-0
.08
-0.0
10.
0010
0.00
20
154
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0232
l172
5986
.315
77-6
8.27
398
1.12
0751
17.3
317
.21
1660
.541
80.
879
-0.0
51-0
.179
-0.0
26-0
.085
0.00
40lm
0265
k116
8092
.571
42-6
8.43
939
1.12
1349
17.6
717
.58
1660
.584
40.
922
-0.0
-0.1
09-0
.001
0-0
.055
-0.0
010
lm04
57k1
8380
80.6
1203
-66.
0282
71.
1273
4717
.50
17.3
412
57.5
744
0.90
6-0
.036
-0.1
28-0
.015
-0.0
45-0
.001
0lm
0172
l662
675
.228
37-6
8.23
722
1.13
021
17.1
016
.90
1848
.807
00.
895
-0.0
050
-0.1
52-0
.002
0-0
.078
-0.0
030
lm01
02l5
415
76.1
4952
-69.
5920
11.
1313
5216
.44
16.3
119
56.6
302
0.91
3-0
.027
-0.1
-0.0
14-0
.037
0.00
40lm
0486
l660
584
.433
5-6
6.09
065
1.13
1517
17.2
116
.99
537.
5438
0.94
1-0
.02
-0.0
75-0
.004
0-0
.035
-0.0
010
lm03
10k1
5114
77.5
2638
-66.
3516
41.
1329
1817
.74
17.5
611
47.8
079
0.96
6-0
.089
-0.0
71-0
.056
-0.0
34-0
.001
0lm
0690
l244
0077
.939
16-7
2.17
394
1.13
369
17.3
117
.18
2124
.844
80.
989
-0.0
17-0
.03
-0.0
070
-0.0
150.
0020
lm03
25l2
7285
80.1
7272
-67.
2736
31.
1357
5816
.48
16.1
922
62.6
074
0.99
3-0
.012
-0.0
080
-0.0
060
-0.0
050
-0.0
lm00
10k1
5429
79.7
7121
-69.
1549
61.
1369
3116
.89
16.5
712
53.5
933
0.96
6-0
.067
-0.0
51-0
.015
-0.0
35-0
.014
lm03
47l1
9578
83.6
9927
-67.
6055
11.
1387
1317
.23
17.1
421
40.8
425
0.91
0.00
50-0
.128
0.00
50-0
.082
0.00
20lm
0292
k211
0174
.103
71-6
6.77
125
1.13
9525
16.6
316
.40
2554
.658
50.
932
0.00
50-0
.081
-0.0
-0.0
33-0
.0lm
0556
m19
867
75.7
9527
-71.
6337
41.
1395
2717
.52
17.3
648
1.68
310.
967
-0.0
21-0
.046
-0.0
060
-0.0
12-0
.001
0lm
0214
n961
682
.929
61-6
8.56
501
1.14
3016
17.4
417
.42
1538
.656
40.
918
-0.0
020
-0.1
43-0
.003
0-0
.091
0.00
10lm
0245
k790
888
.849
47-6
8.40
236
1.14
3467
17.5
417
.45
781.
7629
0.93
3-0
.005
0-0
.088
0.00
10-0
.045
0.00
40lm
0455
l556
780
.565
19-6
5.73
801
1.14
3775
16.4
816
.23
1290
.530
70.
992
0.00
30-0
.079
0.00
40-0
.054
-0.0
030
lm05
61n1
8106
78.6
9971
-70.
7047
31.
1438
3916
.36
16.0
911
26.6
240
0.96
7-0
.01
-0.0
63-0
.008
0-0
.039
-0.0
020
lm02
17n1
4277
*84
.044
76-6
8.95
735
1.14
7572
16.3
316
.20
2320
.672
80.
957
-0.0
39-0
.059
-0.0
1-0
.018
-0.0
010
lm04
67m
6802
82.5
8253
-65.
9442
31.
1478
0216
.09
15.8
578
9.69
180.
929
-0.1
52-0
.102
-0.0
63-0
.031
0.00
70lm
0417
n935
874
.246
17-6
6.11
689
1.14
811
17.3
017
.03
2311
.612
40.
948
-0.0
17-0
.053
-0.0
-0.0
070
-0.0
020
lm05
71l2
4463
80.5
5512
-70.
7443
91.
1486
2817
.77
17.5
511
50.6
653
0.97
3-0
.01
-0.0
53-0
.005
0-0
.029
0.00
20lm
0031
n172
2485
.523
1-6
9.37
412
1.14
893
16.5
116
.32
342.
8286
0.92
8-0
.016
-0.0
9-0
.006
0-0
.033
-0.0
010
lm02
25l1
2189
85.2
0969
-68.
5813
21.
1574
2217
.33
17.2
315
32.6
827
0.97
8-0
.011
-0.0
19-0
.003
00.
0010
0.0
lm00
33m
2670
885
.356
76-6
9.56
066
1.15
8284
17.1
617
.10
1997
.584
30.
982
-0.0
18-0
.047
-0.0
070
-0.0
28-0
.0lm
0575
n110
5380
.843
22-7
1.43
955
1.16
016
17.3
517
.16
1819
.752
40.
965
-0.0
14-0
.046
-0.0
040
-0.0
29-0
.001
0lm
0014
l200
5480
.081
12-7
0.03
237
1.16
0262
17.8
417
.65
1272
.592
10.
93-0
.041
-0.0
7-0
.004
0-0
.025
0.00
20lm
0466
l192
4281
.408
84-6
6.19
533
1.16
3589
17.4
617
.37
2016
.548
20.
975
-0.0
16-0
.026
-0.0
080
-0.0
110.
0020
lm02
83n1
4097
73.3
2353
-66.
8400
71.
1640
5117
.07
16.9
519
48.6
386
0.92
80.
011
-0.1
310.
0-0
.091
-0.0
010
lm05
35n1
1277
72.4
2784
-71.
4727
91.
1684
4917
.09
17.0
315
63.5
932
0.97
9-0
.017
-0.0
31-0
.008
0-0
.014
-0.0
020
lm01
21l1
6803
73.2
0193
-69.
2999
71.
1700
2116
.85
16.9
212
76.4
939
0.98
1-0
.006
0-0
.038
-0.0
020
-0.0
21-0
.001
0lm
0356
n959
184
.766
04-6
7.51
859
1.17
3114
17.3
817
.26
2018
.569
90.
889
-0.0
030
-0.1
47-0
.006
0-0
.059
0.00
20lm
0103
l139
5177
.215
49-6
9.63
018
1.17
4507
16.7
816
.66
388.
8527
0.91
2-0
.027
-0.1
2-0
.012
-0.0
44-0
.003
0lm
0226
n241
6884
.662
96-6
9.02
808
1.17
6008
16.2
015
.99
1453
.863
70.
944
0.00
90-0
.086
0.00
20-0
.047
-0.0
060
lm04
57l1
9060
80.3
0501
-66.
2145
31.
1761
0817
.40
17.2
214
79.6
849
0.96
1-0
.006
0-0
.052
-0.0
-0.0
340.
0020
lm02
11k1
9128
83.4
5113
-67.
7665
21.
1782
6417
.67
17.3
611
17.6
979
0.94
4-0
.029
-0.0
79-0
.008
0-0
.042
-0.0
030
lm02
14m
2903
382
.841
72-6
8.52
601
1.17
8663
16.5
416
.60
2072
.458
70.
925
-0.0
040
-0.1
-0.0
040
-0.0
660.
0050
lm05
40l2
2424
72.8
5002
-70.
7602
91.
1818
8117
.14
16.9
914
64.6
401
0.92
1-0
.002
0-0
.12
0.00
10-0
.07
0.0
lm03
03l2
3428
76.8
0088
-66.
8860
91.
1836
6917
.71
17.6
113
83.8
448
0.88
3-0
.054
-0.1
63-0
.025
-0.0
670.
0030
lm00
21k2
2831
82.8
9536
-69.
1894
11.
1845
3917
.05
17.0
393
1.47
170.
967
0.00
50-0
.062
0.00
30-0
.036
-0.0
030
lm02
01k1
0778
81.5
9068
-67.
7074
1.18
7596
17.7
417
.71
780.
8087
0.97
-0.0
090
-0.0
4-0
.002
0-0
.03
-0.0
010
lm03
12k1
5523
77.4
8035
-66.
7319
41.
1881
1717
.51
17.5
217
64.8
517
0.95
6-0
.023
-0.0
51-0
.007
0-0
.012
-0.0
155
lm01
14m
2789
974
.302
06-6
9.91
214
1.19
1167
16.8
916
.81
2009
.540
90.
942
0.00
20-0
.078
-0.0
030
-0.0
480.
0020
lm02
00k1
9885
80.4
2683
-67.
8309
21.
1914
8317
.40
17.4
121
93.7
733
0.94
-0.0
32-0
.065
-0.0
040
-0.0
14-0
.005
0lm
0120
n612
472
.418
07-6
9.23
849
1.19
1658
16.4
716
.31
1071
.742
70.
958
-0.0
12-0
.036
-0.0
-0.0
050
0.0
lm03
66k1
0436
86.2
3861
-67.
3747
41.
1933
4616
.52
16.2
819
41.7
860
0.91
4-0
.012
-0.1
53-0
.01
-0.0
87-0
.003
0lm
0165
m30
398
74.7
6377
-68.
5201
61.
1936
417
.37
17.0
844
2.81
820.
965
-0.0
14-0
.044
-0.0
070
-0.0
240.
0050
lm00
44k3
974
86.1
2024
-69.
7789
31.
1936
816
.19
16.0
919
41.6
268
0.96
1-0
.013
-0.0
46-0
.002
0-0
.003
00.
0lm
0344
m18
5083
.064
17-6
6.96
759
1.19
3709
16.3
016
.11
1129
.748
10.
946
-0.0
060
-0.0
65-0
.003
0-0
.038
0.00
10lm
0121
k249
2272
.807
62-6
9.22
294
1.19
5194
15.9
015
.79
1281
.514
90.
941
-0.0
17-0
.061
-0.0
040
-0.0
12-0
.002
0lm
0471
m36
3184
.126
83-6
5.00
347
1.19
5592
17.6
817
.44
1751
.924
40.
862
-0.0
52-0
.127
-0.0
090
-0.0
050
0.01
3lm
0210
n255
6883
.094
13-6
7.96
484
1.19
6126
17.3
217
.12
2000
.563
80.
961
-0.0
24-0
.043
-0.0
020
-0.0
050
0.00
30lm
0193
l102
6279
.739
84-6
8.21
21.
2009
917
.30
17.1
117
50.8
674
0.97
1-0
.065
-0.0
59-0
.02
-0.0
440.
0070
lm01
23m
1977
973
.332
47-6
9.51
175
1.20
2701
17.1
117
.13
2187
.649
20.
978
-0.0
12-0
.045
-0.0
080
-0.0
28-0
.0lm
0214
n253
9382
.796
08-6
8.66
299
1.20
5505
17.3
817
.37
494.
5888
0.96
9-0
.01
-0.0
51-0
.001
0-0
.031
-0.0
010
lm01
00m
7540
76.2
7001
-69.
0982
61.
2062
1717
.43
17.3
320
03.5
390
0.93
6-0
.041
-0.0
97-0
.013
-0.0
31-0
.006
0lm
0115
n144
6375
.733
43-6
9.98
184
1.20
6817
.13
16.9
419
62.6
879
0.95
9-0
.007
0-0
.071
0.00
20-0
.034
0.0
lm02
90m
1223
674
.277
58-6
6.33
021
1.20
6866
16.8
016
.84
949.
4763
0.96
6-0
.017
-0.0
45-0
.002
0-0
.017
0.00
10lm
0286
l230
8172
.098
21-6
7.61
777
1.20
7038
17.4
917
.21
1899
.727
90.
879
-0.0
42-0
.125
-0.0
16-0
.048
0.0
lm03
73m
2039
589
.298
-66.
7384
91.
2076
7217
.88
17.7
716
06.6
476
0.93
6-0
.043
-0.0
88-0
.016
-0.0
2-0
.001
0lm
0230
m92
5986
.430
74-6
7.71
334
1.20
7767
17.6
717
.49
1620
.674
00.
871
-0.0
6-0
.16
-0.0
2-0
.072
-0.0
010
lm01
93n5
944
80.2
5679
-68.
1829
31.
2077
7517
.54
17.4
519
29.6
674
0.86
7-0
.054
-0.1
69-0
.021
-0.0
68-0
.0lm
0316
k135
9777
.610
99-6
7.39
053
1.20
9809
16.4
816
.25
1874
.623
50.
981
-0.0
080
-0.0
16-0
.001
0-0
.00.
0010
lm05
40k2
2686
72.9
5889
-70.
6023
81.
2107
0817
.84
17.6
416
27.5
133
0.98
-0.0
17-0
.046
-0.0
090
-0.0
350.
0010
lm03
02n1
2595
76.3
274
-66.
8322
31.
2131
5117
.18
16.8
915
31.6
134
0.92
6-0
.01
-0.0
3-0
.002
0-0
.017
0.00
90lm
0030
n681
584
.470
05-6
9.39
718
1.21
3239
16.4
016
.27
818.
8345
0.93
7-0
.025
-0.0
71-0
.006
0-0
.015
0.00
30lm
0167
l208
7974
.064
04-6
9.00
567
1.21
3472
17.0
516
.83
760.
7172
0.93
7-0
.005
0-0
.117
-0.0
030
-0.0
73-0
.002
0lm
0290
m76
5174
.332
92-6
6.29
643
1.21
3756
17.4
617
.64
459.
7105
0.89
6-0
.003
0-0
.14
-0.0
010
-0.0
73-0
.003
0lm
0255
m21
132
91.1
7064
-68.
5159
21.
2139
9417
.74
17.5
718
28.8
639
0.89
9-0
.002
0-0
.132
-0.0
010
-0.0
69-0
.001
0lm
0352
l241
1284
.587
5-6
6.92
691
1.21
4317
17.6
317
.43
1812
.767
90.
901
-0.0
010
-0.1
40.
0020
-0.0
630.
0040
lm00
33l8
069
84.9
8061
-69.
6016
81.
2150
3916
.80
16.9
118
83.7
074
0.94
9-0
.011
-0.0
71-0
.004
0-0
.038
0.00
40lm
0423
m21
313
75.7
7782
-65.
3418
41.
2157
417
.68
17.5
212
79.5
999
0.97
40.
03-0
.006
0-0
.006
00.
0090
0.02
4lm
0553
l264
2775
.934
62-7
1.10
917
1.21
6011
16.2
316
.11
1284
.512
00.
952
-0.0
15-0
.045
-0.0
010
-0.0
0.00
10lm
0240
l139
4087
.988
11-6
7.89
771
1.22
005
17.3
817
.26
2256
.649
50.
984
-0.0
28-0
.023
-0.0
070
-0.0
11-0
.002
0lm
0352
l116
3484
.540
92-6
6.83
952
1.22
1534
17.6
417
.46
2346
.661
00.
955
-0.0
19-0
.047
-0.0
070
-0.0
14-0
.001
0lm
0343
m24
594
84.0
397
-66.
7512
71.
2220
6317
.60
17.4
217
74.9
006
0.95
6-0
.016
-0.0
36-0
.001
0-0
.001
00.
0010
lm03
43l2
7142
83.7
4179
-66.
9221
11.
2243
617
.46
17.3
412
71.5
780
0.95
50.
0080
-0.0
630.
0020
-0.0
28-0
.001
0lm
0552
n281
0275
.408
52-7
1.12
939
1.22
4882
17.6
117
.44
1836
.681
00.
973
-0.0
12-0
.064
-0.0
060
-0.0
34-0
.004
0lm
0025
l199
4083
.133
71-7
0.01
572
1.22
5202
17.6
417
.61
1305
.549
70.
976
-0.0
18-0
.036
-0.0
070
-0.0
170.
0050
lm03
46l1
3640
82.5
6262
-67.
5497
91.
2253
1616
.41
16.1
719
53.7
492
0.93
5-0
.009
0-0
.113
-0.0
060
-0.0
59-0
.002
0lm
0200
l205
6180
.503
97-6
7.94
531.
2258
5216
.01
15.7
912
59.5
936
0.93
5-0
.02
-0.0
81-0
.009
0-0
.03
0.00
40lm
0191
k123
0679
.849
-67.
7135
11.
2260
2417
.34
17.0
682
8.67
581.
006
-0.0
28-0
.06
-0.0
040
-0.0
39-0
.007
0lm
0184
n225
6377
.173
64-6
8.63
574
1.22
6475
17.4
517
.30
2185
.858
20.
929
-0.0
45-0
.1-0
.011
-0.0
42-0
.006
0
156
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0304
n298
4276
.165
02-6
7.29
102
1.22
9024
16.6
416
.32
1476
.653
90.
902
-0.0
16-0
.148
-0.0
090
-0.0
870.
0060
lm01
00l2
2131
75.9
6004
-69.
3549
31.
2293
7117
.53
17.4
019
45.6
895
0.89
4-0
.061
-0.1
45-0
.023
-0.0
64-0
.0lm
0452
m16
067
79.9
2772
-65.
338
1.22
9623
16.5
016
.31
826.
7593
0.94
9-0
.015
-0.0
53-0
.002
0-0
.003
00.
0030
lm03
44m
8364
83.3
4386
-67.
0099
1.23
1791
17.6
617
.58
1184
.691
30.
96-0
.018
-0.0
58-0
.013
-0.0
39-0
.001
0lm
0347
k206
2883
.760
59-6
7.44
287
1.23
1871
16.5
716
.38
2255
.669
10.
992
-0.0
040
-0.0
12-0
.0-0
.008
00.
0010
lm00
90m
2646
678
.635
57-6
9.20
741
1.23
2396
17.2
316
.97
1881
.641
60.
877
0.00
10-0
.19
-0.0
030
-0.0
960.
0010
lm02
52l2
2660
90.1
5279
-68.
3259
91.
2336
3817
.15
16.9
783
5.81
100.
877
-0.0
070
-0.1
82-0
.006
0-0
.073
0.00
80lm
0336
m21
470
81.5
9424
-67.
4457
61.
2360
9617
.43
17.2
219
74.6
066
0.94
4-0
.011
-0.0
9-0
.005
0-0
.068
0.00
70lm
0343
m18
540
84.1
7664
-66.
7115
21.
2373
3616
.56
16.2
519
40.7
662
0.95
1-0
.007
0-0
.071
-0.0
020
-0.0
51-0
.004
0lm
0157
n721
772
.681
38-6
8.89
908
1.23
7435
16.3
916
.15
435.
8342
0.89
-0.0
26-0
.145
-0.0
1-0
.043
-0.0
030
lm02
22n4
768
84.5
9285
-68.
1869
91.
2383
9217
.19
17.1
215
78.6
544
0.92
40.
011
-0.1
270.
0070
-0.0
74-0
.008
0lm
0344
l595
982
.618
7-6
7.14
957
1.24
0057
17.3
017
.09
1187
.699
90.
947
-0.0
010
-0.1
07-0
.009
0-0
.076
-0.0
040
lm00
90m
1364
778
.284
54-6
9.13
381
1.24
0532
16.8
716
.73
1503
.656
30.
922
-0.0
050
-0.1
23-0
.003
0-0
.078
-0.0
020
lm00
95l3
2222
78.8
8433
-70.
0863
41.
2428
4917
.75
17.6
112
24.6
295
0.94
8-0
.003
0-0
.109
-0.0
050
-0.0
680.
0050
lm01
10l8
980
73.8
8764
-69.
2616
91.
2440
616
.78
16.5
412
10.6
036
0.89
8-0
.021
-0.1
49-0
.007
0-0
.067
0.00
60lm
0175
m17
458
76.5
3673
-68.
4479
11.
2448
9716
.47
16.2
211
50.6
119
0.95
3-0
.014
-0.0
53-0
.003
0-0
.011
-0.0
lm03
03n1
0523
77.2
0164
-66.
8071
21.
2463
2117
.89
17.6
519
36.6
491
0.90
7-0
.006
0-0
.143
-0.0
050
-0.0
45-0
.0lm
0276
k139
8293
.837
65-6
8.80
429
1.24
7657
17.1
516
.93
1786
.912
70.
855
-0.0
49-0
.145
-0.0
2-0
.05
0.00
20lm
0294
l782
574
.046
49-6
7.15
764
1.24
8422
16.5
316
.33
1775
.778
30.
969
-0.0
16-0
.024
0.00
200.
0010
0.00
20lm
0342
n240
0282
.995
53-6
6.92
396
1.24
847
17.4
917
.24
1114
.761
30.
984
-0.0
4-0
.027
-0.0
22-0
.016
-0.0
020
lm05
51n1
8330
76.5
7531
-70.
7105
41.
2491
2716
.58
16.2
817
61.8
763
0.96
40.
0030
-0.0
550.
0010
-0.0
360.
0070
lm03
43n2
5612
83.8
4745
-66.
9110
21.
2496
5317
.38
17.2
479
2.75
700.
991
-0.0
21-0
.018
-0.0
070
-0.0
120.
0020
lm03
04n2
4921
75.9
9117
-67.
2605
61.
2499
8516
.56
16.2
916
28.5
280
0.96
3-0
.006
0-0
.052
0.0
-0.0
320.
0030
lm02
14n7
884
82.8
0062
-68.
5543
91.
2503
0517
.07
16.8
819
37.7
049
0.92
7-0
.02
-0.1
05-0
.007
0-0
.056
0.01
lm00
44l2
4715
85.9
8352
-70.
0618
51.
2514
6317
.73
17.7
713
88.8
593
0.94
-0.0
3-0
.068
-0.0
11-0
.01
0.01
1lm
0322
m43
8679
.718
01-6
6.62
687
1.25
4285
17.8
317
.68
2018
.540
00.
989
-0.0
37-0
.017
-0.0
17-0
.014
0.00
50lm
0020
m14
007
82.4
4224
-69.
1412
81.
2565
1816
.99
17.1
514
48.7
009
0.93
-0.0
060
-0.0
86-0
.006
0-0
.053
0.00
20lm
0182
l131
9176
.987
15-6
8.23
504
1.25
6523
17.1
416
.88
2198
.654
70.
871
-0.0
48-0
.19
-0.0
31-0
.09
-0.0
020
lm02
90m
1911
174
.205
15-6
6.38
201
1.25
7556
16.1
415
.85
2199
.797
60.
971
-0.0
15-0
.04
-0.0
040
-0.0
150.
0010
lm03
25m
1576
880
.752
34-6
7.04
384
1.26
0551
16.8
916
.59
434.
7552
0.97
1-0
.014
-0.0
280.
0020
0.00
10-0
.002
0lm
0283
m24
518
73.5
2331
-66.
7657
1.26
0717
16.1
715
.93
1777
.773
90.
935
-0.0
25-0
.094
-0.0
090
-0.0
570.
0020
lm00
54l5
210
87.7
6585
-69.
9396
11.
2618
3616
.38
16.1
813
17.5
507
0.95
1-0
.018
-0.0
6-0
.006
0-0
.017
0.00
30lm
0343
l259
1283
.711
14-6
6.91
478
1.26
4852
16.0
315
.85
1266
.609
40.
985
-0.0
16-0
.024
-0.0
060
-0.0
110.
0lm
0110
l132
8873
.852
5-6
9.29
033
1.27
1404
16.1
715
.96
1306
.500
30.
972
-0.0
2-0
.052
-0.0
060
-0.0
31-0
.0lm
0671
l505
674
.580
04-7
2.12
418
1.27
1916
17.8
317
.76
1856
.608
30.
969
-0.0
39-0
.057
-0.0
19-0
.036
0.00
30lm
0253
l835
590
.851
1-6
8.34
826
1.27
4284
17.4
717
.39
1759
.902
20.
935
-0.0
51-0
.088
-0.0
18-0
.032
-0.0
050
lm04
36k8
952
76.3
6602
-65.
9675
41.
2755
9617
.75
17.6
020
21.5
603
0.99
-0.0
59-0
.02
-0.0
12-0
.005
0-0
.01
lm02
14m
2985
882
.792
06-6
8.53
141
1.27
9218
17.3
617
.35
2008
.563
90.
953
-0.0
080
-0.0
66-0
.003
0-0
.042
0.00
20lm
0555
m12
064
76.7
5923
-71.
2361
51.
2798
4816
.15
15.8
621
86.6
970
0.88
-0.0
17-0
.073
-0.0
030
-0.0
130.
0050
lm05
83m
2571
282
.933
24-7
0.93
984
1.28
0423
17.0
517
.09
2183
.776
20.
951
-0.0
26-0
.06
-0.0
11-0
.026
0.00
40lm
0595
n912
685
.454
16-7
1.35
427
1.28
2031
16.3
116
.18
1388
.856
00.
984
-0.0
020
-0.0
34-0
.002
0-0
.02
0.0
157
lm00
50l9
127
88.1
6042
-69.
2585
81.
2830
1517
.94
17.7
618
62.7
808
0.95
1-0
.049
-0.1
1-0
.014
-0.0
5-0
.003
0lm
0012
m20
602
80.6
4068
-69.
5489
81.
2841
0117
.65
17.2
911
38.8
386
0.94
1-0
.002
0-0
.146
-0.0
030
-0.0
94-0
.003
0lm
0197
n195
3480
.181
87-6
8.98
964
1.28
4845
17.6
217
.26
1933
.738
00.
896
0.00
30-0
.188
0.00
60-0
.101
-0.0
070
lm03
54l1
7529
84.6
4993
-67.
2259
1.28
8998
17.9
417
.82
1181
.793
50.
906
-0.0
76-0
.162
-0.0
38-0
.081
0.00
10lm
0017
m17
883
81.7
5557
-70.
2145
71.
2899
6717
.21
17.3
014
80.8
179
0.98
2-0
.016
-0.0
31-0
.006
0-0
.012
0.00
20lm
0343
k105
3983
.439
29-6
6.66
403
1.29
1479
17.8
117
.75
1597
.662
20.
902
-0.0
27-0
.09
-0.0
12-0
.007
00.
0030
lm02
93l1
4089
74.9
9618
-66.
8347
81.
2920
417
.72
17.5
418
42.8
031
0.98
10.
0050
-0.0
260.
0-0
.019
-0.0
010
lm00
30k6
634
84.0
2922
-69.
0985
1.29
3848
16.1
816
.06
1808
.853
50.
879
-0.0
3-0
.137
-0.0
080
-0.0
440.
0010
lm03
66k1
9655
86.1
4187
-67.
4436
31.
2954
7116
.85
16.6
714
43.7
901
0.86
7-0
.058
-0.1
83-0
.036
-0.0
90.
0050
lm03
51m
7030
85.9
5719
-66.
2857
21.
2961
5316
.49
16.2
755
6.59
730.
976
0.00
10-0
.038
-0.0
020
-0.0
250.
0010
lm01
84k1
1257
76.9
6216
-68.
4233
91.
2978
7516
.95
16.8
414
55.7
438
0.97
8-0
.012
-0.0
22-0
.007
0-0
.013
0.00
10lm
0134
m16
531
70.3
6211
-69.
8530
91.
2984
1616
.83
16.7
518
74.5
483
0.96
6-0
.015
-0.0
35-0
.002
00.
0010
-0.0
030
lm02
20n2
0494
84.7
732
-67.
9360
21.
2991
8317
.16
17.0
112
62.5
922
0.94
6-0
.022
-0.0
6-0
.005
0-0
.007
00.
0040
lm03
45k2
244
83.6
8146
-66.
9685
81.
3010
8516
.48
16.3
315
11.7
218
0.94
6-0
.016
-0.0
8-0
.009
0-0
.039
-0.0
030
lm02
07l9
702
81.6
2493
-68.
9232
81.
3027
5316
.36
16.2
914
44.7
445
0.97
-0.0
11-0
.038
-0.0
040
-0.0
2-0
.004
0lm
0200
l209
5280
.520
18-6
7.94
839
1.30
4803
16.3
916
.16
2029
.486
70.
917
-0.0
22-0
.122
-0.0
070
-0.0
64-0
.002
0lm
0313
k266
2278
.360
45-6
6.75
854
1.30
5016
17.4
417
.29
2310
.659
60.
934
-0.0
050
-0.1
29-0
.003
0-0
.09
0.00
20lm
0122
n218
0972
.586
73-6
9.70
246
1.30
534
16.4
916
.25
2356
.561
90.
946
0.00
20-0
.077
0.00
10-0
.038
-0.0
lm00
33k1
6643
84.8
3539
-69.
5019
41.
3057
4315
.79
15.7
316
29.6
272
0.94
5-0
.024
-0.0
82-0
.009
0-0
.044
0.0
lm00
33k2
8357
84.9
2359
-69.
5735
41.
3068
4115
.88
15.7
723
50.6
233
0.88
1-0
.017
-0.1
51-0
.009
0-0
.066
0.00
20lm
0313
k253
7178
.469
32-6
6.75
051.
3073
0617
.71
17.6
053
9.53
050.
955
0.00
20-0
.076
-0.0
-0.0
550.
0010
lm02
21m
2641
885
.521
84-6
7.81
625
1.30
898
17.4
517
.34
1538
.683
40.
941
0.00
20-0
.07
-0.0
040
-0.0
43-0
.001
0lm
0632
l197
3692
.18
-71.
1302
31.
3097
716
.95
16.7
914
93.8
556
0.92
5-0
.038
-0.1
04-0
.013
-0.0
53-0
.0lm
0344
k452
582
.802
74-6
6.98
583
1.31
0804
16.6
816
.51
802.
8137
0.93
9-0
.015
-0.0
81-0
.008
0-0
.041
-0.0
010
lm03
45k7
107
83.7
232
-67.
0005
61.
3110
4216
.12
15.9
111
52.8
469
0.94
4-0
.003
0-0
.09
0.00
20-0
.046
-0.0
040
lm01
90n1
4623
79.1
1976
-67.
8913
81.
3116
5715
.87
15.6
311
95.6
954
0.84
7-0
.02
-0.2
05-0
.008
0-0
.071
-0.0
lm03
44m
5728
83.1
9564
-66.
9930
31.
3127
9317
.08
16.9
048
9.63
830.
932
-0.0
070
-0.1
150.
0020
-0.0
770.
0010
lm05
51m
1650
476
.628
32-7
0.55
247
1.31
4528
16.6
416
.27
423.
6287
0.94
4-0
.025
-0.0
79-0
.012
-0.0
40.
0020
lm05
70l6
310
79.1
5194
-70.
6397
41.
3147
3717
.66
17.5
018
70.6
559
0.93
7-0
.004
0-0
.064
-0.0
060
-0.0
43-0
.001
0lm
0323
l773
880
.259
7-6
6.79
721.
3152
2416
.99
16.8
913
04.4
933
0.98
4-0
.011
-0.0
43-0
.002
0-0
.036
0.0
lm05
95m
2515
485
.297
65-7
1.29
029
1.31
7016
17.5
917
.74
2227
.659
60.
972
-0.0
020
-0.0
67-0
.002
0-0
.046
0.00
20lm
0321
m13
358
80.3
4625
-66.
3294
71.
3182
117
.46
17.1
619
59.6
417
0.93
5-0
.005
0-0
.1-0
.002
0-0
.05
0.00
10lm
0551
k190
7876
.015
96-7
0.59
653
1.31
8882
17.3
417
.16
1278
.541
50.
978
-0.0
17-0
.026
-0.0
060
-0.0
11-0
.001
0lm
0466
m23
585
81.4
4584
-66.
0769
41.
3189
5816
.68
16.5
122
50.6
023
0.90
4-0
.039
-0.1
42-0
.012
-0.0
51-0
.001
0lm
0340
n223
8383
.092
96-6
6.55
266
1.31
9689
17.7
617
.62
1476
.741
70.
934
-0.0
040
-0.0
78-0
.002
0-0
.037
0.00
20lm
0366
n145
9386
.898
47-6
7.55
653
1.32
1337
17.7
817
.55
450.
8444
0.93
-0.0
17-0
.091
-0.0
050
-0.0
51-0
.003
0lm
0032
k203
1384
.144
94-6
9.56
391.
3237
9217
.14
17.0
780
2.76
030.
97-0
.004
0-0
.063
-0.0
070
-0.0
510.
0lm
0012
l179
3579
.963
02-6
9.66
736
1.32
3984
16.5
916
.44
1622
.552
10.
929
-0.0
030
-0.1
06-0
.006
0-0
.051
0.00
10lm
0210
m22
011
83.1
1026
-67.
7938
71.
3249
5617
.02
16.8
611
79.7
954
0.87
-0.0
56-0
.184
-0.0
27-0
.079
0.00
10lm
0033
m68
5085
.370
87-6
9.44
069
1.32
799
17.1
717
.03
2009
.524
80.
933
-0.0
090
-0.1
05-0
.005
0-0
.07
0.00
10lm
0343
l597
7*83
.647
48-6
6.79
113
1.32
9154
15.8
215
.64
760.
6928
0.96
5-0
.014
-0.0
39-0
.001
0-0
.007
00.
0010
158
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0175
n261
0776
.527
85-6
8.64
711
1.32
9774
17.5
617
.07
1866
.592
60.
972
0.00
60-0
.078
-0.0
070
-0.0
43-0
.002
0lm
0330
l180
2181
.082
09-6
6.52
792
1.33
0011
16.5
416
.42
1219
.645
90.
962
0.00
40-0
.052
0.00
10-0
.023
0.0
lm03
64l6
843
86.3
1096
-67.
1538
51.
3313
7516
.87
16.6
911
50.7
712
0.89
9-0
.039
-0.1
27-0
.013
-0.0
420.
0070
lm03
24n1
1221
79.5
0773
-67.
1743
91.
3342
2716
.89
16.7
718
42.8
412
0.99
5-0
.025
-0.0
030
-0.0
060
-0.0
020
0.00
20lm
0701
k237
7981
.551
07-7
1.99
519
1.33
4253
17.0
216
.86
1496
.681
30.
962
-0.0
010
-0.0
650.
0-0
.046
-0.0
010
lm01
75k1
8907
75.8
0158
-68.
4579
1.33
5629
16.0
215
.96
1447
.754
50.
98-0
.004
0-0
.02
-0.0
030
-0.0
050
0.00
40lm
0110
m24
838
74.6
0204
-69.
1989
81.
3374
5816
.65
16.1
111
98.6
206
0.88
1-0
.043
-0.1
61-0
.016
-0.0
740.
0030
lm02
10k2
4451
82.3
372
-67.
8214
81.
3374
6816
.71
16.5
323
24.6
279
0.89
8-0
.02
-0.1
08-0
.008
0-0
.033
0.00
10lm
0587
n193
8582
.931
65-7
1.78
783
1.33
9509
16.7
216
.65
792.
6937
0.93
9-0
.032
-0.0
94-0
.011
-0.0
450.
0lm
0056
n227
3588
.608
05-7
0.40
959
1.34
1028
16.8
316
.65
2240
.855
60.
941
0.00
50-0
.09
0.0
-0.0
47-0
.001
0lm
0012
l193
9680
.177
63-6
9.67
576
1.34
2001
16.5
816
.17
1528
.660
40.
923
-0.0
2-0
.082
-0.0
040
-0.0
180.
0010
lm00
45n2
7451
87.4
8414
-70.
0613
21.
3427
316
.22
15.9
014
78.7
717
0.95
4-0
.021
-0.0
67-0
.013
-0.0
37-0
.004
0lm
0125
m17
447
73.7
3964
-69.
8470
91.
3430
6117
.76
17.6
821
84.6
421
0.92
6-0
.046
-0.0
91-0
.012
-0.0
39-0
.001
0lm
0032
m19
079
84.2
3338
-69.
5523
51.
3442
1416
.41
16.2
583
3.79
560.
952
-0.0
080
-0.0
57-0
.004
0-0
.022
-0.0
010
lm00
90k1
5522
77.8
3539
-69.
1541
51.
3452
3917
.16
17.3
359
6.46
830.
931
-0.0
090
-0.0
98-0
.005
0-0
.058
-0.0
lm04
24k1
2950
74.7
7183
-65.
6399
31.
3454
9816
.39
16.1
921
84.6
886
0.97
9-0
.01
-0.0
21-0
.005
0-0
.007
00.
0010
lm05
57n1
6353
76.7
8602
-71.
7722
81.
3469
9617
.01
16.8
011
96.5
924
0.93
1-0
.026
-0.0
82-0
.007
0-0
.017
0.00
20lm
0091
l131
4179
.184
65-6
9.27
812
1.34
7207
16.9
116
.91
1903
.589
90.
925
-0.0
1-0
.1-0
.009
0-0
.052
-0.0
010
lm00
40k2
5840
85.8
8344
-69.
2279
51.
3528
1917
.77
17.6
022
28.8
571
0.94
5-0
.016
-0.0
99-0
.008
0-0
.062
-0.0
010
lm00
95n2
1786
79.3
5908
-70.
0243
1.35
5226
17.3
917
.34
2263
.645
90.
883
-0.0
48-0
.141
-0.0
23-0
.046
-0.0
030
lm00
33l1
2538
85.1
8187
-69.
6284
81.
3562
6117
.03
17.1
066
3.93
310.
977
-0.0
010
-0.0
41-0
.001
0-0
.031
-0.0
010
lm01
62l1
1792
73.1
5868
-68.
2297
11.
3563
8317
.47
17.4
217
63.7
818
0.97
7-0
.014
-0.0
35-0
.009
0-0
.009
00.
0lm
0020
m26
7582
.414
69-6
9.06
903
1.35
6457
17.2
117
.00
1439
.776
80.
932
-0.0
040
-0.1
310.
0010
-0.0
88-0
.004
0lm
0225
k231
6685
.099
11-6
8.49
51.
3575
1916
.52
16.3
912
11.7
171
0.87
1-0
.002
0-0
.167
-0.0
010
-0.0
560.
0020
lm05
41n1
0909
74.4
1288
-70.
6943
41.
3578
1817
.91
17.7
014
76.6
226
0.96
8-0
.013
-0.0
5-0
.008
0-0
.038
0.00
10lm
0122
n147
3072
.596
75-6
9.65
419
1.35
9095
17.4
417
.26
2227
.564
50.
971
-0.0
18-0
.041
0.00
10-0
.004
00.
0020
lm00
33l2
0481
85.1
2016
-69.
6773
41.
3599
6117
.11
17.2
818
88.7
095
0.94
8-0
.017
-0.0
46-0
.002
0-0
.008
00.
0020
lm02
25m
4465
85.9
3241
-68.
3747
81.
3606
3416
.37
16.1
519
52.6
404
0.95
8-0
.001
0-0
.073
-0.0
070
-0.0
46-0
.002
0lm
0325
k818
480
.162
87-6
7.00
164
1.36
1238
16.2
516
.09
2223
.829
50.
959
-0.0
12-0
.044
-0.0
010
-0.0
090
0.00
10lm
0164
n109
4373
.532
5-6
8.57
395
1.36
2005
16.5
816
.38
1851
.586
80.
972
-0.0
29-0
.035
-0.0
070
-0.0
170.
0020
lm03
06m
1121
876
.160
53-6
7.36
918
1.36
289
16.8
716
.65
2233
.825
80.
935
-0.0
17-0
.071
-0.0
050
-0.0
17-0
.0lm
0167
n661
974
.392
94-6
8.90
038
1.36
3124
17.5
017
.26
434.
7245
0.93
5-0
.005
0-0
.077
0.00
30-0
.048
-0.0
050
lm03
31n1
1495
82.3
3892
-66.
5626
61.
3631
6515
.84
15.5
421
68.7
479
0.85
6-0
.037
-0.1
86-0
.012
-0.0
660.
0lm
0055
m20
627
89.4
7672
-69.
8823
61.
3653
1217
.43
17.2
620
20.6
020
0.97
8-0
.02
-0.0
22-0
.002
0-0
.001
00.
0010
lm03
26k1
5236
79.2
7837
-67.
3988
81.
3657
0217
.77
17.7
222
36.5
552
0.96
4-0
.024
-0.0
240.
0010
-0.0
020
0.01
1lm
0292
k470
574
.026
2-6
6.63
217
1.36
6304
17.6
717
.53
1973
.570
20.
956
-0.0
12-0
.06
-0.0
060
-0.0
42-0
.0lm
0610
k122
888
.045
73-7
0.49
025
1.36
879
17.4
817
.34
452.
7291
0.97
6-0
.022
-0.0
23-0
.0-0
.008
00.
0050
lm05
51k2
1201
76.1
7855
-70.
6123
61.
3703
515
.97
15.7
417
69.8
058
0.95
20.
0010
-0.0
60.
0040
-0.0
250.
0010
lm02
16l7
335
82.6
3094
-68.
9099
61.
3703
6717
.28
17.1
815
47.6
934
0.93
9-0
.025
-0.0
64-0
.003
0-0
.015
-0.0
lm03
31l1
2991
81.6
9989
-66.
4870
71.
3704
9217
.56
17.4
217
74.8
883
0.92
7-0
.044
-0.1
08-0
.019
-0.0
46-0
.002
0lm
0587
k638
782
.401
28-7
1.54
306
1.37
2249
17.0
016
.78
1761
.886
50.
985
-0.0
15-0
.024
0.0
-0.0
060
-0.0
020
159
lm05
84k1
4035
81.3
1538
-71.
2356
81.
3727
7716
.40
16.2
467
0.89
050.
966
-0.0
24-0
.025
-0.0
040
-0.0
120.
0030
lm04
26m
6757
75.1
0942
-65.
9426
61.
3727
8516
.54
16.3
232
5.91
020.
99-0
.029
-0.0
16-0
.004
0-0
.013
0.00
10lm
0194
l205
1278
.556
26-6
8.63
336
1.37
3732
16.9
216
.76
2009
.550
60.
977
-0.0
2-0
.036
-0.0
060
-0.0
130.
0040
lm04
85l1
6305
85.5
1608
-65.
8128
61.
3740
2117
.56
17.3
913
98.8
692
0.88
9-0
.072
-0.1
67-0
.022
-0.0
8-0
.0lm
0031
n122
8285
.262
32-6
9.38
275
1.37
5196
16.1
416
.07
1498
.711
20.
901
-0.0
060
-0.1
24-0
.001
0-0
.061
-0.0
010
lm02
95k2
7975
74.8
5443
-67.
1197
21.
3754
8316
.96
16.8
311
47.7
847
0.87
6-0
.034
-0.1
16-0
.008
0-0
.044
0.00
40lm
0575
n394
780
.715
9-7
1.35
661
1.37
5523
16.4
016
.19
825.
8252
0.97
5-0
.006
0-0
.036
-0.0
040
-0.0
23-0
.002
0lm
0186
n256
9977
.465
51-6
9.03
439
1.37
6787
16.9
416
.72
2187
.721
50.
856
-0.0
43-0
.156
-0.0
19-0
.048
0.00
10lm
0285
k397
273
.072
18-6
6.97
331.
3774
8616
.90
16.9
021
30.7
948
0.98
-0.0
11-0
.031
-0.0
040
-0.0
20.
0lm
0315
n682
178
.881
15-6
7.13
714
1.37
8079
17.0
216
.75
2240
.805
20.
979
0.00
30-0
.033
0.00
20-0
.013
0.00
10lm
0601
l272
3486
.711
28-7
0.76
364
1.37
8285
17.7
617
.72
1388
.863
00.
907
-0.0
63-0
.123
-0.0
28-0
.062
0.00
50lm
0010
n998
180
.637
01-6
9.27
116
1.37
9098
16.8
616
.61
2202
.685
50.
979
-0.0
13-0
.034
-0.0
010
-0.0
050
0.00
50lm
0123
k255
5073
.257
35-6
9.54
389
1.37
9496
17.7
517
.75
424.
8026
0.94
5-0
.005
0-0
.083
-0.0
020
-0.0
57-0
.002
0lm
0010
k356
379
.888
56-6
9.07
681
1.38
0453
17.5
317
.36
1306
.539
30.
866
-0.0
55-0
.132
-0.0
030
-0.0
060
0.01
6lm
0161
l222
5374
.140
08-6
7.93
355
1.38
0684
17.2
917
.12
1755
.906
80.
946
0.00
60-0
.073
0.00
20-0
.024
-0.0
040
lm00
33k1
6425
84.8
1241
-69.
5006
71.
3818
4115
.95
15.8
415
49.7
162
0.92
8-0
.003
0-0
.104
0.00
30-0
.064
-0.0
030
lm01
87k2
5395
77.8
1155
-68.
8599
61.
3844
7616
.89
16.8
988
4.57
970.
943
-0.0
050
-0.0
91-0
.003
0-0
.038
0.00
10lm
0033
l898
285
.159
85-6
9.60
625
1.38
4664
17.4
617
.36
2347
.595
70.
959
-0.0
090
-0.0
74-0
.003
0-0
.056
-0.0
020
lm01
21n1
0952
73.6
4131
-69.
2638
11.
3896
3116
.94
16.7
715
03.6
168
0.96
3-0
.01
-0.0
34-0
.007
0-0
.017
-0.0
010
lm00
37n1
5636
85.4
7739
-70.
3667
81.
3899
8717
.71
17.6
314
65.7
833
0.93
6-0
.04
-0.1
1-0
.008
0-0
.038
-0.0
070
lm04
53n1
8119
80.8
885
-65.
4649
81.
3924
8717
.53
17.4
021
60.7
252
1.00
6-0
.027
-0.0
050
-0.0
040
-0.0
030
0.00
40lm
0346
m15
709
83.1
288
-67.
4078
11.
3961
6415
.72
15.5
319
10.7
349
0.99
3-0
.019
-0.0
060
-0.0
050
-0.0
020
0.00
40lm
0337
k241
8781
.788
41-6
7.47
141.
3972
2716
.60
16.3
920
20.5
398
0.98
-0.0
11-0
.04
-0.0
070
-0.0
170.
0020
lm02
17n1
2376
83.9
6639
-68.
9427
91.
3981
9816
.30
16.0
823
27.6
841
0.98
9-0
.008
0-0
.011
-0.0
-0.0
020
0.00
10lm
0110
n112
7074
.411
83-6
9.27
154
1.39
8457
16.5
216
.36
2005
.592
70.
877
-0.0
5-0
.174
-0.0
26-0
.078
0.00
70lm
0127
l204
9873
.217
69-7
0.39
849
1.39
8538
16.8
816
.64
2234
.785
60.
887
-0.0
44-0
.162
-0.0
22-0
.072
0.00
10lm
0040
l120
7086
.005
17-6
9.28
234
1.39
9558
16.8
117
.00
1965
.643
50.
948
-0.0
010
-0.0
64-0
.002
0-0
.039
0.00
10lm
0597
l192
7284
.779
25-7
1.78
888
1.40
2455
16.0
315
.75
1259
.609
40.
861
-0.0
41-0
.183
-0.0
18-0
.062
-0.0
010
lm02
00k2
1051
80.5
6212
-67.
7880
81.
4033
6517
.88
17.6
312
37.6
677
0.96
1-0
.029
-0.0
76-0
.024
-0.0
480.
0080
lm04
57k2
4395
80.2
8756
-66.
0730
31.
4067
117
.81
17.7
215
06.6
956
0.88
7-0
.01
-0.1
60.
0030
-0.0
83-0
.001
0lm
0306
l186
5975
.833
59-6
7.57
889
1.40
7038
17.5
817
.47
1893
.637
80.
97-0
.038
-0.0
4-0
.009
0-0
.019
0.00
10lm
0166
l126
4173
.179
95-6
8.94
171
1.40
8868
17.5
617
.22
1526
.608
00.
982
-0.0
63-0
.044
-0.0
19-0
.041
-0.0
040
lm03
43n2
5594
84.1
3251
-66.
9085
1.40
9684
15.7
915
.50
1885
.701
50.
88-0
.027
-0.1
57-0
.01
-0.0
54-0
.002
0lm
0174
l193
7374
.791
43-6
8.64
692
1.41
0559
17.8
717
.73
1971
.642
80.
93-0
.058
-0.1
04-0
.025
-0.0
40.
01lm
0165
n250
5274
.791
52-6
8.64
701
1.41
0581
17.8
817
.68
2208
.581
50.
913
-0.0
6-0
.119
-0.0
34-0
.057
-0.0
010
lm04
33m
7146
77.4
8491
-65.
2367
91.
4136
4616
.31
16.2
022
59.6
061
0.93
1-0
.03
-0.1
01-0
.012
-0.0
49-0
.002
0lm
0440
m22
885
78.2
8887
-65.
0111
31.
4153
7317
.24
17.0
818
05.8
437
0.91
5-0
.032
-0.0
92-0
.008
0-0
.026
0.00
50lm
0332
l249
8980
.934
09-6
6.92
286
1.41
5919
17.5
517
.44
2160
.734
40.
957
-0.0
030
-0.0
630.
0040
-0.0
40.
0080
lm03
32n2
1956
81.4
9459
-66.
8992
81.
4162
6417
.05
16.9
210
86.8
833
0.93
8-0
.047
-0.0
76-0
.012
-0.0
26-0
.002
0lm
0191
l101
6579
.647
41-6
7.85
672
1.41
8043
16.3
016
.04
1433
.810
40.
884
-0.0
31-0
.151
-0.0
13-0
.048
0.00
10lm
0226
k213
7584
.357
7-6
8.86
111.
4180
5517
.47
17.3
718
75.7
102
0.92
40.
0020
-0.1
320.
0010
-0.0
880.
0060
160
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0033
m14
746
85.3
1466
-69.
4886
41.
4203
4315
.73
15.6
420
53.5
057
0.94
8-0
.017
-0.0
58-0
.005
0-0
.011
0.0
lm01
86n6
732
77.4
6315
-68.
9031
51.
4204
3316
.24
16.2
041
8.83
730.
969
-0.0
22-0
.061
-0.0
050
-0.0
430.
0010
lm01
23n2
3584
73.5
269
-69.
6904
71.
4211
8516
.50
16.2
821
61.7
151
0.98
1-0
.007
0-0
.032
-0.0
020
-0.0
15-0
.0lm
0331
k223
1981
.796
09-6
6.39
641.
4214
8516
.26
16.0
917
64.8
726
0.88
1-0
.048
-0.1
62-0
.018
-0.0
61-0
.001
0lm
0427
k756
975
.483
19-6
5.95
961
1.42
3526
16.5
616
.30
1920
.607
10.
90.
0050
-0.1
530.
0010
-0.0
860.
0010
lm00
90l7
821
78.2
2237
-69.
2583
51.
4254
3317
.63
17.5
014
81.6
316
0.9
-0.0
6-0
.154
-0.0
24-0
.068
0.00
50lm
0454
n540
980
.130
29-6
5.77
294
1.42
6147
16.0
115
.73
760.
8097
0.97
6-0
.006
0-0
.033
-0.0
020
-0.0
10.
0lm
0021
n514
083
.508
23-6
9.22
983
1.42
9287
16.1
715
.98
1977
.651
70.
967
-0.0
15-0
.03
-0.0
0.00
10-0
.0lm
0467
l111
9682
.140
63-6
6.14
551
1.42
9906
16.3
316
.09
1630
.517
80.
937
0.0
-0.0
97-0
.001
0-0
.043
-0.0
lm04
75m
1598
484
.087
21-6
5.64
972
1.43
014
17.3
017
.11
2244
.813
10.
969
-0.0
2-0
.03
-0.0
030
-0.0
040
0.00
10lm
0225
l185
2385
.443
12-6
8.61
931.
4324
8116
.68
16.5
110
93.8
515
0.89
5-0
.0-0
.148
-0.0
010
-0.0
650.
0040
lm00
50m
1166
888
.440
83-6
9.12
669
1.43
2856
16.7
416
.47
2211
.786
00.
981
-0.0
040
-0.0
240.
0020
-0.0
13-0
.003
0lm
0030
m97
4484
.469
97-6
9.16
274
1.43
4738
16.3
116
.38
2320
.691
10.
955
-0.0
23-0
.067
-0.0
080
-0.0
41-0
.002
0lm
0216
m68
0582
.714
99-6
8.74
527
1.43
6319
16.0
315
.91
1253
.616
40.
973
-0.0
020
-0.0
36-0
.0-0
.024
0.0
lm00
80m
5139
94.5
9422
-69.
1927
31.
4364
2717
.89
17.6
622
94.8
690
0.94
4-0
.02
-0.1
15-0
.017
-0.0
76-0
.002
0lm
0336
n625
581
.518
3-6
7.48
752
1.43
8008
16.3
216
.03
1904
.762
30.
923
-0.0
3-0
.136
-0.0
13-0
.087
-0.0
080
lm00
30n5
266
84.2
8567
-69.
2408
61.
4388
4516
.32
16.3
621
83.7
966
0.94
6-0
.01
-0.0
94-0
.003
0-0
.056
-0.0
010
lm03
27m
2371
780
.531
88-6
7.45
696
1.43
9496
15.9
815
.69
1764
.862
50.
968
0.00
10-0
.024
-0.0
-0.0
150.
0010
lm01
11m
6204
75.4
8886
-69.
0791
11.
4399
9916
.97
16.7
282
1.81
730.
955
-0.0
22-0
.037
-0.0
010
-0.0
050
0.00
50lm
0030
n192
7584
.423
19-6
9.33
551
1.44
1502
17.7
917
.65
431.
7545
1.00
6-0
.06
-0.0
27-0
.012
-0.0
250.
0040
lm04
83k1
0155
85.3
4155
-65.
2635
1.44
3148
17.7
817
.68
530.
5960
0.90
80.
0-0
.12
-0.0
040
-0.0
45-0
.001
0lm
0365
k199
1787
.056
24-6
7.08
298
1.44
3952
17.6
817
.58
2211
.771
50.
908
-0.0
14-0
.132
0.00
10-0
.089
0.01
lm02
23l2
0472
85.2
7026
-68.
2747
61.
4469
1817
.25
17.1
718
60.6
640
0.95
3-0
.001
0-0
.056
-0.0
020
-0.0
17-0
.0lm
0101
l489
876
.795
01-6
9.23
651.
4477
9717
.36
17.1
815
91.6
497
0.94
8-0
.052
-0.0
44-0
.025
-0.0
090
-0.0
070
lm01
05l4
144
76.9
2017
-69.
9493
81.
4480
816
.14
15.9
914
68.6
220
0.94
8-0
.03
-0.0
69-0
.007
0-0
.024
0.00
30lm
0424
n177
5874
.858
74-6
5.82
873
1.44
8589
16.5
216
.28
1623
.547
90.
973
-0.0
090
-0.0
39-0
.005
0-0
.028
-0.0
020
lm03
64k1
1532
86.3
7889
-67.
0327
51.
4489
5816
.88
16.8
022
40.6
680
0.96
-0.0
25-0
.056
-0.0
050
-0.0
160.
0lm
0023
m46
35*
83.6
221
-69.
4251
1.45
0334
17.1
616
.92
1506
.716
30.
924
-0.0
47-0
.11
-0.0
14-0
.046
-0.0
020
lm00
30k1
3920
84.0
5815
-69.
1532
31.
4508
2716
.22
16.1
723
05.7
311
0.94
3-0
.015
-0.0
69-0
.007
0-0
.016
0.00
40lm
0040
k259
7885
.984
18-6
9.22
539
1.45
1215
16.4
116
.32
2202
.803
30.
934
-0.0
13-0
.099
-0.0
070
-0.0
60.
0040
lm01
65m
1831
174
.455
11-6
8.45
461.
4521
2216
.60
16.3
983
5.61
150.
898
-0.0
27-0
.141
-0.0
090
-0.0
440.
0lm
0280
l885
172
.270
03-6
6.45
684
1.45
283
17.6
117
.45
2304
.639
50.
944
0.00
30-0
.083
0.0
-0.0
410.
0030
lm04
40l7
192
77.9
1995
-65.
1138
31.
4530
8717
.63
17.5
711
33.6
887
0.98
-0.0
17-0
.017
0.00
10-0
.00.
0080
lm01
51n1
4381
72.5
678
-67.
8850
31.
4531
2217
.49
17.3
422
26.7
864
0.93
7-0
.01
-0.0
79-0
.005
0-0
.021
-0.0
040
lm00
10m
3763
80.2
6873
-69.
0753
41.
4533
3816
.23
15.5
055
5.54
070.
859
-0.0
31-0
.122
-0.0
1-0
.027
-0.0
030
lm03
37k1
9646
81.9
815
-67.
4385
41.
4539
2117
.55
17.3
970
5.75
390.
972
-0.0
2-0
.052
-0.0
11-0
.037
-0.0
020
lm00
95m
1852
579
.432
39-6
9.85
274
1.45
4941
17.2
717
.39
589.
4691
0.97
6-0
.024
-0.0
36-0
.007
0-0
.013
-0.0
020
lm01
80n1
4087
77.2
7753
-67.
9846
51.
4558
7116
.36
16.1
822
43.6
109
0.91
1-0
.034
-0.1
19-0
.012
-0.0
410.
0lm
0090
k113
3377
.984
84-6
9.12
846
1.45
6551
17.5
217
.61
870.
6308
0.95
50.
0060
-0.0
84-0
.001
0-0
.061
-0.0
030
lm01
56n1
4534
71.8
8183
-68.
9428
61.
4571
17.8
217
.67
2237
.552
60.
978
-0.0
11-0
.047
-0.0
060
-0.0
23-0
.006
0lm
0335
m23
184
82.2
4436
-67.
0914
41.
4577
1516
.60
16.3
444
3.61
440.
982
-0.0
26-0
.031
-0.0
090
-0.0
180.
0
161
lm06
05n2
3731
87.5
7283
-71.
4432
91.
4581
4917
.02
17.2
115
80.6
986
0.97
6-0
.04
-0.0
25-0
.022
-0.0
080
0.00
60lm
0315
n192
0278
.609
3-6
7.21
954
1.46
0027
15.8
415
.56
800.
6893
0.97
8-0
.014
-0.0
260.
0-0
.00.
0lm
0021
l146
5083
.198
18-6
9.28
828
1.46
2272
15.7
315
.47
1475
.738
70.
978
-0.0
1-0
.03
-0.0
010
-0.0
050
-0.0
010
lm03
44m
2008
683
.029
73-6
7.08
729
1.46
2707
17.2
417
.08
1576
.696
20.
944
0.00
20-0
.076
-0.0
040
-0.0
510.
0040
lm00
34k9
201
84.1
425
-69.
8144
21.
4639
0216
.55
16.4
013
81.9
065
0.96
8-0
.021
-0.0
37-0
.001
0-0
.005
00.
0020
lm03
35k2
6831
81.7
029
-67.
1175
91.
4647
7417
.45
17.3
438
8.72
340.
964
-0.0
13-0
.057
-0.0
060
-0.0
33-0
.001
0lm
0121
m27
778
73.5
3912
-69.
2162
51.
4651
4617
.26
17.0
448
8.67
620.
963
-0.0
28-0
.062
-0.0
17-0
.045
-0.0
020
lm01
64k2
6049
72.9
875
-68.
5141
31.
4671
6717
.00
16.7
917
50.8
564
0.94
8-0
.014
-0.0
79-0
.005
0-0
.061
0.00
30lm
0165
n173
7874
.574
54-6
8.60
381
1.46
948
17.2
117
.16
795.
6563
0.96
2-0
.033
-0.0
49-0
.006
0-0
.017
-0.0
lm00
33k9
023
85.0
2569
-69.
4535
31.
4699
7616
.33
16.2
221
74.8
031
0.98
4-0
.013
-0.0
24-0
.001
00.
0010
-0.0
020
lm04
55k3
349
80.4
5913
-65.
5717
91.
4701
6617
.16
17.1
315
29.6
556
0.92
2-0
.027
-0.0
81-0
.008
0-0
.009
00.
0050
lm00
92n1
6033
78.6
4-6
9.65
524
1.47
342
15.8
215
.61
811.
8528
0.96
20.
0010
-0.0
45-0
.001
0-0
.02
-0.0
010
lm02
90k1
6764
74.0
6053
-66.
3671
71.
4751
2716
.34
16.1
722
97.6
552
0.98
10.
0030
-0.0
350.
0020
-0.0
230.
0020
lm01
21n2
7034
73.7
4454
-69.
3592
91.
4758
4816
.96
16.7
079
7.65
860.
974
0.00
30-0
.035
0.00
10-0
.022
-0.0
010
lm02
14k2
5540
82.5
5892
-68.
5152
1.47
6843
17.6
017
.54
2240
.624
00.
965
-0.0
11-0
.044
-0.0
040
-0.0
26-0
.004
0lm
0364
n985
586
.495
04-6
7.17
615
1.47
7007
17.6
917
.53
2223
.647
00.
947
-0.0
060
-0.0
780.
0010
-0.0
54-0
.002
0lm
0294
k139
4473
.964
27-6
7.04
175
1.47
8161
17.0
016
.88
1402
.889
80.
93-0
.007
0-0
.119
-0.0
040
-0.0
77-0
.0lm
0020
m14
812
82.5
2879
-69.
1460
81.
4787
2516
.14
15.9
119
17.8
257
0.93
7-0
.025
-0.0
75-0
.006
0-0
.02
0.00
50lm
0173
m22
752
76.3
6809
-68.
1256
51.
4792
3216
.81
16.5
518
88.6
122
0.93
7-0
.011
-0.0
99-0
.009
0-0
.063
0.00
20lm
0173
l292
3375
.898
28-6
8.31
491.
4801
1516
.88
16.7
724
96.8
050
0.98
2-0
.006
0-0
.022
-0.0
080
-0.0
12-0
.001
0lm
0300
k223
3175
.895
9-6
6.40
058
1.48
138
17.9
317
.69
1987
.556
00.
945
-0.0
23-0
.065
-0.0
15-0
.046
0.00
50lm
0041
k251
6286
.989
72-6
9.20
41.
4815
9417
.64
17.6
019
65.6
435
0.91
40.
0020
-0.1
250.
0040
-0.0
6-0
.0lm
0347
l578
083
.529
95-6
7.49
362
1.48
1679
16.0
615
.85
1495
.704
10.
966
-0.0
070
-0.0
53-0
.004
0-0
.036
-0.0
010
lm03
46k1
2896
82.9
3704
-67.
3948
41.
4817
8416
.90
16.9
555
8.55
930.
975
-0.0
1-0
.049
-0.0
1-0
.031
0.00
50lm
0333
m10
861
82.0
787
-66.
6627
1.48
2148
16.0
315
.78
388.
7234
0.98
9-0
.02
-0.0
080
-0.0
080
-0.0
050
0.00
50lm
0556
m65
25*
75.6
8396
-71.
5356
61.
4934
938
16.1
015
.94
864.
5988
0.96
1-0
.076
-0.0
52-0
.035
-0.0
2-0
.004
0lm
0030
n125
00*
84.2
9712
-69.
3905
21.
4997
8415
.82
15.6
611
97.6
811
0.99
5-0
.011
-0.0
1-0
.009
0-0
.005
0-0
.0lm
0346
m23
398
83.0
7818
-67.
4618
31.
5196
8116
.45
16.2
646
7.60
310.
941
-0.0
24-0
.072
-0.0
060
-0.0
22-0
.003
0lm
0056
k819
688
.087
15-7
0.15
366
1.52
3926
16.9
516
.76
420.
7308
0.94
9-0
.008
0-0
.065
0.00
10-0
.028
0.00
40lm
0350
l571
784
.304
06-6
6.44
258
1.52
4372
16.1
815
.99
1835
.827
20.
954
-0.0
21-0
.068
-0.0
020
-0.0
39-0
.003
0lm
0125
l930
273
.278
49-6
9.95
682
1.52
6312
16.9
817
.00
1311
.491
40.
999
-0.0
23-0
.01
-0.0
030
-0.0
070
-0.0
020
lm01
03m
2315
077
.286
43-6
9.52
645
1.52
7199
17.2
317
.07
1482
.649
80.
985
-0.0
25-0
.027
0.00
30-0
.006
00.
0020
lm01
84l1
1316
76.8
3495
-68.
5777
71.
5299
2217
.48
17.2
732
7.83
750.
993
-0.0
2-0
.032
-0.0
090
-0.0
16-0
.002
0lm
0551
k176
7076
.151
62-7
0.58
525
1.53
2272
17.2
216
.99
1236
.584
80.
979
-0.0
18-0
.033
-0.0
020
-0.0
-0.0
020
lm01
23m
9848
73.4
2535
-69.
4539
31.
5341
4517
.27
17.1
625
16.7
341
0.98
5-0
.005
0-0
.022
-0.0
030
-0.0
110.
0030
lm00
40l1
3585
86.0
081
-69.
2927
61.
5341
6717
.25
17.4
012
07.7
430
0.96
9-0
.021
-0.0
310.
0010
-0.0
0.00
20lm
0020
k136
2081
.889
91-6
9.15
231
1.53
4702
16.5
516
.36
762.
6655
0.91
5-0
.006
0-0
.128
-0.0
1-0
.072
0.00
20lm
0196
k267
6478
.835
27-6
8.88
038
1.53
8051
16.6
816
.38
1901
.836
50.
888
-0.0
3-0
.161
-0.0
13-0
.085
-0.0
030
lm02
90l1
7409
74.0
7302
-66.
5289
41.
5390
0316
.34
16.2
122
36.7
852
0.98
-0.0
020
-0.0
33-0
.001
0-0
.021
-0.0
040
lm00
90m
4818
78.4
994
-69.
0821
51.
5419
2416
.49
16.1
813
10.5
084
0.96
2-0
.027
-0.0
43-0
.001
0-0
.005
00.
0020
lm00
16m
1726
980
.518
55-7
0.20
887
1.54
2338
17.3
717
.24
1957
.668
50.
915
-0.0
57-0
.125
-0.0
12-0
.051
-0.0
020
162
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0422
l218
9474
.637
95-6
5.51
208
1.54
5397
15.6
115
.38
1794
.799
20.
947
-0.0
21-0
.047
-0.0
-0.0
040
0.00
10lm
0573
n131
7380
.749
14-7
1.02
406
1.54
5989
17.4
817
.44
1854
.864
60.
926
-0.0
31-0
.082
-0.0
15-0
.01
-0.0
030
lm03
40l8
577
82.7
1093
-66.
4640
51.
5463
6116
.64
16.3
919
77.6
605
0.95
2-0
.011
-0.0
68-0
.004
0-0
.031
0.0
lm04
27m
2145
975
.790
42-6
6.06
479
1.54
6547
16.9
716
.65
2257
.593
20.
945
-0.0
020
-0.0
77-0
.002
0-0
.038
0.00
10lm
0026
k106
6581
.825
62-7
0.17
208
1.54
8267
17.0
016
.98
2025
.525
80.
947
-0.0
4-0
.074
-0.0
16-0
.036
-0.0
020
lm02
14k2
4604
82.5
5082
-68.
509
1.54
8706
15.8
715
.81
1933
.756
40.
975
-0.0
080
-0.0
34-0
.004
0-0
.024
-0.0
010
lm02
81n7
749
73.4
0284
-66.
4426
21.
5490
6117
.20
16.9
518
44.6
662
0.95
60.
0030
-0.0
50.
0040
-0.0
340.
0020
lm03
40n7
354
83.2
2525
-66.
4509
31.
5535
8616
.48
16.1
780
0.64
540.
984
-0.0
070
-0.0
34-0
.005
0-0
.024
0.00
10lm
0375
l616
488
.906
77-6
7.14
641
1.55
3943
16.6
716
.55
801.
7426
0.97
8-0
.008
0-0
.029
-0.0
020
-0.0
080
-0.0
lm00
90n1
1730
78.4
3501
-69.
2799
71.
5549
7317
.00
16.9
211
52.8
088
0.90
5-0
.0-0
.137
-0.0
050
-0.0
830.
0040
lm01
14l6
671
74.0
3483
-69.
9428
41.
5558
7816
.54
16.4
618
04.7
621
0.96
2-0
.002
0-0
.052
-0.0
050
-0.0
2-0
.003
0lm
0586
l235
9281
.654
96-7
1.80
958
1.55
705
17.5
417
.28
2242
.607
10.
939
-0.0
21-0
.085
-0.0
050
-0.0
38-0
.005
0lm
0040
l197
6686
.203
22-6
9.33
944
1.55
7666
17.2
517
.20
1196
.704
80.
946
-0.0
15-0
.034
-0.0
020
0.00
200.
0030
lm02
85n5
241
73.7
0857
-67.
1363
21.
5577
4515
.93
15.6
419
02.7
300
0.93
7-0
.001
0-0
.076
0.0
-0.0
230.
0010
lm03
41m
1467
083
.817
84-6
6.34
805
1.55
8747
15.9
215
.66
1554
.704
30.
985
-0.0
11-0
.022
-0.0
050
-0.0
11-0
.0lm
0285
m12
790
73.5
3067
-67.
0314
71.
5590
716
.69
16.4
718
19.6
920
0.94
9-0
.013
-0.0
390.
0020
-0.0
040
0.00
80lm
0285
l265
8573
.158
96-6
7.28
642
1.55
9802
17.3
217
.10
815.
8174
0.98
2-0
.012
-0.0
28-0
.004
0-0
.021
-0.0
010
lm03
15m
1016
478
.765
89-6
7.00
723
1.56
0277
16.9
416
.68
1145
.694
50.
975
-0.0
010
-0.0
340.
0010
-0.0
20.
0lm
0110
n256
6874
.282
18-6
9.35
849
1.56
4822
16.3
116
.13
2031
.480
30.
963
-0.0
2-0
.051
-0.0
090
-0.0
28-0
.0lm
0184
l966
076
.885
69-6
8.56
789
1.56
8984
16.2
116
.05
1591
.657
60.
955
0.00
10-0
.066
-0.0
010
-0.0
31-0
.002
0lm
0167
l574
073
.933
2-6
8.89
664
1.57
2604
17.5
617
.36
2183
.662
50.
907
-0.0
-0.1
29-0
.002
0-0
.076
-0.0
050
lm02
14l2
5109
82.3
7873
-68.
6702
1.57
5578
17.4
417
.59
1492
.695
00.
995
-0.0
040
-0.0
29-0
.008
0-0
.017
0.00
10lm
0032
l228
7483
.873
82-6
9.70
626
1.57
6927
15.6
115
.43
1108
.845
70.
867
-0.0
3-0
.147
-0.0
13-0
.057
0.00
20lm
0337
k234
9281
.835
01-6
7.46
624
1.57
8628
17.3
517
.18
1459
.782
20.
963
-0.0
12-0
.07
-0.0
15-0
.041
0.00
40lm
0207
k154
7281
.653
77-6
8.80
021.
5794
2315
.73
15.6
713
17.5
052
0.93
8-0
.024
-0.0
77-0
.011
-0.0
45-0
.002
0lm
0166
l163
9073
.294
55-6
8.96
988
1.57
9747
16.0
915
.81
2245
.778
30.
97-0
.019
-0.0
48-0
.01
-0.0
330.
0030
lm00
23m
7584
83.5
8765
-69.
4420
91.
5798
8716
.13
15.9
022
35.6
280
0.86
4-0
.044
-0.1
85-0
.024
-0.0
860.
0020
lm01
15m
5231
75.3
5313
-69.
7787
21.
5803
7317
.73
17.6
618
62.5
755
0.94
9-0
.002
0-0
.097
-0.0
040
-0.0
640.
0010
lm03
41n6
753
84.0
7502
-66.
4906
41.
5809
6816
.67
16.4
220
14.5
633
0.96
5-0
.011
-0.0
44-0
.003
0-0
.023
0.00
10lm
0593
m12
530
85.2
9938
-70.
8668
11.
5813
9617
.34
17.2
221
99.6
400
0.93
4-0
.055
-0.0
9-0
.027
-0.0
370.
0090
lm01
92n3
0512
79.2
2526
-68.
3380
51.
5835
4716
.95
16.8
422
32.6
252
0.94
6-0
.04
-0.1
25-0
.052
-0.0
790.
01lm
0434
m21
038
76.5
4471
-65.
6932
71.
5855
4716
.29
16.0
614
15.8
778
0.98
8-0
.014
-0.0
29-0
.004
0-0
.015
-0.0
020
lm05
03l1
5319
88.8
0091
-65.
5445
1.58
6779
17.2
717
.19
1931
.733
20.
964
-0.0
7-0
.061
-0.0
44-0
.033
-0.0
010
lm01
72l1
5709
75.0
954
-68.
3373
11.
5880
3417
.55
17.4
620
99.8
753
0.95
0.00
70-0
.096
-0.0
050
-0.0
62-0
.001
0lm
0540
k919
973
.109
41-7
0.50
689
1.58
8396
16.4
016
.15
1813
.731
40.
953
-0.0
16-0
.046
-0.0
020
-0.0
030
0.00
30lm
0335
n574
782
.246
93-6
7.13
654
1.58
8518
17.2
217
.04
1149
.711
30.
947
0.00
80-0
.087
-0.0
060
-0.0
530.
0010
lm01
23m
2270
073
.552
3-6
9.52
692
1.58
8994
16.4
916
.31
556.
5427
0.87
8-0
.048
-0.1
68-0
.019
-0.0
770.
0040
lm01
21n2
5422
73.3
0901
-69.
3815
51.
5906
8117
.37
17.2
318
15.6
981
0.90
2-0
.108
-0.1
6-0
.046
-0.0
92-0
.003
0lm
0376
m12
338
88.5
3671
-67.
3879
61.
5916
1516
.88
16.7
050
3.69
120.
95-0
.015
-0.0
53-0
.004
0-0
.004
00.
0lm
0100
k136
6075
.904
39-6
9.14
193
1.59
1895
16.7
816
.67
1305
.509
40.
944
-0.0
080
-0.0
93-0
.003
0-0
.045
-0.0
030
lm03
87l7
856
90.7
4458
-67.
5176
21.
5922
4316
.65
16.4
419
19.7
987
0.93
5-0
.135
-0.0
97-0
.068
-0.0
430.
0020
163
lm03
30n1
0876
81.2
6355
-66.
4736
71.
5936
1216
.74
16.8
311
50.6
932
0.97
4-0
.015
-0.0
37-0
.006
0-0
.013
-0.0
lm01
20l2
4125
72.0
6416
-69.
3702
81.
5944
817
.42
17.4
111
15.6
637
0.90
80.
0020
-0.1
53-0
.0-0
.088
-0.0
010
lm02
10l2
0271
82.4
3808
-67.
9382
21.
5945
9916
.62
16.4
220
28.5
189
0.88
7-0
.046
-0.1
56-0
.02
-0.0
66-0
.004
0lm
0453
k810
680
.378
16-6
5.24
698
1.59
5613
17.4
817
.34
1840
.725
10.
99-0
.031
-0.0
2-0
.016
-0.0
070
-0.0
040
lm05
50n7
880
75.8
0149
-70.
6544
11.
5968
5817
.14
16.8
622
58.5
811
0.97
9-0
.021
-0.0
29-0
.011
-0.0
170.
0020
lm04
35l5
752
77.2
7269
-65.
7368
31.
5970
3317
.74
17.5
922
24.5
803
0.95
5-0
.072
-0.1
02-0
.036
-0.0
57-0
.003
0lm
0344
m82
9183
.098
27-6
7.01
023
1.59
7243
16.5
416
.36
825.
8571
0.88
3-0
.04
-0.1
59-0
.019
-0.0
710.
0lm
0292
n116
2174
.279
99-6
6.82
953
1.59
9642
16.8
016
.59
1860
.567
20.
973
0.00
30-0
.042
-0.0
020
-0.0
28-0
.006
0lm
0126
k137
5872
.264
26-7
0.20
293
1.60
1905
17.0
316
.85
1918
.601
80.
981
-0.0
22-0
.038
-0.0
1-0
.019
-0.0
040
lm01
54k2
1118
71.3
9661
-68.
4872
1.60
291
17.3
917
.25
1750
.851
10.
964
-0.0
13-0
.052
-0.0
060
-0.0
340.
0030
lm01
75n2
3496
76.5
9228
-68.
6319
1.60
4598
17.4
317
.32
1878
.616
60.
907
-0.0
72-0
.125
-0.0
31-0
.069
-0.0
010
lm01
11m
1609
275
.530
49-6
9.13
855
1.60
4599
16.3
316
.05
1890
.605
60.
94-0
.024
-0.0
67-0
.005
0-0
.019
-0.0
030
lm00
31m
7414
85.6
1249
-69.
0871
31.
6059
8915
.61
15.4
615
91.7
013
0.94
-0.0
18-0
.1-0
.012
-0.0
440.
0010
lm01
75k1
8167
76.0
6658
-68.
4525
61.
6062
0616
.47
16.3
314
02.8
984
0.93
8-0
.023
-0.0
76-0
.005
0-0
.016
0.0
lm00
44l2
3659
85.8
3336
-70.
0552
1.60
7072
16.3
916
.20
1481
.736
30.
876
-0.0
75-0
.169
-0.0
26-0
.082
0.00
10lm
0197
k234
6779
.842
63-6
8.84
883
1.60
8347
16.3
216
.07
1918
.710
40.
975
-0.0
11-0
.028
-0.0
070
-0.0
110.
0020
lm03
25n2
3385
80.4
343
-67.
2488
31.
6090
117
.10
16.8
820
58.4
899
0.95
3-0
.0-0
.057
-0.0
020
-0.0
250.
0010
lm00
52m
1892
688
.608
4-6
9.55
504
1.61
1031
16.0
515
.77
1566
.720
30.
964
-0.0
25-0
.056
-0.0
070
-0.0
260.
0010
lm01
61n2
4107
74.5
1188
-67.
9418
21.
6114
7517
.76
17.5
615
64.5
855
0.97
8-0
.03
-0.0
250.
0020
-0.0
030
0.00
70lm
0367
n683
587
.455
23-6
7.50
409
1.61
154
17.7
317
.52
2033
.544
70.
971
-0.0
030
-0.0
68-0
.001
0-0
.061
-0.0
040
lm02
15m
2258
583
.794
33-6
8.48
498
1.61
3457
17.4
517
.22
2155
.804
70.
969
-0.0
2-0
.059
-0.0
13-0
.046
-0.0
010
lm06
03l2
4970
86.8
177
-71.
0998
61.
6142
2717
.27
17.2
410
87.8
655
0.88
7-0
.079
-0.1
95-0
.042
-0.1
020.
0030
lm00
30k1
3205
83.9
8549
-69.
1476
41.
6152
0516
.09
16.1
118
08.8
535
0.90
6-0
.03
-0.1
13-0
.011
-0.0
370.
0030
lm05
50m
2019
675
.552
69-7
0.58
644
1.61
6823
17.3
117
.09
1126
.615
20.
979
-0.0
18-0
.05
-0.0
080
-0.0
35-0
.0lm
0294
k319
574
.152
99-6
6.97
358
1.62
0032
17.1
817
.08
1173
.624
40.
981
-0.0
16-0
.033
-0.0
070
-0.0
2-0
.002
0lm
0156
m42
6271
.910
81-6
8.85
731.
6202
6415
.97
15.7
822
57.5
616
0.93
3-0
.019
-0.0
78-0
.004
0-0
.021
-0.0
lm04
25n1
5511
75.6
5717
-65.
8027
31.
6233
8417
.71
17.5
116
03.5
934
0.97
2-0
.016
-0.0
50.
0080
-0.0
41-0
.007
0lm
0426
l157
0274
.426
31-6
6.16
279
1.62
4957
15.7
215
.46
508.
6286
0.89
7-0
.03
-0.1
1-0
.01
-0.0
310.
0070
lm02
10l1
8828
82.5
2517
-67.
9267
11.
6258
9717
.63
17.5
423
02.7
223
0.91
-0.0
47-0
.074
-0.0
16-0
.025
0.00
80lm
0710
k102
8582
.931
66-7
1.92
374
1.62
7842
17.7
117
.66
1593
.682
30.
969
-0.0
050
-0.0
450.
0010
-0.0
30.
0010
lm00
90n2
9958
78.5
351
-69.
3833
11.
6284
0717
.44
17.3
521
64.7
591
0.93
8-0
.009
0-0
.097
-0.0
070
-0.0
57-0
.002
0lm
0344
k106
0182
.550
39-6
7.02
696
1.62
8604
16.6
616
.51
1441
.789
00.
912
-0.0
34-0
.107
-0.0
15-0
.039
0.00
20lm
0711
m42
1884
.538
37-7
1.86
447
1.63
0559
17.3
417
.24
488.
7207
0.89
1-0
.035
-0.0
94-0
.007
0-0
.012
0.02
6lm
0236
l256
4086
.268
2-6
9.03
441.
6313
1217
.32
17.1
094
1.54
170.
842
-0.0
5-0
.202
-0.0
050
-0.0
840.
015
lm05
84l6
042
81.6
7559
-71.
3408
71.
6323
4417
.07
17.1
019
57.6
888
0.93
9-0
.039
-0.0
78-0
.01
-0.0
3-0
.001
0lm
0151
m41
2872
.466
64-6
7.70
253
1.63
3059
15.9
515
.58
1465
.656
40.
906
0.00
40-0
.155
0.00
30-0
.093
0.00
30lm
0424
n101
3374
.977
82-6
5.77
246
1.63
539
16.3
016
.08
706.
7728
0.98
5-0
.016
-0.0
29-0
.006
0-0
.016
0.0
lm00
93n2
4281
79.2
7628
-69.
6823
91.
6357
9917
.49
17.3
555
6.51
910.
925
-0.0
070
-0.1
41-0
.0-0
.078
-0.0
020
lm02
04m
1867
981
.155
2-6
8.45
898
1.63
6472
17.4
417
.36
1455
.769
20.
963
-0.0
19-0
.04
-0.0
080
-0.0
270.
0010
lm02
01n2
6407
82.1
4915
-67.
9539
11.
6386
717
.71
17.4
710
93.8
296
0.94
1-0
.015
-0.0
5-0
.009
0-0
.021
0.00
10lm
0333
k991
581
.696
75-6
6.65
927
1.63
9068
16.5
816
.40
2245
.677
30.
955
-0.0
090
-0.0
59-0
.005
0-0
.025
-0.0
020
164
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0090
m43
2178
.601
31-6
9.07
897
1.64
1272
17.1
917
.04
1231
.610
10.
906
-0.0
57-0
.118
-0.0
25-0
.052
0.00
40lm
0032
m22
261
84.3
5161
-69.
5720
31.
6441
4615
.70
15.4
823
45.5
978
0.97
4-0
.007
0-0
.038
-0.0
090
-0.0
3-0
.003
0lm
0551
l210
8175
.922
28-7
0.73
455
1.64
5211
15.6
815
.48
1903
.745
30.
963
-0.0
16-0
.037
0.0
-0.0
010
-0.0
010
lm03
54m
1387
584
.965
51-6
7.04
351
1.64
5882
17.3
617
.22
819.
8363
0.98
3-0
.012
-0.0
230.
0030
-0.0
020
-0.0
050
lm03
14k2
4373
77.6
4572
-67.
1111
81.
6491
7916
.35
16.3
021
86.7
216
0.87
9-0
.057
-0.1
66-0
.028
-0.0
750.
0020
lm00
52l4
698
88.1
0094
-69.
5857
91.
6509
7917
.20
17.0
515
49.7
634
0.93
6-0
.01
-0.0
99-0
.009
0-0
.058
0.00
40lm
0551
l153
6576
.072
1-7
0.69
851.
6520
8316
.25
15.9
812
66.5
146
0.98
8-0
.008
0-0
.028
-0.0
050
-0.0
21-0
.001
0lm
0101
l229
0076
.920
21-6
9.34
193
1.65
3449
16.2
616
.14
1139
.845
20.
891
-0.0
26-0
.122
-0.0
1-0
.032
0.00
30lm
0310
m15
759
77.9
497
-66.
4224
61.
6536
5817
.30
17.1
012
57.5
597
0.98
2-0
.024
-0.0
19-0
.001
00.
0010
-0.0
040
lm03
15n1
4721
78.6
2626
-67.
1917
51.
6549
9716
.87
16.5
717
86.7
429
0.97
7-0
.002
0-0
.037
0.00
10-0
.02
0.00
30lm
0317
k486
978
.577
66-6
7.33
758
1.65
617
17.7
117
.50
776.
7495
0.98
4-0
.006
0-0
.059
-0.0
090
-0.0
54-0
.006
0lm
0304
n255
3576
.067
79-6
7.26
431.
6572
4515
.76
15.4
622
48.7
779
0.99
9-0
.002
0-0
.017
-0.0
060
-0.0
110.
0010
lm00
33k1
5395
85.0
6121
-69.
4932
61.
6580
115
.92
15.8
522
57.6
709
0.90
8-0
.04
-0.1
16-0
.013
-0.0
440.
0020
lm00
30l4
662
84.0
9164
-69.
2367
91.
6606
5116
.99
17.1
714
68.6
786
0.92
80.
0040
-0.1
2-0
.001
0-0
.078
0.00
40lm
0344
l240
7682
.641
83-6
7.27
292
1.66
2852
16.3
016
.12
1447
.834
90.
933
-0.0
22-0
.077
-0.0
020
-0.0
11-0
.0lm
0325
k980
580
.318
71-6
7.01
041.
6643
5116
.19
15.9
511
66.6
467
0.94
9-0
.007
0-0
.073
-0.0
010
-0.0
390.
0030
lm02
07n1
8537
82.0
2376
-68.
9846
71.
6647
7715
.60
15.3
623
18.6
740
0.95
9-0
.018
-0.0
510.
0-0
.009
00.
0040
lm05
83l2
2712
82.3
5358
-71.
0823
61.
6655
6515
.60
15.4
412
53.6
088
0.94
8-0
.015
-0.0
87-0
.008
0-0
.048
-0.0
010
lm03
51m
1277
385
.822
24-6
6.32
968
1.66
6009
16.4
216
.15
1865
.694
30.
976
-0.0
54-0
.049
-0.0
19-0
.041
-0.0
010
lm03
64m
5107
86.6
1851
-66.
9854
51.
6662
3117
.45
17.2
814
39.8
010
0.92
9-0
.001
0-0
.132
0.00
10-0
.082
0.00
10lm
0377
n700
089
.184
35-6
7.51
179
1.66
7075
17.2
116
.93
1625
.666
70.
952
-0.0
12-0
.066
-0.0
090
-0.0
260.
0020
lm02
12n2
0573
83.0
2989
-68.
2850
41.
6680
9216
.91
16.9
419
53.7
398
0.92
9-0
.011
-0.1
15-0
.008
0-0
.085
0.0
lm03
47l1
7494
83.7
5017
-67.
5900
31.
6689
0116
.46
16.3
110
93.8
434
0.98
3-0
.012
-0.0
26-0
.006
0-0
.01
0.00
10lm
0216
l879
382
.576
22-6
8.92
088
1.66
9043
15.8
615
.68
1997
.580
30.
928
-0.0
31-0
.103
-0.0
020
-0.0
34-0
.006
0lm
0127
n645
573
.559
84-7
0.29
475
1.66
9262
16.3
216
.07
1958
.599
60.
887
-0.0
5-0
.161
-0.0
22-0
.062
-0.0
010
lm01
74k2
3286
74.9
3274
-68.
4936
81.
6697
8217
.56
17.4
722
06.7
780
0.94
9-0
.034
-0.0
65-0
.014
-0.0
190.
0050
lm01
55k1
7320
72.1
6521
-68.
4585
11.
6707
8617
.40
17.3
719
80.5
256
0.96
8-0
.083
-0.0
6-0
.028
-0.0
5-0
.002
0lm
0460
l231
1881
.202
9-6
5.17
684
1.67
0908
17.6
717
.59
1424
.890
10.
924
-0.0
15-0
.13
-0.0
050
-0.0
68-0
.004
0lm
0473
l153
0983
.709
99-6
5.44
981
1.67
1121
17.3
917
.32
1885
.706
30.
962
-0.0
7-0
.059
-0.0
47-0
.035
0.00
20lm
0184
k228
0776
.852
44-6
8.49
225
1.67
2505
16.8
516
.66
1583
.660
10.
964
-0.0
27-0
.082
-0.0
15-0
.062
-0.0
010
lm00
30m
3468
84.4
2029
-69.
0781
21.
6740
9816
.18
16.1
122
64.7
604
0.92
7-0
.01
-0.1
18-0
.009
0-0
.08
0.00
40lm
0127
m85
8973
.762
25-7
0.15
474
1.67
6613
17.1
416
.98
2297
.631
80.
959
-0.0
22-0
.032
0.0
0.00
200.
0050
lm00
35m
2323
385
.696
45-6
9.88
486
1.67
7625
15.5
815
.34
797.
5962
0.95
1-0
.014
-0.0
420.
00.
00.
0lm
0156
m16
1971
.732
44-6
8.76
539
1.68
1305
17.1
517
.03
1864
.561
30.
993
0.00
20-0
.02
-0.0
-0.0
15-0
.002
0lm
0113
k252
5974
.862
16-6
9.53
946
1.68
1418
17.4
517
.39
858.
7184
0.97
7-0
.019
-0.0
32-0
.001
00.
0010
0.00
30lm
0356
l710
084
.697
1-6
7.50
193
1.68
2072
16.9
616
.81
2185
.704
00.
923
-0.0
29-0
.08
-0.0
12-0
.026
0.0
lm03
44l1
3598
82.6
2982
-67.
2010
51.
6853
9516
.39
16.1
545
0.81
850.
919
0.00
10-0
.129
-0.0
020
-0.0
89-0
.001
0lm
0376
n112
3088
.291
72-6
7.53
606
1.68
6368
17.5
917
.41
1664
.548
60.
965
-0.0
060
-0.1
15-0
.017
-0.0
760.
0090
lm01
06l1
6000
76.1
9455
-70.
3658
1.68
6602
17.4
517
.29
1779
.778
80.
936
0.00
40-0
.088
-0.0
050
-0.0
52-0
.001
0lm
0377
l92
89.0
9938
-67.
6003
61.
6876
7717
.60
17.3
776
1.75
830.
956
-0.0
45-0
.074
-0.0
22-0
.041
-0.0
040
lm00
55l7
331
88.7
6966
-69.
9460
81.
6884
7917
.40
17.3
919
11.8
249
0.97
7-0
.004
0-0
.02
-0.0
020
-0.0
19-0
.003
0
165
lm04
24n1
7990
74.7
9369
-65.
8914
1.69
0344
17.0
216
.79
2198
.633
60.
96-0
.018
-0.0
78-0
.01
-0.0
590.
0030
lm03
40n5
950
83.0
4071
-66.
4409
91.
6925
7715
.68
15.4
716
07.6
250
0.91
6-0
.001
0-0
.143
0.0
-0.0
890.
0040
lm00
21m
1520
783
.333
7-6
9.13
687
1.69
5205
17.5
017
.39
1145
.703
00.
874
-0.0
75-0
.177
-0.0
41-0
.099
0.01
4lm
0186
m18
764
77.3
7196
-68.
8263
31.
6970
3115
.73
15.5
522
57.6
156
0.96
50.
0030
-0.0
50.
0030
-0.0
32-0
.002
0lm
0344
k440
982
.525
54-6
6.98
509
1.69
7053
16.2
816
.09
1616
.587
10.
950.
0010
-0.0
89-0
.0-0
.053
-0.0
010
lm01
21l1
5224
72.8
0434
-69.
2925
41.
6997
0816
.64
16.5
110
90.6
622
0.97
4-0
.023
-0.0
36-0
.001
0-0
.013
0.00
10lm
0221
n123
9885
.799
38-6
7.87
471
1.70
0592
17.3
917
.20
1889
.696
90.
908
-0.0
030
-0.1
230.
0010
-0.0
590.
0020
lm01
60m
2404
573
.420
43-6
7.80
215
1.70
2329
16.2
516
.01
1898
.736
90.
88-0
.028
-0.1
34-0
.011
-0.0
230.
0010
lm02
15k2
5234
83.5
4176
-68.
5006
51.
7027
1116
.67
16.5
713
75.8
974
0.95
6-0
.031
-0.0
61-0
.005
0-0
.021
-0.0
030
lm02
14n4
693
82.9
0646
-68.
5338
91.
7027
5417
.44
17.5
221
78.7
367
0.97
50.
0010
-0.0
66-0
.002
0-0
.049
-0.0
090
lm06
04k1
9867
85.5
5982
-71.
2818
61.
7028
3616
.50
16.5
044
5.72
790.
962
-0.0
12-0
.069
-0.0
11-0
.048
-0.0
030
lm03
15k1
9071
78.2
3229
-67.
0672
91.
7029
5317
.17
17.0
640
1.75
880.
988
-0.0
1-0
.019
-0.0
030
-0.0
10.
0020
lm00
85k5
094
94.9
5248
-69.
7825
1.70
5211
16.4
816
.33
2223
.689
90.
98-0
.016
-0.0
20.
0010
0.0
0.00
10lm
0167
n606
474
.666
38-6
8.89
41.
7081
216
.65
16.4
418
88.5
883
0.98
6-0
.011
-0.0
33-0
.006
0-0
.023
-0.0
020
lm01
60k1
5778
73.3
0671
-67.
7540
11.
7092
1116
.65
16.3
718
11.7
418
0.88
8-0
.039
-0.1
55-0
.019
-0.0
530.
0010
lm01
55k2
2815
72.3
7866
-68.
4916
21.
7101
2816
.93
17.0
019
07.7
234
0.97
2-0
.061
-0.0
42-0
.015
-0.0
27-0
.003
0lm
0131
l128
4671
.289
77-6
9.39
025
1.71
0566
16.2
316
.09
870.
5622
0.96
6-0
.024
-0.0
51-0
.008
0-0
.021
0.00
40lm
0587
k277
4282
.469
04-7
1.67
718
1.71
1556
16.4
316
.19
1208
.747
30.
975
-0.0
15-0
.025
0.0
-0.0
020
0.0
lm01
11m
7486
75.3
29-6
9.08
815
1.71
3146
17.4
017
.16
2171
.700
40.
932
0.0
-0.1
1-0
.002
0-0
.063
0.00
30lm
0207
m26
339
81.8
4312
-68.
8687
91.
7150
1516
.11
15.8
918
03.8
386
0.84
7-0
.051
-0.1
67-0
.027
-0.0
790.
0040
lm04
47n7
830
79.2
0754
-66.
1082
21.
7155
6117
.47
17.2
722
25.6
609
0.89
2-0
.063
-0.1
34-0
.024
-0.0
60.
0040
lm03
26k2
3448
79.1
6561
-67.
4577
31.
7160
3616
.92
16.8
120
28.5
100
0.94
2-0
.014
-0.0
98-0
.008
0-0
.054
0.00
30lm
0292
n164
8374
.369
28-6
6.86
049
1.71
682
15.6
715
.42
2471
.886
80.
972
-0.0
11-0
.03
-0.0
020
0.00
10-0
.002
0lm
0050
n202
8088
.647
21-6
9.38
678
1.71
811
17.5
717
.45
871.
6393
0.96
20.
0010
-0.0
590.
0010
-0.0
360.
0010
lm03
44n5
050
83.0
0607
-67.
1404
51.
7189
516
.62
16.4
513
64.9
387
0.98
1-0
.02
-0.0
22-0
.006
0-0
.011
0.00
50lm
0347
k177
2283
.538
96-6
7.42
469
1.72
4282
16.8
916
.78
1768
.856
00.
957
0.00
70-0
.072
-0.0
010
-0.0
540.
0020
lm03
20n1
9241
79.7
2365
-66.
5277
51.
7247
7417
.04
16.9
112
58.5
611
0.99
3-0
.036
-0.0
080
-0.0
090
-0.0
070
-0.0
020
lm01
17k2
6536
75.0
7509
-70.
2802
51.
7257
8816
.89
16.6
379
7.59
990.
972
-0.0
15-0
.047
-0.0
070
-0.0
27-0
.003
0lm
0366
m35
4386
.482
29-6
7.32
311
1.72
7942
17.0
816
.97
1828
.802
80.
895
-0.0
56-0
.137
-0.0
22-0
.054
0.00
30lm
0285
l175
4373
.299
65-6
7.21
674
1.72
8627
16.2
515
.98
1838
.676
10.
977
-0.0
13-0
.036
-0.0
030
-0.0
090
-0.0
010
lm01
26l2
0410
72.0
8139
-70.
3952
61.
7291
8516
.94
16.9
018
60.5
466
0.93
9-0
.05
-0.1
11-0
.026
-0.0
64-0
.002
0lm
0333
k279
2581
.906
91-6
6.76
681
1.73
1749
17.5
517
.49
1883
.664
50.
893
-0.0
66-0
.144
-0.0
3-0
.07
-0.0
040
lm01
10k2
3246
74.0
4754
-69.
1985
31.
7320
1815
.94
15.7
417
55.8
812
0.89
9-0
.032
-0.1
27-0
.013
-0.0
43-0
.001
0lm
0354
n956
484
.742
62-6
7.17
105
1.73
5055
16.9
416
.80
1305
.563
20.
982
-0.0
16-0
.02
0.0
0.0
-0.0
lm01
25k2
2446
72.9
9053
-69.
8850
81.
7351
8616
.64
16.5
616
00.5
591
0.90
6-0
.038
-0.1
26-0
.017
-0.0
550.
0040
lm01
14m
1515
174
.594
23-6
9.83
697
1.74
1331
17.2
017
.09
1605
.544
50.
945
-0.0
12-0
.1-0
.009
0-0
.081
-0.0
020
lm06
23m
1743
191
.496
37-7
0.91
431
1.74
138
17.5
917
.43
2307
.773
80.
976
-0.0
52-0
.052
-0.0
1-0
.029
-0.0
010
lm03
45k3
891
83.7
1194
-66.
9797
21.
7424
8615
.98
15.7
950
7.57
860.
881
-0.0
57-0
.17
-0.0
27-0
.08
0.00
30lm
0317
k171
6278
.188
83-6
7.42
939
1.74
4914
16.3
516
.18
1529
.629
50.
953
-0.0
070
-0.0
73-0
.004
0-0
.043
-0.0
020
lm07
00k1
3942
80.5
0345
-71.
9429
31.
7463
6117
.33
17.1
211
90.7
323
0.97
9-0
.028
-0.0
29-0
.001
0-0
.001
00.
0060
lm07
10k7
222
82.6
1599
-71.
9023
21.
7464
7617
.28
17.0
718
89.8
399
0.96
6-0
.024
-0.0
34-0
.001
00.
0020
0.00
30
166
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0127
l673
173
.212
6-7
0.29
473
1.74
8158
15.4
915
.21
1992
.517
80.
896
-0.0
41-0
.133
-0.0
15-0
.045
-0.0
020
lm01
27m
9330
73.6
3977
-70.
1607
41.
7511
6115
.87
15.6
725
55.6
741
0.98
7-0
.011
-0.0
140.
0010
-0.0
010
0.00
30lm
0181
m21
196
78.0
2705
-67.
7727
21.
7514
9116
.77
16.7
412
71.5
380
0.99
-0.0
43-0
.012
-0.0
090
-0.0
110.
0010
lm02
05n1
5591
81.8
3723
-68.
5895
41.
7536
9716
.30
16.0
037
7.81
220.
98-0
.012
-0.0
3-0
.005
0-0
.016
0.00
30lm
0356
k552
684
.674
36-6
7.33
731
1.75
4305
17.5
117
.53
1842
.860
30.
925
-0.0
020
-0.0
98-0
.011
-0.0
610.
0040
lm05
64l6
100
77.3
2867
-71.
3353
51.
7544
8816
.79
16.5
418
44.7
313
0.97
10.
0040
-0.0
650.
0010
-0.0
45-0
.001
0lm
0285
n732
273
.694
27-6
7.15
244
1.75
4575
16.4
716
.16
1091
.663
80.
963
-0.0
030
-0.0
41-0
.003
0-0
.022
0.00
30lm
0112
n127
7574
.607
44-6
9.62
906
1.75
6539
15.8
315
.66
2231
.567
70.
987
-0.0
010
-0.0
26-0
.002
0-0
.017
0.0
lm04
36l1
4585
76.4
2263
-66.
1591
71.
7569
7116
.04
15.6
518
64.6
055
0.96
4-0
.023
-0.0
57-0
.012
-0.0
34-0
.002
0lm
0184
n982
477
.501
89-6
8.56
479
1.75
7143
16.1
415
.97
2084
.911
90.
965
0.00
10-0
.057
0.00
20-0
.038
-0.0
010
lm00
20m
1062
182
.486
96-6
9.12
021.
7588
7615
.39
15.2
518
75.6
794
0.98
60.
0010
-0.0
26-0
.001
0-0
.01
0.00
10lm
0223
m18
449
85.7
7103
-68.
1128
1.75
9816
16.8
716
.66
1101
.878
40.
94-0
.027
-0.0
52-0
.003
0-0
.008
00.
0lm
0090
l212
3677
.964
17-6
9.34
711
1.76
0117
.35
17.2
653
0.55
690.
964
-0.0
12-0
.069
-0.0
080
-0.0
46-0
.002
0lm
0030
n222
7884
.361
-69.
3554
1.76
0563
16.7
816
.69
2226
.865
70.
956
-0.0
-0.0
52-0
.001
0-0
.023
0.0
lm00
95l3
0693
78.9
2326
-70.
0776
21.
7610
1616
.00
15.8
215
79.7
005
0.89
5-0
.001
0-0
.14
0.00
10-0
.066
0.00
20lm
0217
n248
8584
.039
69-6
8.92
426
1.76
2408
16.2
716
.18
802.
8084
0.93
70.
0-0
.108
-0.0
020
-0.0
750.
0050
lm03
43m
9142
83.8
3843
-66.
6530
41.
7635
5616
.69
16.5
846
8.65
780.
917
-0.0
53-0
.109
-0.0
2-0
.05
0.00
40lm
0045
n247
5487
.405
13-7
0.09
581
1.76
449
16.8
116
.51
819.
7090
0.98
3-0
.011
-0.0
28-0
.004
0-0
.018
0.00
40lm
0206
k180
0480
.536
53-6
8.81
668
1.76
5559
16.8
216
.71
1595
.739
80.
894
-0.0
59-0
.156
-0.0
22-0
.074
-0.0
050
lm04
46k1
2751
77.9
4-6
5.99
113
1.76
6655
17.1
016
.95
1904
.749
90.
965
-0.0
2-0
.069
-0.0
1-0
.05
0.00
40lm
0304
n290
8475
.991
17-6
7.28
674
1.77
2755
15.8
015
.52
1628
.528
00.
981
-0.0
12-0
.024
-0.0
060
-0.0
080
0.0
lm02
23n1
9445
85.6
5399
-68.
342
1.77
3336
17.3
017
.17
1122
.635
60.
983
-0.0
21-0
.018
0.00
100.
0010
0.00
10lm
0283
k137
5573
.164
4-6
6.69
281.
7744
0916
.51
16.3
441
4.73
840.
965
-0.0
19-0
.035
0.0
0.0
0.00
10lm
0550
k195
7775
.292
69-7
0.58
692
1.77
4651
16.0
415
.74
2304
.684
80.
99-0
.003
0-0
.03
0.0
-0.0
23-0
.001
0lm
0291
m21
869
75.0
7896
-66.
3838
1.77
4816
17.4
017
.17
1820
.675
20.
931
-0.0
9-0
.112
-0.0
39-0
.062
0.00
10lm
0101
k866
977
.078
02-6
9.10
507
1.77
5599
16.4
916
.23
1305
.509
40.
987
-0.0
18-0
.024
-0.0
020
-0.0
030
-0.0
050
lm01
07k1
8605
77.0
512
-70.
2212
11.
7766
4416
.94
16.7
322
59.6
017
0.95
3-0
.012
-0.0
62-0
.006
0-0
.029
-0.0
020
lm02
41m
1803
489
.226
76-6
7.77
295
1.77
7518
17.4
417
.25
1255
.648
60.
972
-0.0
1-0
.034
-0.0
050
-0.0
180.
0010
lm03
47m
2208
083
.968
17-6
7.45
279
1.77
7695
15.6
615
.38
428.
7524
0.96
1-0
.011
-0.0
57-0
.007
0-0
.029
-0.0
010
lm00
12l1
6381
79.9
1597
-69.
6584
21.
7790
215
.96
15.6
837
6.87
290.
949
-0.0
28-0
.08
-0.0
090
-0.0
15-0
.002
0lm
0031
m22
434
85.6
1171
-69.
1946
61.
7790
4917
.32
17.2
111
81.7
833
0.97
8-0
.014
-0.0
61-0
.005
0-0
.035
-0.0
030
lm05
43k1
2503
74.1
7109
-70.
8689
31.
7804
6817
.12
16.9
915
67.6
014
0.97
2-0
.01
-0.0
31-0
.003
0-0
.007
0-0
.002
0lm
0110
n110
1574
.565
63-6
9.26
961.
7817
0416
.04
15.8
211
39.8
417
0.97
8-0
.012
-0.0
16-0
.001
00.
00.
0010
lm02
17l1
7550
83.3
8491
-68.
9815
91.
7842
0116
.77
16.7
025
56.7
273
0.97
3-0
.01
-0.0
28-0
.005
0-0
.017
-0.0
lm00
14m
1494
0*80
.454
21-6
9.83
811.
7856
3417
.27
17.1
517
11.9
362
0.97
6-0
.008
0-0
.044
-0.0
040
-0.0
18-0
.003
0lm
0120
m68
4072
.476
89-6
9.08
672
1.78
5889
17.1
316
.96
1777
.768
40.
958
-0.0
26-0
.041
-0.0
010
-0.0
020
0.00
40lm
0313
k199
3978
.399
02-6
6.71
775
1.78
7155
17.2
617
.17
1097
.654
70.
879
-0.0
67-0
.163
-0.0
31-0
.082
0.00
40lm
0031
m11
024
85.6
2526
-69.
2203
11.
7887
4117
.59
17.5
422
30.6
328
0.92
5-0
.005
0-0
.12
-0.0
030
-0.0
62-0
.005
0lm
0167
m10
826
74.4
7513
-68.
7739
11.
7887
7916
.05
15.8
511
81.6
320
0.98
6-0
.012
-0.0
15-0
.001
0-0
.001
0-0
.0lm
0290
l521
373
.956
04-6
6.43
437
1.79
1025
15.4
715
.28
2201
.592
70.
932
-0.0
28-0
.089
-0.0
11-0
.025
-0.0
lm02
85n1
2253
*73
.377
58-6
7.19
251.
7919
9817
.11
16.9
315
24.5
967
0.92
3-0
.002
0-0
.13
-0.0
080
-0.1
050.
0020
167
lm03
44l1
6103
82.6
3064
-67.
2183
11.
7929
415
.60
15.3
615
76.6
962
0.98
3-0
.009
0-0
.049
-0.0
050
-0.0
30.
0010
lm01
22m
1943
672
.568
34-6
9.55
117
1.79
6151
16.2
516
.15
1825
.659
10.
945
-0.0
010
-0.0
69-0
.005
0-0
.021
-0.0
lm01
21k7
851
73.2
5922
-69.
0930
51.
7976
3716
.56
16.2
922
65.5
959
0.96
1-0
.01
-0.0
88-0
.003
0-0
.052
0.00
20lm
0284
n225
8372
.819
71-6
7.26
464
1.79
8432
16.9
016
.71
1579
.608
70.
958
-0.0
2-0
.044
-0.0
-0.0
060
0.00
10lm
0053
k119
4189
.148
92-6
9.47
271
1.79
9736
17.5
517
.53
800.
7358
0.91
3-0
.072
-0.1
24-0
.033
-0.0
620.
0040
lm03
00k5
450
75.8
4331
-66.
2824
51.
8017
4716
.08
15.7
541
9.59
640.
969
-0.0
14-0
.025
0.00
10-0
.00.
0050
lm01
64m
2801
073
.589
27-6
8.51
651.
8017
6217
.38
17.2
373
3.70
680.
978
-0.0
1-0
.024
0.00
20-0
.018
0.0
lm04
67k1
1376
82.0
8206
-65.
9833
71.
8021
7515
.57
15.3
422
15.8
423
0.92
5-0
.036
-0.1
09-0
.013
-0.0
43-0
.001
0lm
0497
m32
9487
.596
41-6
5.98
825
1.80
2402
17.0
116
.77
1828
.798
30.
944
-0.0
34-0
.075
-0.0
070
-0.0
2-0
.001
0lm
0173
m15
001
76.3
9634
-68.
081.
8030
3517
.54
17.3
018
80.5
939
0.97
3-0
.017
-0.0
31-0
.012
-0.0
260.
0010
lm00
10l2
4269
80.1
0633
-69.
3668
31.
8038
3815
.97
15.7
411
97.6
493
0.99
2-0
.007
0-0
.012
-0.0
-0.0
-0.0
020
lm04
55n9
465
80.8
8538
-65.
7585
81.
8047
2617
.27
17.0
214
47.8
054
0.96
1-0
.012
-0.0
65-0
.011
-0.0
53-0
.003
0lm
0336
l200
1181
.168
75-6
7.63
918
1.80
7377
17.1
516
.84
533.
5488
0.94
0.00
10-0
.095
-0.0
020
-0.0
630.
0lm
0342
k470
882
.880
24-6
6.63
464
1.80
7389
16.9
716
.78
1952
.623
00.
952
-0.0
48-0
.071
-0.0
14-0
.03
0.00
30lm
0340
l195
9482
.805
36-6
6.58
521
1.80
9525
15.5
815
.36
1388
.901
20.
875
-0.0
55-0
.173
-0.0
26-0
.08
0.00
10lm
0551
l860
876
.250
12-7
0.65
461.
8097
8316
.84
16.5
711
83.6
547
0.98
5-0
.021
-0.1
060.
0030
-0.0
81-0
.011
lm01
12n1
2177
74.3
9924
-69.
6260
71.
8126
6515
.44
15.2
722
56.5
889
0.96
2-0
.01
-0.0
39-0
.0-0
.001
00.
0030
lm03
34l2
0839
80.9
4674
-67.
2968
61.
8132
5516
.02
15.7
710
59.8
849
0.95
8-0
.019
-0.0
47-0
.002
0-0
.004
0-0
.001
0lm
0323
m29
284
80.3
3912
-66.
7768
51.
8148
7917
.56
17.4
217
01.4
666
0.95
3-0
.032
-0.0
42-0
.0-0
.002
00.
0050
lm00
46k1
7569
86.1
6095
-70.
2370
51.
8152
1616
.94
16.7
819
39.6
243
0.90
8-0
.05
-0.1
07-0
.018
-0.0
440.
0090
lm02
57m
2028
1*91
.274
33-6
8.85
292
1.82
1306
17.3
017
.08
1506
.815
70.
951
0.00
30-0
.053
0.00
20-0
.018
0.00
10lm
0555
m84
1576
.758
04-7
1.20
828
1.82
1561
16.4
716
.20
1093
.625
10.
978
-0.0
080
-0.0
27-0
.003
0-0
.012
0.0
lm05
83l1
9373
82.4
5484
-71.
0631
11.
8223
0916
.04
15.8
919
06.5
891
0.96
9-0
.017
-0.0
58-0
.01
-0.0
350.
0010
lm03
53l1
6176
85.3
1671
-66.
8604
81.
8233
5717
.26
17.1
919
60.7
184
0.90
9-0
.055
-0.1
17-0
.021
-0.0
520.
0060
lm01
35l1
9824
71.0
0415
-70.
0245
61.
8238
8317
.02
16.9
222
34.5
602
0.89
7-0
.047
-0.1
53-0
.016
-0.0
61-0
.002
0lm
0340
m67
9283
.048
16-6
6.29
128
1.82
5479
16.5
216
.22
2240
.628
80.
981
-0.0
11-0
.028
-0.0
060
-0.0
080
-0.0
020
lm00
45k1
8341
86.9
7064
-69.
8612
21.
8256
6116
.26
16.1
574
1.81
330.
991
-0.0
090
-0.0
23-0
.003
0-0
.014
-0.0
080
lm01
86n1
1896
77.3
649
-68.
9384
71.
8279
917
.18
16.9
718
30.7
491
0.94
9-0
.009
0-0
.067
-0.0
14-0
.045
0.01
3lm
0131
n108
39*
71.6
3107
-69.
2634
71.
8290
1218
.10
17.5
819
20.6
538
0.91
80.
0080
-0.1
21-0
.009
0-0
.115
0.01
lm04
15l2
3100
73.7
0022
-65.
8615
61.
8304
816
.43
16.2
415
99.5
827
0.96
1-0
.005
0-0
.065
-0.0
090
-0.0
470.
0090
lm01
66m
1307
773
.673
42-6
8.78
261
1.83
2137
16.9
617
.03
838.
6081
0.89
0.00
30-0
.133
-0.0
010
-0.0
4-0
.001
0lm
0231
l245
0187
.071
48-6
7.95
773
1.83
3426
16.6
816
.49
891.
6922
0.97
8-0
.02
-0.0
140.
0040
0.00
400.
0lm
0305
l177
9676
.786
45-6
7.20
861.
8335
4417
.40
17.2
721
37.8
799
0.96
7-0
.028
-0.0
31-0
.002
0-0
.005
00.
0050
lm01
93n1
3361
80.3
2984
-68.
2255
81.
8345
8917
.61
17.4
118
62.6
168
0.97
5-0
.013
-0.0
6-0
.007
0-0
.049
-0.0
020
lm01
21m
2486
573
.644
49-6
9.19
693
1.83
5103
16.0
515
.85
1640
.489
90.
899
-0.0
31-0
.147
-0.0
15-0
.057
-0.0
050
lm02
94k2
4995
73.9
9868
-67.
1107
81.
8383
5415
.98
15.8
131
7.85
960.
886
-0.0
57-0
.159
-0.0
29-0
.068
-0.0
030
lm03
21k2
0265
80.0
6634
-66.
4147
41.
8398
5517
.24
17.1
119
75.6
187
0.96
8-0
.029
-0.0
4-0
.001
0-0
.003
00.
0020
lm01
14k1
7880
74.0
8566
-69.
8622
81.
8420
7517
.02
16.8
521
92.6
912
0.97
4-0
.017
-0.0
31-0
.007
0-0
.015
0.00
10lm
0033
k287
284
.967
54-6
9.41
477
1.84
2642
17.2
317
.08
1838
.843
10.
945
-0.0
11-0
.113
-0.0
050
-0.0
90.
0010
lm02
13k2
5910
83.4
9101
-68.
1480
41.
8437
7817
.30
17.2
918
85.6
921
0.96
7-0
.008
0-0
.034
-0.0
050
-0.0
15-0
.001
0lm
0211
l225
1983
.288
88-6
7.93
771.
8447
6116
.59
16.4
719
18.7
507
0.96
8-0
.026
-0.0
34-0
.001
0-0
.002
00.
0030
168
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0587
l104
9182
.517
1-7
1.72
761
1.84
8852
17.2
217
.08
1264
.609
90.
93-0
.072
-0.1
16-0
.038
-0.0
74-0
.003
0lm
0195
m11
246
79.9
8669
-68.
4141
11.
8538
8617
.54
17.4
622
13.7
821
0.94
3-0
.005
0-0
.081
-0.0
050
-0.0
45-0
.003
0lm
0345
m87
3983
.847
96-6
7.00
511.
8548
0716
.14
15.8
640
4.63
160.
949
-0.0
060
-0.0
86-0
.002
0-0
.064
0.00
50lm
0057
n652
589
.446
52-7
0.29
132
1.85
5932
15.9
415
.62
1240
.720
70.
895
-0.0
32-0
.126
-0.0
080
-0.0
38-0
.0lm
0317
m68
04*
78.7
0661
-67.
3424
21.
8582
5617
.21
16.9
817
68.8
260
0.95
5-0
.007
0-0
.076
-0.0
010
-0.0
66-0
.001
0lm
0551
m80
9176
.525
53-7
0.49
753
1.85
9092
15.5
215
.12
2187
.708
00.
892
-0.0
39-0
.164
-0.0
14-0
.069
0.00
30lm
0095
m26
03*
79.7
062
-69.
7678
71.
8595
7617
.75
17.6
619
51.6
915
0.90
7-0
.002
0-0
.083
-0.0
080
-0.0
210.
0050
lm00
93m
1000
279
.259
87-6
9.45
666
1.86
0486
16.5
916
.38
554.
5324
0.93
4-0
.004
0-0
.099
-0.0
010
-0.0
46-0
.003
0lm
0424
m15
104
75.1
2583
-65.
6484
31.
8610
2116
.09
15.8
678
1.80
190.
99-0
.011
-0.0
12-0
.006
0-0
.009
00.
0010
lm03
40m
1208
383
.238
1-6
6.32
889
1.86
1203
17.2
217
.01
1820
.720
20.
976
0.00
10-0
.036
0.00
10-0
.025
0.0
lm02
41n8
563
89.3
9576
-67.
8564
41.
8614
8216
.16
15.9
315
82.7
486
0.90
1-0
.052
-0.1
27-0
.023
-0.0
58-0
.001
0lm
0022
l136
3181
.916
29-6
9.64
278
1.86
3346
16.8
316
.77
2216
.643
10.
879
-0.0
53-0
.131
-0.0
23-0
.032
0.00
40lm
0100
k615
676
.103
84-6
9.09
203
1.86
3582
16.7
416
.55
1154
.812
90.
969
-0.0
010
-0.0
36-0
.011
-0.0
2-0
.006
0lm
0455
l174
6280
.371
03-6
5.82
681.
8661
6816
.97
16.8
519
47.7
648
0.95
3-0
.001
0-0
.07
-0.0
030
-0.0
390.
0lm
0115
l932
175
.115
13-6
9.95
691
1.86
7104
16.9
916
.85
1890
.605
60.
96-0
.023
-0.0
280.
0040
0.00
200.
0030
lm00
27m
1237
2*83
.599
52-7
0.18
111.
8710
1216
.78
16.9
523
11.7
005
0.98
50.
0030
-0.0
270.
0030
-0.0
1-0
.001
0lm
0291
l253
4974
.751
74-6
6.55
471
1.87
4248
16.9
716
.84
2177
.697
50.
987
-0.0
12-0
.022
0.00
20-0
.016
-0.0
030
lm01
73m
2058
776
.253
69-6
8.11
408
1.87
4478
17.0
716
.83
851.
7610
0.98
5-0
.021
-0.0
18-0
.006
0-0
.01
-0.0
lm01
07k3
631
77.2
7077
-70.
1260
11.
8766
1817
.44
17.2
712
78.5
456
0.95
-0.0
23-0
.051
0.00
30-0
.003
0-0
.009
0lm
0540
m22
710
73.4
5325
-70.
5957
51.
8766
8116
.75
16.5
519
83.5
465
0.94
7-0
.002
0-0
.098
-0.0
010
-0.0
650.
0030
lm01
71n1
8834
76.4
9656
-67.
9603
91.
8770
9517
.29
17.2
939
0.76
270.
926
-0.0
68-0
.122
-0.0
35-0
.066
0.00
30lm
0226
k637
884
.449
84-6
8.74
611
1.87
7873
16.9
116
.94
1661
.538
10.
913
-0.0
57-0
.103
-0.0
26-0
.048
0.00
60lm
0550
k193
8575
.061
88-7
0.58
553
1.87
8439
16.1
615
.91
1154
.843
40.
93-0
.029
-0.0
76-0
.004
0-0
.02
0.00
20lm
0375
n241
3789
.195
23-6
7.27
931.
8797
7817
.11
17.1
015
90.6
778
0.98
-0.0
030
-0.0
170.
0-0
.012
0.00
10lm
0195
m92
7980
.309
64-6
8.39
999
1.88
0086
16.6
916
.47
1600
.629
80.
943
0.00
40-0
.104
0.00
60-0
.05
-0.0
010
lm01
25m
2959
973
.430
14-6
9.92
033
1.88
1055
17.7
017
.49
1815
.698
10.
959
-0.0
-0.0
750.
0-0
.054
0.01
4lm
0161
l218
3073
.968
7-6
7.98
756
1.88
166
17.0
816
.89
1491
.608
00.
957
-0.0
090
-0.0
54-0
.004
0-0
.029
-0.0
010
lm03
41n6
056
84.2
0983
-66.
4800
31.
8836
1715
.51
15.1
922
41.8
182
0.96
5-0
.016
-0.0
57-0
.007
0-0
.042
0.0
lm03
35l2
2611
81.7
3184
-67.
2499
71.
8863
8915
.86
15.6
520
20.5
398
0.98
9-0
.006
0-0
.019
-0.0
040
-0.0
140.
0lm
0015
l249
8580
.865
42-7
0.04
807
1.88
6947
16.1
415
.91
1200
.679
60.
971
-0.0
080
-0.0
37-0
.006
0-0
.019
-0.0
lm00
12n1
9000
80.5
5954
-69.
6654
81.
8879
4316
.00
15.7
111
35.7
745
0.93
2-0
.024
-0.0
78-0
.007
0-0
.019
0.0
lm05
45n1
9142
74.5
0541
-71.
4139
11.
8880
9516
.81
16.5
948
0.75
770.
963
-0.0
010
-0.0
540.
0010
-0.0
35-0
.003
0lm
0175
m26
832*
76.4
5506
-68.
5012
31.
8896
817
.01
16.8
912
34.6
289
0.97
3-0
.008
0-0
.026
-0.0
020
-0.0
090
0.0
lm01
84n1
8118
77.4
2301
-68.
6105
41.
8907
2316
.61
16.3
320
57.4
846
0.93
8-0
.034
-0.0
570.
0010
-0.0
090
0.00
40lm
0030
l102
7784
.178
94-6
9.27
775
1.89
0838
17.2
817
.22
1869
.624
80.
974
-0.0
19-0
.04
-0.0
010
-0.0
11-0
.006
0lm
0347
l129
8283
.777
51-6
7.55
415
1.89
1817
15.5
815
.49
2027
.573
90.
907
-0.0
26-0
.126
-0.0
12-0
.051
0.00
20lm
0011
n177
8381
.625
21-6
9.30
326
1.90
002
17.5
617
.20
562.
5280
0.97
3-0
.026
-0.0
47-0
.01
-0.0
420.
0040
lm02
12m
1916
982
.750
26-6
8.15
107
1.90
0405
15.6
815
.60
1599
.642
10.
899
-0.0
26-0
.13
-0.0
1-0
.037
0.0
lm04
66n2
0073
81.5
8242
-66.
1981
81.
9005
0217
.08
16.8
919
12.7
399
0.95
8-0
.041
-0.0
48-0
.005
0-0
.009
00.
0lm
0013
m74
6681
.514
09-6
9.44
365
1.90
3719
15.6
315
.31
342.
7785
0.92
3-0
.018
-0.0
92-0
.006
0-0
.027
0.00
10lm
0217
n174
3383
.921
03-6
8.98
272
1.90
6896
16.3
216
.29
2228
.653
70.
973
-0.0
040
-0.0
49-0
.001
0-0
.033
0.00
40
169
lm00
93m
2803
279
.546
09-6
9.54
877
1.90
8406
17.2
517
.14
401.
6675
0.99
-0.0
37-0
.024
-0.0
3-0
.018
-0.0
040
lm04
55l8
958
80.5
1532
-65.
7637
21.
9097
7316
.78
16.5
712
72.5
857
0.98
8-0
.002
0-0
.015
-0.0
020
-0.0
040
0.00
10lm
0164
n288
4973
.446
2-6
8.68
422
1.91
087
17.3
517
.24
1610
.559
00.
965
-0.0
31-0
.045
-0.0
030
-0.0
110.
0lm
0355
n173
3185
.982
05-6
7.29
131
1.91
4858
17.4
617
.28
1533
.729
80.
922
-0.0
58-0
.116
-0.0
23-0
.052
0.00
20lm
0424
n245
1675
.052
72-6
5.88
275
1.91
5386
15.6
915
.41
1529
.608
30.
986
-0.0
11-0
.027
-0.0
060
-0.0
12-0
.001
0lm
0447
m19
131
79.2
3011
-66.
0312
1.91
5947
16.4
316
.15
2164
.755
20.
978
-0.0
21-0
.037
-0.0
090
-0.0
19-0
.001
0lm
0220
m11
743
84.8
8121
-67.
7282
61.
9172
6117
.11
16.9
017
45.8
922
0.96
6-0
.027
-0.0
20.
00.
0010
0.00
90lm
0333
n161
8782
.206
17-6
6.84
772
1.91
737
15.9
615
.71
1495
.850
80.
962
-0.0
080
-0.0
53-0
.005
0-0
.022
0.0
lm03
54k2
785
84.4
5844
-66.
9705
81.
9180
1517
.61
17.4
419
72.6
113
0.97
5-0
.014
-0.0
3-0
.007
0-0
.009
0-0
.001
0lm
0194
k170
0278
.717
17-6
8.44
985
1.91
8376
17.1
016
.99
792.
7186
0.97
-0.0
14-0
.034
-0.0
020
-0.0
170.
0010
lm03
55l1
8117
85.4
6136
-67.
2273
1.91
8576
17.5
417
.41
1297
.574
60.
97-0
.019
-0.0
280.
00.
0020
0.00
20lm
0014
k224
3580
.153
28-6
9.88
395
1.91
8806
16.7
116
.57
1945
.746
00.
969
-0.0
22-0
.029
0.00
20-0
.001
00.
0040
lm01
11k2
6219
*74
.923
94-6
9.20
579
1.91
9088
17.3
217
.24
1913
.686
20.
950.
0010
-0.0
89-0
.004
0-0
.044
-0.0
020
lm02
11l2
2349
83.2
0144
-67.
9369
91.
9198
216
.58
16.4
922
58.6
050
0.86
9-0
.057
-0.1
87-0
.034
-0.0
80.
0040
lm05
86m
2618
582
.159
01-7
1.66
707
1.92
0948
15.8
615
.57
456.
8295
0.95
7-0
.021
-0.0
44-0
.004
0-0
.011
0.00
70lm
0100
m15
042*
76.3
4099
-69.
1476
1.92
189
17.2
117
.17
1842
.820
30.
946
-0.0
030
-0.0
420.
0050
-0.0
120.
0040
lm05
95l1
8614
84.6
8188
-71.
4147
11.
9232
2316
.89
16.7
820
48.4
974
0.97
-0.0
22-0
.032
-0.0
030
-0.0
070
0.0
lm00
91l5
423
79.0
5376
-69.
2368
1.92
3877
16.9
016
.97
2259
.620
70.
979
-0.0
21-0
.011
-0.0
010
0.00
300.
0050
lm05
90n5
052
84.3
154
-70.
6362
61.
9250
1217
.42
17.3
222
97.7
623
0.88
7-0
.073
-0.1
49-0
.026
-0.0
610.
0090
lm03
01l2
2532
76.4
6532
-66.
5436
61.
9251
0116
.21
15.9
717
31.9
349
0.92
4-0
.049
-0.1
22-0
.019
-0.0
470.
0020
lm01
87k1
7340
77.8
906
-68.
8109
71.
9257
7617
.04
16.8
618
70.6
228
0.90
4-0
.065
-0.1
45-0
.029
-0.0
71-0
.007
0lm
0113
k262
9274
.915
11-6
9.54
491
1.92
7036
16.4
416
.41
2027
.523
80.
97-0
.021
-0.0
33-0
.005
0-0
.005
00.
0030
lm03
06m
3943
75.9
4557
-67.
3222
51.
9272
4116
.77
16.7
118
42.8
157
0.95
50.
0010
-0.0
74-0
.003
0-0
.049
-0.0
060
lm03
51l9
504
85.3
3408
-66.
4634
91.
9283
3617
.56
17.4
112
36.6
965
0.91
8-0
.001
0-0
.131
0.00
20-0
.096
-0.0
030
lm03
55m
1625
185
.785
6-6
7.05
684
1.92
9207
17.3
117
.15
1860
.669
50.
955
-0.0
11-0
.052
-0.0
040
-0.0
090
0.00
10lm
0223
n141
0585
.573
37-6
8.23
561.
9298
7615
.54
15.3
410
64.8
019
0.94
9-0
.027
-0.0
64-0
.009
0-0
.026
0.00
10lm
0213
m21
940*
83.9
8845
-68.
1243
21.
9299
0817
.30
17.0
614
70.6
691
0.93
-0.0
040
-0.1
05-0
.003
0-0
.071
0.00
90lm
0333
k393
081
.894
61-6
6.62
161
1.93
1105
16.7
716
.61
1424
.885
30.
968
-0.0
15-0
.023
-0.0
020
-0.0
020
-0.0
010
lm01
93k2
5506
79.7
946
-68.
1418
51.
9312
4417
.31
17.3
422
02.6
715
0.96
8-0
.021
-0.0
36-0
.005
0-0
.013
0.00
10lm
0612
l107
9187
.822
47-7
1.03
349
1.93
1428
16.8
716
.73
1935
.765
10.
963
-0.0
31-0
.052
-0.0
080
-0.0
220.
0020
lm00
40l1
0857
85.8
5925
-69.
2738
1.93
296
15.7
115
.73
1870
.716
40.
954
-0.0
11-0
.066
-0.0
030
-0.0
410.
0010
lm04
36m
1006
9*76
.660
67-6
5.98
062
1.93
3416
.63
16.4
215
77.6
794
0.94
30.
0020
-0.1
070.
0010
-0.0
67-0
.003
0lm
0593
k191
27*
84.8
9216
-70.
9041
41.
9337
1217
.28
17.2
421
87.8
067
0.99
20.
0-0
.028
-0.0
020
-0.0
12-0
.002
0lm
0324
n940
579
.595
24-6
7.16
281.
9393
216
.36
16.2
351
0.59
970.
894
-0.0
64-0
.157
-0.0
31-0
.082
0.00
50lm
0214
l242
2882
.464
17-6
8.66
476
1.94
0698
16.1
115
.92
1643
.536
10.
983
-0.0
070
-0.0
23-0
.005
0-0
.011
0.00
30lm
0175
m19
864
76.6
5556
-68.
4602
91.
9465
9116
.35
16.0
136
1.86
580.
982
-0.0
16-0
.035
-0.0
080
-0.0
22-0
.0lm
0184
k175
9976
.655
75-6
8.46
017
1.94
6593
16.4
316
.19
2185
.858
20.
976
-0.0
23-0
.037
-0.0
1-0
.024
0.0
lm02
87k5
453*
73.2
6482
-67.
3371
41.
9466
2216
.78
16.5
518
51.5
814
0.92
7-0
.008
0-0
.095
-0.0
010
-0.0
350.
0020
lm03
45k1
1158
83.6
8483
-67.
0275
51.
9469
1215
.29
15.0
639
8.77
370.
872
-0.0
49-0
.173
-0.0
19-0
.076
0.0
lm03
62n1
8001
*86
.561
98-6
6.88
331
1.95
0688
17.3
217
.31
1125
.682
60.
978
-0.0
040
-0.0
23-0
.002
0-0
.001
0-0
.0lm
0331
l193
8281
.996
02-6
6.52
695
1.95
1358
15.8
715
.63
837.
7715
0.90
4-0
.052
-0.1
39-0
.02
-0.0
590.
0010
170
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0107
n205
3577
.441
38-7
0.40
098
1.95
3697
17.2
617
.07
1442
.794
00.
959
-0.0
12-0
.029
-0.0
080
-0.0
160.
0050
lm00
33m
2217
785
.459
51-6
9.53
269
1.95
4291
15.6
715
.66
1079
.823
80.
939
-0.0
030
-0.0
74-0
.001
0-0
.041
-0.0
010
lm03
14n5
827*
77.8
8079
-67.
1447
1.95
5694
16.9
916
.78
1898
.598
60.
967
-0.0
070
-0.0
5-0
.002
0-0
.033
0.0
lm00
32l1
2916
83.9
4649
-69.
6421
81.
9604
5915
.77
15.6
620
26.5
388
0.98
-0.0
15-0
.038
-0.0
050
-0.0
270.
0020
lm01
91n9
387*
80.2
9841
-67.
9263
61.
9627
516
.74
16.4
479
9.83
490.
957
0.01
1-0
.097
-0.0
040
-0.0
790.
0010
lm00
30k1
2130
*84
.071
57-6
9.13
973
1.96
284
17.0
817
.00
2063
.491
40.
959
-0.0
020
-0.0
76-0
.002
0-0
.055
-0.0
010
lm00
24m
7851
82.3
537
-69.
8022
11.
9662
6817
.28
17.2
322
43.6
361
0.89
90.
0060
-0.1
530.
0030
-0.1
020.
0lm
0170
l146
5174
.949
12-6
7.89
419
1.96
7818
17.6
017
.50
2334
.573
60.
935
-0.0
19-0
.101
-0.0
090
-0.0
27-0
.004
0lm
0294
n623
0*74
.468
89-6
7.14
491
1.96
9417
.02
16.8
515
27.5
936
0.99
3-0
.001
0-0
.019
-0.0
040
-0.0
160.
0030
lm01
23k1
2359
73.0
1024
-69.
4713
81.
9695
7415
.85
15.6
922
51.7
679
0.97
7-0
.005
0-0
.018
-0.0
020
-0.0
040
0.00
20lm
0165
l188
86*
74.2
6136
-68.
6112
41.
9747
9417
.35
17.3
415
32.5
938
0.89
4-0
.003
0-0
.145
-0.0
030
-0.0
570.
0010
lm00
91m
3031
679
.316
3-6
9.22
21.
9787
6116
.83
16.7
853
0.55
690.
928
-0.0
42-0
.105
-0.0
21-0
.052
0.00
10lm
0090
l129
95*
78.0
6702
-69.
2912
21.
9823
4216
.86
16.7
817
55.8
747
0.93
20.
0070
-0.0
530.
0030
-0.0
150.
0030
lm03
20l2
2546
*79
.329
81-6
6.55
835
1.98
4791
516
.37
16.1
321
83.7
525
0.92
6-0
.066
-0.1
16-0
.025
-0.0
67-0
.009
0lm
0020
k121
15*
81.9
8923
-69.
1416
91.
9894
755
14.4
014
.14
506.
5490
0.97
2-0
.013
-0.0
27-0
.002
0-0
.009
00.
0030
lm01
01n2
3916
*77
.416
95-6
9.34
105
1.99
006
14.6
214
.32
1154
.812
90.
863
-0.0
19-0
.184
-0.0
030
-0.0
720.
0070
lm00
25n1
5353
*83
.669
55-6
9.98
922
1.99
0814
16.6
316
.40
1916
.594
40.
972
-0.0
14-0
.029
-0.0
030
-0.0
0.00
10lm
0031
n230
92*
85.4
9733
-69.
3481
52.
0188
3217
.28
17.1
713
75.9
103
0.96
10.
0050
-0.0
460.
0010
-0.0
150.
0010
lm00
15n1
0153
*81
.448
54-6
9.95
987
2.02
0196
17.2
417
.20
1396
.903
60.
987
0.0
-0.0
180.
0-0
.01
0.00
10lm
0344
l255
1882
.610
61-6
7.28
287
2.02
3458
16.5
816
.42
2027
.573
90.
915
-0.0
66-0
.125
-0.0
27-0
.074
-0.0
050
lm05
83k6
016
82.4
9748
-70.
8483
22.
0243
8916
.20
15.9
914
75.7
354
0.97
5-0
.012
-0.0
36-0
.008
0-0
.024
-0.0
010
lm03
06l8
041*
75.7
7498
-67.
5026
22.
0253
776
17.6
017
.43
1821
.750
30.
972
-0.0
-0.0
40.
0030
-0.0
30.
0030
lm02
83n2
4858
73.3
6237
-66.
9084
32.
0261
0216
.43
16.2
718
19.6
920
0.97
6-0
.021
-0.0
47-0
.01
-0.0
320.
0020
lm05
61l1
5749
78.0
7403
-70.
6912
22.
0287
6417
.39
17.2
818
54.6
210
0.94
60.
0060
-0.0
580.
0030
-0.0
-0.0
010
lm03
66l1
5212
86.1
8124
-67.
5631
2.02
9431
15.7
215
.48
2033
.544
70.
973
-0.0
14-0
.034
-0.0
030
-0.0
010
0.00
30lm
0551
n105
0376
.505
45-7
0.66
306
2.03
144
15.8
515
.58
1881
.617
10.
991
-0.0
11-0
.012
0.0
-0.0
010
0.00
30lm
0323
l287
4179
.892
95-6
6.92
704
2.03
2993
17.5
017
.45
2344
.612
91.
003
-0.0
2-0
.034
-0.0
020
-0.0
25-0
.0lm
0632
l146
3792
.275
26-7
1.08
018
2.03
3454
16.5
016
.67
384.
7207
0.96
5-0
.021
-0.0
42-0
.009
0-0
.014
0.00
20lm
0307
l175
4276
.760
1-6
7.58
324
2.03
4164
15.6
415
.33
1628
.528
00.
99-0
.01
-0.0
17-0
.0-0
.0-0
.0lm
0386
l175
76*
89.9
2579
-67.
6368
12.
0417
117
.96
17.7
815
68.7
252
0.91
60.
011
-0.1
330.
0010
-0.1
03-0
.01
lm01
21l2
2166
72.9
5621
-69.
3845
62.
0424
4214
.94
14.9
721
30.7
894
0.98
6-0
.002
0-0
.016
-0.0
020
-0.0
1-0
.0lm
0310
n185
7478
.059
85-6
6.54
982.
0437
4316
.92
16.7
911
29.6
499
0.98
6-0
.019
-0.0
17-0
.001
0-0
.001
00.
0020
lm00
33k1
1169
85.0
617
-69.
4663
72.
0439
6315
.32
15.1
413
81.9
065
0.87
2-0
.038
-0.1
79-0
.013
-0.0
780.
0010
lm02
96m
1445
874
.261
1-6
7.39
555
2.04
4072
15.5
015
.30
2198
.628
00.
923
-0.0
3-0
.091
-0.0
060
-0.0
260.
0050
lm03
23k3
395
80.0
2339
-66.
6192
32.
0466
9417
.04
17.1
222
24.7
712
0.93
1-0
.049
-0.1
23-0
.027
-0.0
75-0
.001
0lm
0394
m95
36*
92.0
4965
-67.
0156
32.
0480
4416
.82
16.6
121
40.8
873
0.94
0.00
30-0
.119
0.00
40-0
.096
-0.0
010
lm04
27n1
2788
*76
.053
93-6
6.15
369
2.04
8492
17.7
717
.66
1764
.841
50.
95-0
.003
0-0
.061
-0.0
010
-0.0
370.
0040
lm01
84n1
1334
77.1
8704
-68.
5739
12.
0488
4517
.19
17.0
318
92.8
390
0.93
40.
0010
-0.0
98-0
.009
0-0
.066
-0.0
020
lm01
81l1
5831
77.9
7285
-67.
8912
62.
0499
6516
.44
16.2
510
91.7
610
0.93
8-0
.026
-0.0
63-0
.005
0-0
.012
0.00
30lm
0177
l228
2176
.204
12-6
9.01
093
2.05
0346
16.3
816
.07
403.
7508
0.95
8-0
.013
-0.0
53-0
.012
-0.0
320.
0030
lm03
23k1
6171
80.1
1238
-66.
6972
82.
0509
6417
.04
16.9
643
4.75
520.
903
-0.1
02-0
.141
-0.0
4-0
.076
0.00
30
171
lm02
07k2
7793
*81
.773
97-6
8.87
582.
0549
9417
.11
16.9
419
55.6
861
0.93
7-0
.013
-0.0
59-0
.002
0-0
.012
0.00
10lm
0214
l232
5782
.606
28-6
8.65
832.
0565
0517
.55
17.4
221
30.8
364
0.96
5-0
.023
-0.0
4-0
.009
0-0
.034
0.00
60lm
0454
l249
5679
.677
53-6
5.88
205
2.05
7119
16.4
616
.26
1109
.817
70.
985
-0.0
14-0
.026
-0.0
1-0
.019
0.00
10lm
0467
m13
027*
82.4
3788
-65.
9909
92.
0578
661
16.3
616
.13
1977
.644
60.
925
0.00
30-0
.089
-0.0
020
-0.0
32-0
.002
0lm
0030
l128
6684
.005
75-6
9.29
671
2.05
8756
15.6
915
.62
2223
.628
80.
948
-0.0
27-0
.065
-0.0
070
-0.0
2-0
.001
0lm
0101
m21
049
77.6
1272
-69.
1768
62.
0591
9815
.91
15.7
520
93.9
045
0.92
5-0
.014
-0.0
87-0
.005
0-0
.014
-0.0
050
lm02
17n1
1196
83.9
752
-68.
9330
82.
0592
6516
.00
15.7
811
97.6
603
0.99
2-0
.007
0-0
.014
-0.0
010
-0.0
050
-0.0
010
lm00
31l2
6732
85.0
0806
-69.
3696
62.
0607
8717
.38
17.3
515
81.6
987
0.97
7-0
.007
0-0
.081
-0.0
020
-0.0
69-0
.009
0lm
0346
m26
007*
83.1
9507
-67.
4804
2.06
2730
116
.92
16.7
519
52.6
230
0.90
9-0
.001
0-0
.138
-0.0
090
-0.0
820.
0lm
0347
m24
253
84.1
2629
-67.
4671
2.06
2809
16.8
416
.64
1618
.682
10.
984
-0.0
1-0
.045
-0.0
090
-0.0
250.
0030
lm00
15m
3337
0*81
.495
03-6
9.92
983
2.06
4046
16.7
116
.46
775.
8333
0.87
3-0
.004
0-0
.166
0.00
10-0
.058
0.00
10lm
0581
l215
36*
82.6
2171
-70.
7256
22.
0641
1617
.37
17.2
219
01.8
440
0.96
-0.0
23-0
.096
-0.0
080
-0.0
81-0
.003
0lm
0021
l660
983
.013
33-6
9.24
357
2.06
4204
15.8
015
.57
384.
7892
0.87
7-0
.058
-0.1
56-0
.022
-0.0
760.
0060
lm01
03n1
9330
*77
.574
42-6
9.65
899
2.06
4678
16.7
816
.51
2185
.653
20.
981
0.01
3-0
.051
0.00
50-0
.038
-0.0
010
lm01
82k1
6150
*76
.836
47-6
8.12
493
2.06
5838
16.3
116
.18
2227
.610
90.
991
-0.0
020
-0.0
380.
0070
-0.0
090
-0.0
020
lm03
40m
1595
082
.986
13-6
6.35
673
2.06
6753
15.7
815
.54
402.
6230
0.98
9-0
.009
0-0
.021
-0.0
050
-0.0
070
-0.0
lm02
94k3
0560
73.8
5571
-67.
0603
82.
0669
5916
.48
16.4
011
50.6
036
0.98
20.
0020
-0.0
54-0
.002
0-0
.039
-0.0
13lm
0606
m11
871
86.4
4399
-71.
5754
72.
0718
4717
.05
16.9
617
52.8
762
0.97
4-0
.025
-0.0
30.
00.
0030
0.0
lm00
13k3
0220
*81
.044
65-6
9.56
256
2.07
2228
17.1
417
.15
2218
.845
20.
972
0.00
40-0
.071
-0.0
050
-0.0
59-0
.001
0lm
0030
k163
4284
.145
84-6
9.17
465
2.07
2852
16.2
516
.14
2225
.702
20.
963
-0.0
21-0
.077
-0.0
070
-0.0
6-0
.006
0lm
0344
m10
932
83.2
9023
-67.
0270
52.
0773
7115
.94
15.7
117
76.8
603
0.98
-0.0
080
-0.0
23-0
.004
0-0
.008
00.
0020
lm00
30n2
0233
84.2
28-6
9.38
287
2.07
7922
15.9
115
.78
2141
.853
50.
99-0
.006
0-0
.021
0.0
-0.0
070
-0.0
010
lm05
87l1
8183
*82
.605
52-7
1.78
322
2.07
7996
16.7
016
.59
1277
.548
10.
972
0.00
30-0
.029
0.00
20-0
.006
0-0
.0lm
0364
n128
0286
.753
11-6
7.19
625
2.07
8818
16.8
416
.67
1336
.476
30.
909
0.00
40-0
.14
0.00
10-0
.077
-0.0
020
lm01
20n2
8365
72.6
6602
-69.
3786
42.
0793
1516
.75
16.6
110
90.6
622
0.97
1-0
.006
0-0
.027
-0.0
050
-0.0
140.
0060
lm03
20n1
1672
79.7
1178
-66.
4789
32.
0822
4717
.40
17.2
718
34.7
450
0.97
9-0
.03
-0.0
23-0
.003
00.
0010
-0.0
040
lm03
76m
1986
188
.630
75-6
7.48
616
2.08
2899
16.8
416
.59
1910
.838
90.
985
0.00
60-0
.042
0.00
20-0
.025
-0.0
030
lm01
35k2
2834
71.1
4445
-69.
8975
22.
0860
7516
.83
16.7
714
04.7
858
0.95
5-0
.003
0-0
.072
-0.0
030
-0.0
37-0
.004
0lm
0216
l176
0282
.583
84-6
8.98
538
2.08
8156
16.0
915
.90
2155
.804
70.
94-0
.008
0-0
.107
-0.0
040
-0.0
790.
0030
lm02
83l8
947
73.2
4627
-66.
8092
82.
0882
2516
.07
15.9
025
75.5
757
0.94
1-0
.003
0-0
.085
-0.0
030
-0.0
560.
0030
lm03
53k1
3716
85.4
3765
-66.
6865
72.
0904
17.1
517
.04
2183
.806
10.
982
0.0
-0.0
37-0
.011
-0.0
190.
0090
lm03
74l1
5319
87.9
8088
-67.
2202
52.
0905
4716
.63
16.4
416
30.5
740
0.90
4-0
.055
-0.1
07-0
.024
-0.0
330.
01lm
0120
n118
1072
.364
81-6
9.27
577
2.09
0994
16.6
916
.56
1867
.564
60.
984
-0.0
1-0
.021
-0.0
030
-0.0
070
0.0
lm00
21n1
4065
83.6
9031
-69.
2812
52.
0919
7317
.16
17.0
181
8.81
440.
963
-0.0
12-0
.077
-0.0
010
-0.0
53-0
.007
0lm
0017
k186
80*
80.8
4479
-70.
2232
22.
0940
4817
.30
17.3
625
35.8
269
0.96
10.
0-0
.055
0.00
40-0
.025
-0.0
010
lm04
26n2
3242
*75
.023
46-6
6.21
718
2.09
473
16.6
716
.37
1982
.543
50.
944
-0.0
030
-0.0
80.
0020
-0.0
560.
0lm
0311
k116
3478
.245
1-6
6.33
708
2.09
5304
16.9
816
.74
1997
.551
00.
987
-0.0
090
-0.0
19-0
.001
0-0
.004
00.
0010
lm05
43m
1126
7*74
.621
18-7
0.85
887
2.09
621
16.8
916
.78
1291
.488
90.
876
-0.0
040
-0.1
7-0
.001
0-0
.077
0.00
20lm
0284
n240
9172
.427
96-6
7.28
827
2.09
8031
17.2
317
.15
1546
.747
40.
976
-0.0
29-0
.024
0.00
200.
0010
0.00
80lm
0120
n120
6472
.711
61-6
9.27
655
2.09
9324
17.0
716
.96
2344
.525
30.
928
-0.0
12-0
.067
-0.0
050
-0.0
030
-0.0
010
lm00
20k1
8818
81.9
151
-69.
1884
42.
1014
9115
.79
15.5
715
55.6
796
0.96
4-0
.002
0-0
.044
-0.0
020
-0.0
22-0
.0
172
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0184
k771
476
.919
56-6
8.40
232
2.10
2557
15.4
115
.21
1842
.823
60.
977
-0.0
11-0
.021
0.00
10-0
.002
0-0
.003
0lm
0211
k229
00*
83.5
6939
-67.
7899
52.
1039
9817
.58
17.4
319
45.7
784
0.98
1-0
.009
0-0
.039
-0.0
040
-0.0
330.
0010
lm03
46n1
1026
83.2
7558
-67.
5331
62.
1082
7815
.35
15.0
920
53.5
015
0.97
4-0
.008
0-0
.046
-0.0
020
-0.0
350.
0lm
0121
n196
9773
.299
7-6
9.31
924
2.10
8675
17.2
317
.13
871.
5515
0.96
-0.0
090
-0.0
52-0
.001
0-0
.03
0.00
10lm
0090
n289
7778
.400
84-6
9.37
809
2.10
8725
16.4
516
.36
455.
8341
0.94
2-0
.026
-0.1
11-0
.014
-0.0
840.
0020
lm02
10n2
4868
82.9
734
-67.
9606
52.
1137
516
.60
16.4
014
70.6
691
0.93
6-0
.012
-0.0
880.
0030
-0.0
39-0
.004
0lm
0585
k286
782
.670
01-7
1.16
974
2.11
3799
17.3
317
.26
1566
.628
80.
945
-0.0
1-0
.058
-0.0
11-0
.016
0.00
30lm
0014
l168
0680
.071
67-7
0.01
212.
1162
7417
.35
17.1
914
42.8
081
0.91
50.
0090
-0.1
28-0
.006
0-0
.086
-0.0
040
lm01
84k2
7793
*76
.918
22-6
8.52
216
2.11
6352
17.4
717
.45
1749
.927
00.
948
-0.0
080
-0.0
65-0
.004
0-0
.013
-0.0
020
lm03
40l8
015
82.7
471
-66.
4597
62.
1178
6615
.86
15.6
510
75.7
470
0.95
7-0
.019
-0.0
520.
0-0
.009
00.
01lm
0447
m16
378
79.0
9147
-66.
0132
72.
1199
3816
.71
16.4
911
53.6
390
0.97
8-0
.011
-0.0
37-0
.01
-0.0
2-0
.003
0lm
0285
k419
373
.283
19-6
6.97
343
2.12
335
15.5
915
.46
1867
.570
20.
984
-0.0
16-0
.012
-0.0
040
-0.0
050
0.00
10lm
0345
k762
883
.437
81-6
7.00
561
2.12
3454
15.3
715
.18
1169
.796
50.
965
-0.0
050
-0.0
44-0
.002
0-0
.017
0.00
10lm
0111
k672
274
.884
13-6
9.08
629
2.12
4105
17.0
516
.86
1374
.888
70.
953
-0.0
030
-0.0
630.
0020
-0.0
330.
0020
lm01
31m
1381
9*71
.702
55-6
9.13
283
2.12
4317
.22
17.0
821
95.6
001
0.91
40.
0020
-0.1
14-0
.002
0-0
.038
0.00
60lm
0020
l916
382
.077
43-6
9.26
829
2.12
7403
16.2
215
.96
1164
.721
20.
981
-0.0
21-0
.021
-0.0
-0.0
010
-0.0
010
lm01
64l8
885
73.0
8891
-68.
5636
42.
1294
6917
.09
16.9
622
45.7
783
0.97
6-0
.013
-0.0
37-0
.004
0-0
.013
0.00
10lm
0831
m87
3886
.437
87-7
3.42
908
2.13
2923
17.3
517
.38
1920
.786
50.
931
-0.0
050
-0.1
01-0
.004
0-0
.051
0.00
30lm
0214
k135
9082
.360
9-6
8.43
753
2.13
3649
17.2
117
.14
950.
4813
0.96
5-0
.023
-0.0
250.
0020
0.00
30-0
.0lm
0164
m11
674
73.6
4248
-68.
4231
72.
1361
617
.16
17.0
622
14.6
954
0.94
3-0
.005
0-0
.07
0.00
10-0
.025
0.00
20lm
0327
m55
6280
.564
02-6
7.33
692.
1370
4616
.20
15.9
414
23.8
485
0.97
-0.0
16-0
.026
-0.0
-0.0
010
0.00
20lm
0557
n520
876
.487
16-7
1.68
366
2.13
7119
15.5
315
.16
2251
.633
70.
949
-0.0
020
-0.0
68-0
.002
0-0
.028
0.00
10lm
0335
n145
4282
.378
6-6
7.18
996
2.13
9656
17.2
116
.97
1751
.858
20.
946
-0.0
090
-0.0
94-0
.007
0-0
.071
-0.0
090
lm00
93n2
2090
*79
.416
49-6
9.67
019
2.14
0468
17.5
517
.57
1622
.544
20.
975
-0.0
040
-0.0
40.
0080
-0.0
35-0
.0lm
0574
m16
657
79.9
4568
-71.
2485
42.
1407
5615
.98
15.8
219
30.6
592
0.93
9-0
.02
-0.0
95-0
.011
-0.0
70.
0lm
0157
m11
115
72.8
539
-68.
7723
82.
1417
617
.16
16.9
923
30.5
523
0.94
8-0
.026
-0.0
52-0
.006
0-0
.012
-0.0
020
lm01
15k2
3126
74.8
9513
-69.
8848
92.
1422
1817
.25
17.2
213
81.9
210
0.98
2-0
.003
0-0
.05
0.00
20-0
.038
-0.0
030
lm03
64k5
553
86.2
3784
-66.
9894
82.
1438
2116
.65
16.4
922
45.8
514
0.98
9-0
.016
-0.0
140.
0010
0.0
-0.0
010
lm03
17k3
682
78.4
3808
-67.
3299
12.
1452
3916
.24
15.9
722
57.6
240
0.95
6-0
.011
-0.0
63-0
.007
0-0
.041
0.00
70lm
0013
l323
6580
.913
83-6
9.72
612.
1457
5516
.15
16.1
838
0.70
201.
025
-0.0
020
-0.0
28-0
.001
0-0
.026
-0.0
020
lm02
80n2
3309
72.7
8232
-66.
5674
22.
1464
0816
.90
16.7
417
68.7
941
0.94
4-0
.035
-0.0
59-0
.008
0-0
.017
0.00
20lm
0031
l948
0*84
.971
1-6
9.25
849
2.14
9394
17.1
017
.26
2206
.656
50.
97-0
.001
0-0
.063
-0.0
060
-0.0
22-0
.005
0lm
0365
l953
287
.078
31-6
7.16
921
2.14
9591
17.3
717
.26
1076
.849
70.
914
-0.0
98-0
.131
-0.0
46-0
.087
0.00
10lm
0354
l792
384
.426
79-6
7.15
897
2.14
9846
17.2
317
.07
1078
.871
10.
998
-0.0
32-0
.024
-0.0
21-0
.017
0.00
40lm
0331
m11
496
82.3
5971
-66.
3166
42.
1514
7315
.98
15.6
794
7.50
960.
967
-0.0
15-0
.026
0.00
10-0
.001
00.
0040
lm01
84k1
2216
76.6
4318
-68.
4287
22.
1544
7515
.51
15.1
912
81.5
396
0.94
20.
0020
-0.0
9-0
.006
0-0
.054
-0.0
010
lm01
75m
1431
076
.642
87-6
8.42
884
2.15
4499
15.1
914
.95
351.
8527
0.97
1-0
.003
0-0
.08
0.00
40-0
.064
-0.0
080
lm02
85m
2081
773
.351
47-6
7.08
557
2.15
5777
16.2
416
.18
1619
.530
50.
986
-0.0
090
-0.0
27-0
.005
0-0
.022
-0.0
020
lm01
12n2
0997
74.4
3411
-69.
7480
82.
1565
0316
.45
16.3
242
8.62
440.
942
-0.0
25-0
.068
-0.0
060
-0.0
190.
0030
lm02
04k1
1078
*80
.589
88-6
8.41
759
2.15
745
16.9
116
.90
327.
8730
0.98
1-0
.004
0-0
.026
-0.0
030
-0.0
110.
0010
lm00
25n2
2937
83.3
5719
-70.
0313
82.
1578
7415
.35
15.1
922
33.5
777
0.99
5-0
.013
-0.0
070
-0.0
010
-0.0
010
-0.0
173
lm03
75k1
9793
88.8
2509
-67.
0947
92.
1586
9116
.43
16.3
016
41.5
539
0.93
1-0
.005
0-0
.078
-0.0
030
-0.0
18-0
.002
0lm
0016
n213
06*
80.6
1341
-70.
3948
2.15
9334
17.0
016
.83
1763
.805
80.
883
-0.0
81-0
.172
-0.0
43-0
.092
-0.0
020
lm03
77m
4439
89.3
4411
-67.
3373
12.
1603
3517
.52
17.2
821
98.7
009
0.96
4-0
.043
-0.0
52-0
.003
0-0
.013
-0.0
020
lm00
14m
1670
080
.303
62-6
9.84
745
2.16
0507
17.3
417
.26
1771
.884
10.
945
-0.0
080
-0.0
87-0
.012
-0.0
67-0
.003
0lm
0344
k168
5482
.613
13-6
7.06
915
2.16
4252
16.0
015
.81
533.
5582
0.96
6-0
.009
0-0
.077
-0.0
030
-0.0
580.
0030
lm00
31m
1900
185
.263
59-6
9.17
275
2.16
5249
17.1
917
.32
1150
.740
30.
954
-0.0
34-0
.08
-0.0
080
-0.0
26-0
.01
lm03
21m
8452
80.6
0069
-66.
2937
52.
1682
2116
.88
16.5
581
9.82
270.
974
-0.0
17-0
.027
0.0
-0.0
010
-0.0
010
lm03
17k5
360
78.5
1571
-67.
3418
32.
1697
1615
.68
15.4
578
6.83
200.
984
-0.0
090
-0.0
16-0
.003
0-0
.007
00.
0040
lm01
22m
5050
*72
.741
68-6
9.43
543
2.16
9742
16.3
616
.15
2172
.692
20.
966
-0.0
16-0
.067
-0.0
1-0
.047
-0.0
010
lm04
76n8
386*
83.5
0353
-66.
1080
62.
1700
301
17.2
117
.07
2236
.603
00.
886
-0.0
070
-0.1
490.
0040
-0.0
640.
0060
lm02
14n1
0775
*82
.998
-68.
5720
92.
1757
2817
.39
17.2
311
66.6
841
0.98
2-0
.015
-0.0
28-0
.01
-0.0
230.
0020
lm01
04k1
0462
76.1
6645
-69.
8147
72.
1780
2816
.43
16.2
213
67.8
576
0.88
2-0
.016
-0.1
7-0
.003
0-0
.088
-0.0
040
lm00
12m
1679
880
.647
25-6
9.52
878
2.18
3354
15.8
415
.48
697.
8926
0.93
6-0
.02
-0.0
95-0
.015
-0.0
59-0
.002
0lm
0205
n257
4282
.169
42-6
8.69
351
2.18
4881
15.3
514
.97
1136
.851
10.
964
-0.0
050
-0.0
57-0
.011
-0.0
27-0
.0lm
0294
n133
8874
.436
11-6
7.18
884
2.18
8141
15.6
915
.44
1858
.828
20.
983
-0.0
-0.0
21-0
.012
-0.0
080
-0.0
070
lm03
66l6
375*
86.1
5242
-67.
4924
72.
1890
061
17.1
517
.00
2155
.848
70.
974
-0.0
070
-0.0
38-0
.006
0-0
.019
-0.0
030
lm05
43m
9484
*74
.378
11-7
0.85
007
2.18
9417
.29
17.1
386
4.69
090.
975
-0.0
-0.0
460.
0010
-0.0
38-0
.001
0lm
0315
m20
618*
78.8
6678
-67.
0694
52.
1919
517
.34
17.1
513
89.8
800
0.97
-0.0
060
-0.0
27-0
.003
0-0
.009
00.
0010
lm01
13m
6637
*75
.318
89-6
9.43
376
2.19
245
17.0
016
.88
1830
.710
10.
971
-0.0
040
-0.0
26-0
.001
0-0
.009
0-0
.003
0lm
0461
n156
4082
.522
2-6
5.17
632.
1925
4617
.34
17.1
214
45.8
946
0.97
4-0
.007
0-0
.031
-0.0
030
-0.0
120.
0020
lm01
91n2
265
79.9
646
-67.
8349
12.
1932
4117
.04
16.9
019
00.7
488
0.95
3-0
.015
-0.0
66-0
.008
0-0
.041
0.00
20lm
0013
m20
283
81.5
1292
-69.
5146
2.19
3383
15.3
915
.13
2255
.652
30.
969
-0.0
15-0
.034
0.0
0.0
0.0
lm01
23k1
5744
72.8
1945
-69.
4915
52.
1957
7416
.50
16.3
410
90.6
622
0.98
9-0
.031
-0.0
16-0
.009
0-0
.016
0.00
10lm
0541
n498
174
.665
65-7
0.64
066
2.19
5876
16.8
316
.48
1775
.772
00.
984
-0.0
16-0
.022
-0.0
070
-0.0
130.
0020
lm00
44n5
926
86.5
9323
-69.
9439
32.
1980
316
.92
16.9
120
17.5
920
0.88
6-0
.098
-0.1
57-0
.044
-0.0
820.
0070
lm02
81n1
4618
73.5
6365
-66.
4911
62.
1997
8617
.07
16.8
715
26.5
916
0.88
9-0
.087
-0.1
81-0
.048
-0.1
080.
0060
lm03
00m
2557
176
.144
99-6
6.41
666
2.20
0747
15.9
415
.64
1825
.702
80.
94-0
.021
-0.0
59-0
.002
0-0
.009
00.
0030
lm03
40m
1956
883
.179
12-6
6.38
233
2.20
2876
17.4
917
.25
1803
.869
20.
968
-0.0
17-0
.042
-0.0
11-0
.024
0.0
lm02
90n1
2262
74.3
59-6
6.48
642
2.20
3112
16.3
716
.21
1181
.647
00.
948
-0.0
090
-0.0
99-0
.009
0-0
.075
0.00
40lm
0370
k175
1287
.812
32-6
6.37
514
2.20
7377
17.0
716
.89
1524
.688
10.
887
-0.0
74-0
.145
-0.0
31-0
.065
0.00
40lm
0107
k229
8577
.271
91-7
0.24
754
2.20
7411
17.3
217
.09
435.
7162
0.98
0.00
50-0
.036
0.00
10-0
.024
-0.0
020
lm02
90l2
1965
73.9
6035
-66.
5757
72.
2112
9215
.93
15.8
531
7.85
960.
989
-0.0
040
-0.0
12-0
.001
0-0
.006
0-0
.003
0lm
0241
l253
9089
.188
69-6
7.97
323
2.21
4714
17.4
417
.34
365.
7348
0.97
8-0
.006
0-0
.03
-0.0
050
-0.0
210.
0010
lm06
10k4
113
87.8
5881
-70.
5359
2.21
4823
17.1
516
.98
1244
.682
30.
975
0.00
20-0
.039
-0.0
010
-0.0
29-0
.0lm
0591
n253
1485
.290
76-7
0.74
622.
2168
8716
.04
15.8
411
67.8
282
0.92
9-0
.03
-0.0
81-0
.009
0-0
.022
0.00
20lm
0220
k199
6184
.459
12-6
7.79
554
2.21
799
17.0
016
.84
2297
.769
70.
905
-0.0
69-0
.133
-0.0
28-0
.069
-0.0
040
lm00
20k1
1440
82.0
627
-69.
1366
12.
2201
6915
.22
14.9
318
69.6
092
0.97
5-0
.009
0-0
.063
-0.0
070
-0.0
46-0
.002
0lm
0203
n153
9381
.844
17-6
8.23
549
2.22
5954
15.5
215
.28
394.
7756
0.97
3-0
.012
-0.0
250.
0010
0.0
0.00
30lm
0581
k693
182
.646
45-7
0.48
988
2.22
7595
17.0
716
.87
1879
.640
20.
978
-0.0
2-0
.019
-0.0
010
-0.0
020
0.00
60lm
0230
m41
5586
.841
93-6
7.67
424
2.22
9129
17.1
616
.89
2019
.582
10.
974
-0.0
030
-0.0
52-0
.013
-0.0
27-0
.013
lm00
33m
2476
285
.328
05-6
9.54
912
2.23
0059
16.3
116
.16
837.
7160
0.98
6-0
.006
0-0
.029
-0.0
020
-0.0
21-0
.001
0
174
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0285
n464
573
.581
79-6
7.13
282.
2307
5517
.20
16.9
822
25.5
834
0.98
1-0
.012
-0.0
24-0
.005
0-0
.015
0.00
10lm
0303
n124
0376
.834
86-6
6.82
148
2.23
4478
16.6
916
.53
1860
.581
60.
944
-0.0
070
-0.0
85-0
.003
0-0
.052
0.00
10lm
0335
k267
6081
.739
43-6
7.11
696
2.23
4913
16.2
216
.09
1117
.693
30.
887
-0.0
65-0
.149
-0.0
26-0
.068
0.00
10lm
0103
l113
1677
.230
53-6
9.61
654
2.23
5387
16.8
716
.78
1272
.554
10.
976
-0.0
14-0
.032
-0.0
060
-0.0
14-0
.004
0lm
0175
k257
2475
.997
16-6
8.49
432
2.24
1225
17.2
617
.22
1153
.601
50.
932
-0.0
37-0
.1-0
.016
-0.0
41-0
.002
0lm
0301
n983
276
.878
18-6
6.45
832
2.24
2879
16.1
615
.99
1895
.745
40.
984
-0.0
12-0
.018
-0.0
060
-0.0
11-0
.0lm
0127
n214
8773
.644
13-7
0.40
732
2.24
4659
17.1
116
.88
1341
.922
30.
965
0.00
20-0
.056
-0.0
010
-0.0
41-0
.002
0lm
0200
k250
3480
.532
84-6
7.81
569
2.24
4789
16.6
516
.21
1788
.813
20.
947
-0.0
19-0
.079
-0.0
1-0
.056
0.00
40lm
0193
m14
935
79.9
7507
-68.
0820
32.
2497
9715
.10
14.8
915
70.5
930
0.96
7-0
.017
-0.0
38-0
.001
0-0
.005
00.
0020
lm00
20k2
4295
82.1
302
-69.
2279
42.
2507
0116
.27
16.0
519
16.5
944
0.97
90.
0010
-0.0
270.
0010
-0.0
130.
0010
lm03
31l1
7455
81.9
9669
-66.
5146
62.
2549
8416
.95
16.9
319
34.7
177
0.96
3-0
.001
0-0
.053
-0.0
-0.0
34-0
.0lm
0466
l152
3981
.324
46-6
6.16
268
2.25
864
16.2
215
.99
2211
.763
80.
931
-0.0
16-0
.115
-0.0
1-0
.078
0.00
40lm
0021
l327
9183
.077
67-6
9.38
839
2.25
996
16.9
416
.78
1644
.552
70.
962
-0.0
040
-0.0
720.
0010
-0.0
470.
0010
lm00
33l8
128*
85.0
0657
-69.
6018
82.
2622
781
16.0
616
.26
1838
.843
10.
927
-0.0
16-0
.122
-0.0
080
-0.0
93-0
.004
0lm
0355
k331
785
.179
43-6
6.97
744
2.26
5278
17.3
817
.32
1850
.818
21.
004
-0.0
21-0
.012
0.00
40-0
.003
0-0
.01
lm01
17m
1058
475
.354
56-7
0.17
046
2.26
826
15.6
115
.36
1139
.841
70.
973
-0.0
14-0
.023
0.0
-0.0
-0.0
010
lm05
51n1
3003
76.5
5602
-70.
6779
2.27
0432
15.4
515
.11
1861
.659
40.
991
0.00
40-0
.025
-0.0
020
-0.0
20.
0lm
0294
m26
342
74.5
6661
-67.
1114
2.27
1254
17.1
116
.95
1867
.591
50.
992
-0.0
2-0
.014
-0.0
18-0
.008
0-0
.001
0lm
0100
n569
076
.657
27-6
9.23
942.
2732
116
.90
16.7
520
09.5
280
0.90
7-0
.009
0-0
.117
-0.0
020
-0.0
56-0
.001
0lm
0030
n182
0284
.494
21-6
9.32
818
2.27
3798
16.1
315
.97
1873
.745
00.
988
-0.0
18-0
.014
-0.0
040
-0.0
110.
0010
lm05
51k2
2031
75.9
421
-70.
6197
52.
2760
117
.29
17.1
720
14.5
141
0.95
8-0
.011
-0.0
48-0
.018
-0.0
3-0
.002
0lm
0093
m18
940
79.4
1344
-69.
5021
62.
2772
2116
.57
16.3
912
72.5
694
0.98
6-0
.012
-0.0
24-0
.006
0-0
.014
-0.0
lm01
23m
1204
673
.519
01-6
9.46
607
2.27
8014
16.0
515
.96
2172
.692
20.
913
-0.0
45-0
.106
-0.0
13-0
.04
0.00
50lm
0173
l139
8575
.927
25-6
8.23
103
2.27
859
16.2
116
.06
2208
.592
50.
968
-0.0
19-0
.025
0.0
0.00
100.
0030
lm00
92m
2011
7*78
.507
88-6
9.55
312
2.27
942
16.9
116
.83
2390
.524
40.
973
-0.0
080
-0.0
26-0
.003
0-0
.012
-0.0
020
lm03
54m
1836
784
.906
15-6
7.07
169
2.27
9477
16.8
416
.74
1952
.645
90.
962
-0.0
070
-0.0
48-0
.005
0-0
.008
00.
0lm
0161
m20
878
74.5
8093
-67.
7728
92.
2795
816
.52
16.3
087
9.55
200.
968
-0.0
020
-0.0
55-0
.0-0
.034
-0.0
010
lm06
81m
1607
377
.636
93-7
1.94
809
2.28
0521
17.3
917
.16
1503
.639
20.
945
0.00
60-0
.092
-0.0
020
-0.0
66-0
.0lm
0037
m13
144*
85.3
6341
-70.
1932
12.
2806
3217
.45
17.3
110
71.8
607
0.97
40.
0030
-0.0
60.
0010
-0.0
42-0
.001
0lm
0211
m23
264
83.9
8286
-67.
7886
12.
2809
8216
.35
16.1
111
50.7
130
0.89
-0.0
56-0
.146
-0.0
26-0
.067
0.00
20lm
0117
m15
641
75.5
9811
-70.
2015
12.
2838
16.3
016
.10
442.
7809
0.98
7-0
.008
0-0
.017
0.0
-0.0
10.
0030
lm01
75n3
1573
*76
.579
35-6
8.67
835
2.28
6902
15.9
315
.87
2030
.498
10.
993
-0.0
020
-0.0
13-0
.002
0-0
.008
0-0
.001
0lm
0543
n271
9574
.728
01-7
1.10
363
2.29
3317
17.2
517
.06
1289
.507
60.
962
-0.0
31-0
.038
0.0
0.00
100.
0010
lm01
84k1
3561
*76
.855
96-6
8.43
673
2.29
4172
16.5
816
.53
418.
8373
0.98
8-0
.011
-0.0
17-0
.005
0-0
.01
-0.0
020
lm02
94n1
0273
74.3
1829
-67.
1699
52.
2989
0415
.77
15.5
622
39.7
894
0.93
1-0
.039
-0.0
9-0
.019
-0.0
420.
0070
lm03
37k2
0128
81.9
1348
-67.
4423
52.
3002
9815
.54
15.2
817
94.8
525
0.94
5-0
.014
-0.0
99-0
.006
0-0
.066
0.0
lm00
90l1
3156
78.1
5229
-69.
2921
62.
3012
6616
.70
16.5
021
84.7
283
0.87
9-0
.017
-0.1
53-0
.005
0-0
.072
-0.0
010
lm03
55n1
2209
85.7
5128
-67.
1831
42.
3037
9417
.25
17.1
513
83.8
643
0.92
7-0
.063
-0.1
08-0
.022
-0.0
420.
0040
lm03
13m
2134
878
.798
07-6
6.72
394
2.30
4919
15.6
315
.32
2545
.753
30.
958
-0.0
17-0
.043
-0.0
010
-0.0
040
-0.0
010
lm03
43l1
7247
83.7
9672
-66.
8606
92.
3084
1117
.37
17.2
810
90.6
924
0.96
0.0
-0.0
62-0
.001
0-0
.039
-0.0
010
lm03
22k2
0845
79.3
1416
-66.
7731
42.
3115
4715
.93
15.7
589
2.62
130.
918
-0.0
4-0
.097
-0.0
13-0
.033
0.00
30
175
lm05
86k1
6977
81.5
3131
-71.
6079
82.
3161
0815
.24
14.9
915
56.7
363
0.97
90.
0030
-0.0
350.
0-0
.024
0.00
20lm
0166
k828
0*73
.303
92-6
8.75
893
2.32
533
16.8
816
.77
2229
.786
20.
946
-0.0
050
-0.0
64-0
.001
0-0
.02
0.00
10lm
0563
m21
591*
78.9
1696
-70.
9188
22.
3276
3217
.31
17.1
920
03.5
423
0.97
80.
0070
-0.0
37-0
.003
0-0
.016
-0.0
060
lm03
66l2
1345
86.1
9773
-67.
6337
2.32
8524
16.7
316
.52
1908
.821
60.
985
-0.0
26-0
.02
-0.0
020
-0.0
070
0.0
lm02
00l1
9491
80.4
8924
-67.
9369
2.32
9272
15.9
315
.86
1993
.574
70.
938
-0.0
29-0
.058
-0.0
020
-0.0
040
0.00
90lm
0592
n116
46*
84.1
8167
-71.
1173
12.
3295
3417
.04
16.9
717
75.7
456
0.97
30.
0010
-0.0
30.
0040
-0.0
1-0
.002
0lm
0096
n211
4778
.540
99-7
0.38
856
2.33
2835
17.1
516
.98
1914
.627
10.
922
-0.0
030
-0.1
19-0
.0-0
.078
0.00
70lm
0186
n147
9077
.106
58-6
8.95
847
2.33
3025
17.1
117
.16
538.
5531
0.94
7-0
.037
-0.0
58-0
.01
-0.0
190.
0010
lm00
30m
4163
84.3
7804
-69.
0881
72.
3334
1615
.30
15.3
138
8.84
960.
899
0.00
20-0
.118
-0.0
010
-0.0
270.
0060
lm01
21l1
2322
73.1
6189
-69.
3917
2.33
4903
16.8
216
.64
1482
.576
00.
971
-0.0
090
-0.0
42-0
.009
0-0
.017
-0.0
010
lm00
20k2
403*
82.1
265
-69.
0729
22.
3358
7217
.85
17.7
053
7.50
880.
874
-0.0
060
-0.1
770.
0030
-0.1
080.
01lm
0033
n254
4885
.459
3-6
9.70
678
2.34
0327
16.2
615
.99
1771
.898
10.
987
0.0
-0.0
6-0
.001
0-0
.044
-0.0
010
lm01
15k2
8730
*75
.132
18-6
9.91
555
2.34
1022
16.8
016
.76
1246
.595
20.
991
-0.0
050
-0.0
35-0
.001
0-0
.025
0.00
30lm
0211
k930
8*83
.447
62-6
7.70
132
2.34
1696
17.2
217
.12
1289
.575
10.
956
-0.0
11-0
.039
-0.0
030
-0.0
130.
0020
lm01
86k5
622
76.9
543
-68.
7438
62.
3418
9816
.62
16.3
521
73.6
941
0.96
8-0
.001
0-0
.042
-0.0
050
-0.0
22-0
.002
0lm
0033
l897
884
.972
57-6
9.60
731
2.34
4895
15.7
515
.85
2047
.488
20.
996
-0.0
090
-0.0
1-0
.002
0-0
.003
0-0
.0lm
0103
k404
377
.115
7-6
9.42
463
2.34
5441
15.8
915
.84
1224
.613
00.
974
-0.0
16-0
.038
-0.0
12-0
.019
0.00
70lm
0426
m23
482
75.0
7795
-66.
0628
42.
3455
7315
.15
14.8
314
47.7
508
0.95
-0.0
15-0
.042
-0.0
020
0.00
300.
0010
lm01
21l2
7892
73.2
1002
-69.
3667
82.
3460
417
.10
16.9
717
55.8
861
0.92
5-0
.004
0-0
.12
0.00
10-0
.07
-0.0
040
lm01
12l2
9182
74.1
3397
-69.
7355
82.
3473
8515
.57
15.3
825
74.6
019
0.95
20.
0040
-0.0
67-0
.0-0
.02
0.0
lm01
11n1
6405
75.4
7253
-69.
2932
42.
3479
7416
.90
16.7
715
39.6
904
0.96
6-0
.018
-0.0
26-0
.002
00.
0010
0.00
10lm
0364
n590
186
.491
51-6
7.14
732
2.34
7977
16.5
616
.51
374.
8669
0.91
3-0
.004
0-0
.101
0.00
20-0
.027
0.00
10lm
0437
n826
7*77
.381
03-6
6.11
499
2.35
3292
17.4
917
.33
2082
.923
60.
937
-0.0
030
-0.0
68-0
.002
0-0
.027
0.0
lm02
87n1
4280
*73
.571
27-6
7.55
517
2.35
3686
17.4
017
.15
1550
.625
20.
977
-0.0
030
-0.0
65-0
.003
0-0
.046
-0.0
010
lm02
23n3
0265
85.8
7513
-68.
3303
32.
3555
3115
.64
15.4
014
77.7
595
0.89
4-0
.035
-0.1
51-0
.018
-0.0
670.
0lm
0091
n165
2079
.310
01-6
9.29
892
2.36
1363
16.1
115
.91
1894
.611
10.
943
-0.0
3-0
.065
-0.0
050
-0.0
130.
0080
lm00
31m
1930
585
.283
77-6
9.17
464
2.36
1448
16.8
116
.83
1079
.823
80.
882
-0.0
67-0
.16
-0.0
33-0
.077
-0.0
lm02
94n9
088
74.4
3098
-67.
1626
82.
3656
8216
.87
16.7
512
73.4
985
0.88
-0.0
71-0
.161
-0.0
36-0
.079
0.00
20lm
0033
m29
238*
85.5
3677
-69.
5749
22.
3694
4217
.11
17.0
312
55.6
286
0.98
1-0
.004
0-0
.02
0.00
10-0
.015
-0.0
030
lm03
55n1
9896
*85
.675
14-6
7.23
285
2.37
175
17.3
917
.38
2239
.817
70.
980.
0-0
.024
0.0
-0.0
190.
0020
lm03
63m
3939
*87
.713
31-6
6.62
361
2.37
3044
17.9
717
.80
2317
.706
70.
969
-0.0
020
-0.0
4-0
.003
0-0
.025
-0.0
030
lm03
14n1
0346
77.7
4369
-67.
175
2.37
5213
15.3
515
.12
948.
4991
0.99
3-0
.004
0-0
.014
-0.0
040
-0.0
10.
0lm
0205
l592
881
.647
04-6
8.53
675
2.37
907
17.0
017
.00
1823
.808
60.
97-0
.014
-0.0
24-0
.001
00.
0-0
.001
0lm
0012
l245
72*
79.9
3726
-69.
7058
72.
3808
17.7
017
.55
2184
.752
10.
941
-0.0
080
-0.0
89-0
.005
0-0
.047
0.00
50lm
0120
l127
7272
.010
1-6
9.28
588
2.38
1339
16.7
516
.58
2186
.650
90.
983
-0.0
1-0
.022
-0.0
060
-0.0
12-0
.001
0lm
0367
m17
417*
87.3
9254
-67.
4282
72.
3814
6216
.60
16.4
615
81.7
108
0.97
70.
0060
-0.0
410.
0060
-0.0
390.
0010
lm05
41m
1720
174
.391
01-7
0.55
125
2.38
1813
16.3
416
.07
1924
.601
80.
92-0
.05
-0.1
15-0
.017
-0.0
440.
0010
lm04
27m
1691
576
.034
4-6
6.02
195
2.38
2868
17.3
717
.06
2191
.663
10.
97-0
.009
0-0
.049
-0.0
16-0
.026
0.00
70lm
0355
m83
9985
.750
41-6
7.00
582.
3843
416
.70
16.5
412
71.6
074
0.99
7-0
.01
-0.0
060
0.00
10-0
.001
0-0
.0lm
0035
n291
7485
.257
3-7
0.08
448
2.38
5178
15.8
415
.75
2225
.702
20.
944
-0.0
020
-0.1
14-0
.001
0-0
.078
-0.0
010
lm02
90m
1699
374
.308
85-6
6.42
699
2.38
6669
15.9
615
.78
2161
.732
30.
993
-0.0
090
-0.0
12-0
.003
0-0
.008
0-0
.001
0
176
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0346
n107
3583
.110
24-6
7.53
125
2.38
7713
15.2
815
.06
1953
.749
20.
873
-0.0
36-0
.153
-0.0
19-0
.058
0.00
50lm
0354
l926
384
.533
28-6
7.16
815
2.38
8225
16.9
116
.78
1192
.738
60.
971
-0.0
27-0
.034
0.00
100.
0030
0.00
20lm
0557
l109
4576
.163
66-7
1.73
352.
3888
6617
.07
16.8
315
47.5
995
0.97
20.
0010
-0.0
64-0
.005
0-0
.045
0.00
70lm
0590
m35
0183
.994
41-7
0.50
731
2.38
9369
16.3
316
.09
2322
.675
40.
961
-0.0
19-0
.035
0.0
-0.0
020
-0.0
lm01
87l1
7648
78.0
774
-68.
9755
42.
3905
3217
.15
17.0
817
74.8
356
0.95
60.
0020
-0.0
68-0
.002
0-0
.045
-0.0
lm01
65l9
604
74.0
7694
-68.
5603
82.
3905
9917
.02
16.9
614
97.5
988
0.99
-0.0
2-0
.013
-0.0
020
-0.0
010
-0.0
030
lm02
97k1
6068
74.9
4967
-67.
4086
42.
3942
6715
.34
15.0
819
27.6
449
0.98
3-0
.006
0-0
.014
-0.0
010
0.00
100.
0010
lm00
15m
1296
4*81
.585
82-6
9.82
269
2.39
4782
17.3
817
.14
1198
.659
80.
964
-0.0
080
-0.0
490.
0040
-0.0
330.
0030
lm05
56k7
966
75.0
2718
-71.
5434
82.
3982
0816
.40
16.2
749
0.63
970.
984
-0.0
15-0
.011
-0.0
020
0.00
300.
0010
lm02
30l1
5982
86.0
8001
-67.
9137
22.
3983
5116
.89
16.7
413
16.5
454
0.97
0.00
30-0
.035
-0.0
050
-0.0
15-0
.003
0lm
0305
n139
6976
.924
68-6
7.22
035
2.39
9246
15.9
615
.75
2183
.700
20.
982
-0.0
090
-0.0
17-0
.001
0-0
.001
00.
0010
lm00
93m
6482
79.3
1403
-69.
4374
62.
4000
6817
.32
17.1
815
11.6
682
0.96
50.
0010
-0.0
58-0
.006
0-0
.039
0.00
40lm
0030
k742
184
.084
8-6
9.10
452.
4038
4216
.77
16.6
541
4.71
420.
963
-0.0
22-0
.05
-0.0
31-0
.02
-0.0
1lm
0344
n906
983
.375
07-6
7.16
455
2.40
841
17.0
516
.89
1500
.708
30.
917
0.00
30-0
.127
-0.0
070
-0.0
83-0
.002
0lm
0323
n207
98*
80.6
6736
-66.
8736
12.
4086
7217
.43
17.2
416
19.5
834
0.95
60.
0010
-0.0
76-0
.002
0-0
.06
0.00
60lm
0033
m27
772
85.3
8415
-69.
5671
32.
4112
1616
.64
16.5
522
39.6
372
0.98
7-0
.008
0-0
.017
-0.0
030
-0.0
110.
0010
lm02
90n7
998
74.3
7665
-66.
4562
22.
4130
3115
.78
15.9
079
2.78
800.
95-0
.02
-0.0
74-0
.014
-0.0
570.
0lm
0037
l456
384
.780
55-7
0.29
163
2.41
3848
17.2
917
.29
1186
.720
80.
972
-0.0
010
-0.0
5-0
.001
0-0
.032
0.00
10lm
0294
k281
42*
73.9
7016
-67.
1308
12.
4182
0216
.92
16.8
112
37.6
064
0.92
20.
0050
-0.1
290.
0030
-0.0
920.
0030
lm03
46k1
7136
82.6
852
-67.
4266
12.
4188
2415
.49
15.2
880
9.69
450.
931
0.00
10-0
.102
-0.0
020
-0.0
57-0
.001
0lm
0030
l158
1084
.018
83-6
9.31
956
2.41
9399
15.9
715
.99
1510
.698
60.
958
-0.0
12-0
.055
-0.0
080
-0.0
290.
0010
lm00
56l2
5826
87.9
5228
-70.
4338
32.
4199
8617
.17
16.9
419
17.8
619
0.90
80.
0010
-0.1
42-0
.006
0-0
.089
-0.0
040
lm01
57n1
5497
*72
.716
25-6
8.96
325
2.42
7398
17.1
717
.13
1792
.747
60.
985
0.00
10-0
.024
0.0
-0.0
150.
0lm
0015
n174
9981
.723
12-6
9.99
707
2.43
1098
16.8
716
.74
1530
.694
10.
931
-0.0
020
-0.1
03-0
.002
0-0
.066
-0.0
010
lm03
25m
1962
5*80
.366
54-6
7.07
111
2.43
1928
15.9
415
.71
800.
6959
0.98
9-0
.003
0-0
.02
-0.0
010
-0.0
18-0
.001
0lm
0105
l166
4076
.992
86-7
0.07
014
2.43
3279
17.1
016
.98
1212
.610
00.
986
0.0
-0.0
250.
0010
-0.0
14-0
.003
0lm
0345
m84
9083
.841
36-6
7.00
352
2.43
4907
15.7
015
.41
1815
.812
00.
943
-0.0
050
-0.1
-0.0
050
-0.0
66-0
.001
0lm
0325
n971
880
.643
54-6
7.15
893
2.43
6797
16.7
216
.55
1858
.603
00.
989
-0.0
040
-0.0
19-0
.006
0-0
.011
-0.0
010
lm00
13n2
2558
81.2
643
-69.
6749
82.
4374
4516
.01
16.1
485
7.76
050.
941
-0.0
36-0
.066
-0.0
050
-0.0
060
0.00
30lm
0344
l183
5782
.701
44-6
7.23
384
2.44
2181
16.6
016
.41
1940
.766
20.
98-0
.02
-0.0
35-0
.02
-0.0
26-0
.002
0lm
0550
m23
266
75.5
8039
-70.
6071
2.44
3675
15.4
415
.11
835.
6237
0.94
70.
0060
-0.0
660.
0020
-0.0
20.
0lm
0340
l229
6382
.772
49-6
6.57
868
2.44
7199
15.9
515
.74
1148
.828
60.
931
-0.0
-0.1
02-0
.005
0-0
.061
-0.0
lm03
31n5
533
82.1
1053
-66.
4860
62.
4485
815
.95
15.6
470
1.79
000.
989
-0.0
090
-0.0
090
-0.0
18-0
.007
0-0
.005
0lm
0035
k582
685
.176
19-6
9.79
019
2.45
7281
16.1
516
.08
1483
.702
00.
972
-0.0
17-0
.041
-0.0
16-0
.024
-0.0
030
lm05
51n5
128*
76.7
0335
-70.
7428
12.
4577
1217
.69
17.4
584
2.68
090.
963
-0.0
050
-0.0
59-0
.011
-0.0
220.
0020
lm01
65l1
4067
74.1
9318
-68.
5846
82.
4578
8816
.57
16.4
322
63.6
042
0.94
6-0
.035
-0.0
67-0
.006
0-0
.019
0.00
20lm
0374
n649
988
.475
15-6
7.14
809
2.45
9114
17.1
116
.93
2057
.507
70.
984
-0.0
080
-0.0
28-0
.013
-0.0
210.
0lm
0345
m13
290
84.1
0019
-67.
0321
22.
4605
516
.11
15.7
810
77.8
037
0.96
9-0
.013
-0.0
43-0
.01
-0.0
260.
0lm
0120
l224
3772
.166
19-6
9.35
882.
4651
4816
.56
16.4
321
91.6
165
0.96
3-0
.008
0-0
.04
-0.0
040
-0.0
090
0.00
10lm
0344
k506
882
.745
2-6
6.98
962.
4656
0816
.30
16.1
416
18.6
821
0.98
1-0
.003
0-0
.04
-0.0
14-0
.02
0.00
80lm
0343
l280
1983
.619
52-6
6.93
72.
4675
9616
.55
16.3
712
54.6
180
0.98
6-0
.014
-0.0
24-0
.006
0-0
.017
0.00
40
177
lm02
85l2
5392
*73
.303
53-6
7.27
032.
4683
7416
.33
16.0
615
46.7
474
0.97
8-0
.004
0-0
.022
-0.0
030
-0.0
170.
0020
lm02
13k2
4315
83.4
129
-68.
1394
62.
4694
9616
.87
16.8
118
83.6
801
0.95
0.00
20-0
.082
-0.0
010
-0.0
50.
0040
lm00
93m
4296
79.4
8343
-69.
4247
32.
4699
8116
.33
16.1
357
4.50
170.
888
-0.0
64-0
.153
-0.0
31-0
.075
0.00
10lm
0545
m66
9974
.759
74-7
1.18
265
2.47
1238
16.9
016
.71
1775
.772
00.
904
-0.0
13-0
.125
-0.0
030
-0.0
39-0
.001
0lm
0024
l508
382
.099
3-6
9.94
233
2.47
1267
16.5
316
.44
2225
.801
50.
917
-0.0
63-0
.125
-0.0
22-0
.055
0.00
30lm
0406
l944
*93
.199
33-6
7.49
614
2.47
3836
17.3
517
.26
1641
.582
00.
916
-0.0
050
-0.1
02-0
.007
0-0
.035
0.00
30lm
0095
m32
814
79.4
9724
-69.
9274
32.
4749
3417
.16
17.0
653
2.51
520.
948
-0.0
030
-0.0
83-0
.002
0-0
.033
-0.0
020
lm01
21l2
0722
73.0
5065
-69.
3250
82.
4766
6616
.50
16.4
186
4.68
420.
998
-0.0
23-0
.009
0-0
.005
0-0
.009
00.
0020
lm03
21m
1701
8*80
.381
02-6
6.35
411
2.48
037
16.1
815
.84
1955
.670
20.
929
0.00
10-0
.132
0.00
20-0
.099
-0.0
070
lm03
17k7
278
78.4
5743
-67.
3560
12.
4809
6415
.37
15.1
342
0.77
690.
975
-0.0
060
-0.0
31-0
.004
0-0
.021
0.00
10lm
0344
k246
3682
.919
64-6
7.12
202
2.48
3249
15.5
215
.32
1091
.808
80.
961
-0.0
23-0
.053
-0.0
020
-0.0
040
0.00
20lm
0284
n199
5172
.805
19-6
7.24
532
2.48
3961
16.0
715
.80
1546
.747
40.
961
-0.0
050
-0.0
65-0
.007
0-0
.045
0.00
50lm
0167
l115
90*
74.2
5992
-68.
9369
72.
4847
1216
.77
16.5
843
4.72
450.
967
0.00
20-0
.043
0.00
10-0
.02
0.0
lm01
06k1
4838
76.2
3628
-70.
1988
22.
4853
3315
.62
15.5
522
50.5
739
0.93
5-0
.009
0-0
.119
-0.0
040
-0.0
83-0
.002
0lm
0550
n149
0375
.489
79-7
0.70
212.
4871
3616
.15
15.8
812
43.5
615
0.99
9-0
.047
-0.0
040
-0.0
040
-0.0
090
0.00
30lm
0427
l101
1075
.282
92-6
6.13
402
2.48
9254
16.7
216
.48
1927
.650
60.
944
-0.0
14-0
.073
-0.0
080
-0.0
430.
0lm
0331
k101
9881
.901
25-6
6.31
168
2.49
0214
16.5
116
.33
1455
.773
10.
983
-0.0
21-0
.02
-0.0
010
0.00
100.
0020
lm00
10l1
7439
*79
.983
71-6
9.32
095
2.49
3082
15.7
315
.50
1396
.903
60.
97-0
.006
0-0
.019
-0.0
030
-0.0
040
0.00
30lm
0307
k137
1576
.504
85-6
7.39
192.
4950
7416
.66
16.4
684
5.73
510.
979
-0.0
49-0
.06
-0.0
14-0
.029
-0.0
010
lm05
42l1
7356
72.9
7089
-71.
0678
82.
4955
6416
.59
16.5
418
11.7
353
0.98
7-0
.016
-0.0
120.
0020
-0.0
010
-0.0
lm04
57n6
420
80.8
3767
-66.
0913
52.
4956
5415
.64
15.4
119
51.7
180
0.89
7-0
.046
-0.1
18-0
.016
-0.0
450.
012
lm05
72k3
238*
79.5
0726
-70.
8194
72.
4959
6417
.66
17.5
811
26.6
354
0.94
60.
0070
-0.0
860.
0050
-0.0
41-0
.006
0lm
0040
k115
51*
86.0
9652
-69.
1266
12.
4992
3216
.99
16.7
816
34.5
805
0.97
1-0
.0-0
.031
0.0
-0.0
18-0
.001
0lm
0032
l206
4384
.010
87-6
9.69
192
2.49
9392
15.4
515
.24
1148
.593
00.
984
-0.0
070
-0.0
16-0
.0-0
.008
00.
0020
lm01
21l8
367*
73.1
5498
-69.
2507
42.
5007
7716
.28
16.0
713
06.4
884
0.97
3-0
.034
-0.0
3-0
.02
-0.0
170.
0020
lm00
15m
1964
381
.652
13-6
9.85
72.
5036
216
.82
16.6
638
7.75
720.
981
0.00
30-0
.04
-0.0
050
-0.0
31-0
.0lm
0045
k197
0686
.984
8-6
9.86
957
2.50
5617
15.0
514
.88
1589
.731
70.
988
-0.0
27-0
.024
-0.0
1-0
.017
-0.0
030
lm00
10m
6843
80.3
1027
-69.
0945
12.
5059
7415
.92
15.5
743
8.78
440.
946
0.00
20-0
.095
-0.0
1-0
.061
0.00
80lm
0303
m21
604
76.8
608
-66.
7263
92.
5070
116
.29
16.0
511
91.6
543
0.98
-0.0
35-0
.037
-0.0
010
-0.0
010
0.00
20lm
0346
m16
504
82.9
9672
-67.
4137
92.
5088
4115
.91
15.7
122
34.8
536
0.98
2-0
.001
0-0
.019
-0.0
020
-0.0
120.
0020
lm02
16l2
1415
82.6
6991
-69.
0143
42.
5094
0715
.99
15.8
121
90.7
652
0.98
5-0
.004
0-0
.037
0.00
10-0
.021
0.0
lm00
21l3
2167
82.7
9402
-69.
3864
22.
5122
8816
.64
16.7
474
8.77
380.
96-0
.04
-0.0
67-0
.018
-0.0
3-0
.002
0lm
0540
n138
6973
.497
76-7
0.69
082.
5127
5716
.07
15.8
918
33.6
867
0.93
5-0
.0-0
.084
0.0
-0.0
28-0
.0lm
0256
m23
734*
90.2
1733
-68.
8866
32.
5135
7417
.77
17.5
320
30.5
829
0.96
6-0
.006
0-0
.047
0.00
10-0
.03
0.0
lm05
96l1
9261
83.4
3063
-71.
8128
52.
5153
9217
.38
17.1
716
17.6
885
0.93
9-0
.038
-0.0
49-0
.001
0-0
.006
00.
0040
lm00
20l2
6644
81.8
095
-69.
3834
52.
5168
9916
.72
16.5
620
25.5
258
0.89
7-0
.08
-0.1
44-0
.037
-0.0
70.
0030
lm01
80l6
512
77.0
2743
-67.
8409
52.
5169
0915
.79
15.5
411
72.8
434
0.93
-0.0
35-0
.092
-0.0
15-0
.04
0.00
50lm
0567
k688
178
.047
49-7
1.54
482
2.52
0574
17.2
517
.11
2343
.572
50.
958
-0.0
34-0
.04
0.0
-0.0
030
-0.0
050
lm00
40m
2731
886
.377
98-6
9.22
432.
5221
3315
.72
15.6
019
41.6
268
0.86
8-0
.061
-0.1
82-0
.033
-0.0
880.
0020
lm03
43l2
2832
83.5
9525
-66.
8956
12.
5271
9315
.04
14.8
318
93.7
021
0.91
7-0
.006
0-0
.102
-0.0
030
-0.0
250.
0010
lm01
86n5
534
77.2
4272
-68.
8952
62.
5294
9516
.16
16.0
447
7.73
260.
951
-0.0
49-0
.087
-0.0
25-0
.049
-0.0
090
178
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0206
m28
489
81.0
3877
-68.
8739
62.
5317
9116
.81
16.7
214
35.7
606
0.95
6-0
.009
0-0
.052
-0.0
080
-0.0
360.
0070
lm00
97n1
5434
79.4
1568
-70.
3575
12.
5325
1816
.27
16.0
619
57.6
478
0.90
6-0
.007
0-0
.116
-0.0
040
-0.0
430.
0010
lm00
15m
1357
681
.383
94-6
9.82
752.
5341
1716
.77
16.7
213
67.8
727
0.94
6-0
.036
-0.0
67-0
.019
-0.0
32-0
.003
0lm
0023
k356
482
.852
58-6
9.42
447
2.53
6665
17.1
317
.07
507.
5296
0.97
80.
0070
-0.0
6-0
.001
0-0
.047
-0.0
020
lm01
90m
1123
9*78
.964
18-6
7.71
148
2.53
8094
17.2
717
.10
1766
.913
00.
944
0.00
90-0
.081
-0.0
020
-0.0
65-0
.002
0lm
0294
l112
1674
.077
55-6
7.18
053
2.54
6991
16.6
016
.40
2256
.584
40.
962
-0.0
050
-0.0
54-0
.018
-0.0
25-0
.009
0lm
0010
l421
079
.840
39-6
9.23
612
2.55
1967
17.0
016
.86
588.
5004
0.94
3-0
.072
-0.1
04-0
.035
-0.0
63-0
.007
0lm
0466
n153
4781
.479
-66.
1622
32.
5527
2216
.68
16.6
279
5.76
990.
978
-0.0
19-0
.023
-0.0
020
0.0
-0.0
020
lm02
12n1
8380
82.7
2618
-68.
2714
62.
5538
9317
.21
17.2
315
30.7
138
0.95
50.
01-0
.087
-0.0
030
-0.0
56-0
.012
lm03
47m
1466
084
.048
89-6
7.40
174
2.55
4528
16.3
616
.10
1364
.938
70.
959
-0.0
12-0
.058
-0.0
17-0
.032
-0.0
060
lm00
10k1
7235
80.1
8843
-69.
1671
42.
5561
1116
.21
15.9
419
59.6
465
0.94
3-0
.001
0-0
.057
-0.0
010
-0.0
170.
0010
lm03
33l2
4619
82.0
1793
-66.
9016
12.
5567
0615
.71
15.5
119
77.6
400
0.98
-0.0
12-0
.02
-0.0
040
-0.0
090
0.00
10lm
0105
m14
713*
77.4
7108
-69.
8322
22.
5589
116
.83
16.6
814
96.6
366
0.97
90.
0020
-0.0
29-0
.001
0-0
.011
0.0
lm05
81m
2151
982
.779
34-7
0.57
647
2.55
9421
17.1
016
.95
1901
.844
00.
949
-0.0
63-0
.076
-0.0
28-0
.05
-0.0
050
lm01
55n2
2259
72.6
2359
-68.
6391
42.
5601
0517
.14
17.0
215
23.6
658
0.94
7-0
.051
-0.0
84-0
.02
-0.0
4-0
.002
0lm
0457
k246
6780
.380
14-6
6.07
433
2.56
1858
16.5
116
.27
1786
.763
30.
98-0
.008
0-0
.03
-0.0
050
-0.0
16-0
.001
0lm
0211
l166
6283
.549
77-6
7.90
057
2.56
1989
16.7
616
.59
1089
.684
90.
933
-0.0
-0.1
010.
0-0
.067
-0.0
010
lm01
00m
1626
676
.620
51-6
9.15
496
2.56
5832
16.7
416
.46
2303
.632
30.
937
-0.0
34-0
.074
-0.0
080
-0.0
180.
0010
lm01
70m
4805
75.2
3106
-67.
6807
62.
5662
3216
.19
15.8
633
4.90
630.
909
-0.0
49-0
.108
-0.0
21-0
.045
-0.0
040
lm03
16k1
4599
77.2
4938
-67.
3973
72.
5697
2616
.79
16.6
315
89.6
733
0.88
7-0
.01
-0.1
53-0
.012
-0.0
760.
0010
lm03
07m
1549
177
.249
16-6
7.39
742
2.56
975
16.7
816
.58
1463
.695
30.
916
0.00
20-0
.151
-0.0
010
-0.0
8-0
.007
0lm
0292
n237
0874
.270
14-6
6.94
127
2.56
9894
16.0
815
.84
2389
.511
40.
954
-0.0
060
-0.0
84-0
.002
0-0
.058
0.0
lm05
86l1
3797
81.4
6549
-71.
7383
72.
5741
0816
.37
16.1
816
03.6
181
0.91
1-0
.057
-0.1
25-0
.025
-0.0
56-0
.003
0lm
0112
l185
7574
.151
31-6
9.66
844
2.57
4239
16.5
616
.36
1711
.909
40.
963
-0.0
15-0
.026
-0.0
020
0.00
20-0
.0lm
0177
k176
6775
.825
58-6
8.81
452
2.57
7507
16.5
116
.28
1096
.671
10.
915
-0.0
13-0
.129
-0.0
-0.0
740.
0050
lm00
20k2
4655
82.1
3845
-69.
2302
62.
5793
3415
.95
15.7
312
66.6
051
0.95
70.
0050
-0.0
840.
0010
-0.0
610.
0lm
0602
l611
885
.658
51-7
0.99
859
2.58
0945
15.6
115
.68
390.
7804
0.97
2-0
.01
-0.0
35-0
.001
0-0
.015
0.0
lm02
11m
5293
83.8
299
-67.
6695
52.
5861
315
.95
15.7
018
33.8
282
0.98
2-0
.013
-0.0
63-0
.004
0-0
.048
0.00
10lm
0054
m17
797
88.2
2564
-69.
8642
82.
5867
4516
.09
15.9
815
38.7
375
0.95
1-0
.014
-0.0
49-0
.004
0-0
.01
0.00
10lm
0343
l256
1383
.616
61-6
6.91
348
2.58
9002
15.6
815
.49
2579
.716
30.
964
-0.0
080
-0.0
59-0
.006
0-0
.04
-0.0
040
lm03
41n5
260
83.8
6604
-66.
4727
22.
5895
514
.90
14.6
140
5.85
220.
974
-0.0
15-0
.024
0.00
30-0
.00.
0030
lm03
55n2
6448
85.9
0168
-67.
2726
52.
5928
3815
.07
14.7
611
20.7
651
0.93
90.
0040
-0.0
890.
0030
-0.0
480.
0lm
0331
k181
3481
.882
85-6
6.36
722
2.59
5648
16.6
916
.50
1620
.613
70.
991
-0.0
070
-0.0
2-0
.004
0-0
.014
-0.0
lm00
41k2
1578
87.0
6688
-69.
1802
2.59
5659
17.0
316
.89
812.
7853
0.96
5-0
.046
-0.0
44-0
.004
0-0
.009
0-0
.002
0lm
0012
m28
1480
.395
38-6
9.42
642.
5989
16.8
416
.59
1804
.821
90.
980.
0030
-0.0
480.
0030
-0.0
35-0
.001
0lm
0366
n144
2886
.802
8-6
7.55
567
2.60
1096
17.1
617
.02
1899
.817
20.
962
-0.0
28-0
.03
0.00
100.
0010
0.00
20lm
0427
m16
528
75.7
7647
-66.
0217
82.
6082
2616
.28
15.9
951
7.59
340.
967
-0.0
12-0
.056
-0.0
080
-0.0
370.
0020
lm03
40n5
836
83.1
235
-66.
4399
92.
6144
5915
.75
15.4
714
63.7
628
0.93
5-0
.008
0-0
.105
-0.0
080
-0.0
7-0
.001
0lm
0040
k234
7685
.916
-69.
2081
22.
6154
1815
.90
15.7
019
01.7
951
0.97
5-0
.019
-0.0
53-0
.016
-0.0
320.
0050
lm01
16l1
9585
*74
.018
44-7
0.38
601
2.61
797
16.7
216
.52
1447
.746
80.
975
-0.0
010
-0.0
43-0
.005
0-0
.039
0.00
80lm
0212
m20
099*
82.8
7114
-68.
1566
12.
6211
2816
.92
16.8
623
43.5
959
0.96
8-0
.006
0-0
.039
-0.0
010
-0.0
21-0
.001
0
179
lm03
03n1
6128
76.8
2415
-66.
8436
42.
6211
9617
.01
16.8
625
35.7
713
0.94
7-0
.014
-0.0
91-0
.011
-0.0
68-0
.009
0lm
0551
m73
4376
.668
48-7
0.49
136
2.62
2983
17.3
317
.03
1126
.615
20.
912
-0.0
72-0
.116
-0.0
27-0
.049
-0.0
010
lm03
77l5
586
89.1
5001
-67.
6027
32.
6288
9416
.59
16.3
118
61.7
884
0.93
-0.0
47-0
.105
-0.0
15-0
.042
-0.0
010
lm00
20l9
813
81.9
2152
-69.
2723
32.
6313
5215
.84
15.5
843
4.67
090.
942
-0.0
090
-0.0
87-0
.005
0-0
.061
-0.0
020
lm03
45k1
3606
83.5
5195
-67.
0449
22.
6315
3414
.90
14.7
139
5.68
780.
929
-0.0
27-0
.109
-0.0
11-0
.057
-0.0
lm03
16l1
7312
77.6
4399
-67.
5734
32.
6316
3116
.53
16.3
419
06.8
206
0.98
2-0
.004
0-0
.026
-0.0
020
-0.0
17-0
.001
0lm
0183
l171
8577
.700
33-6
8.24
991
2.63
4221
17.1
017
.01
2517
.798
80.
981
-0.0
15-0
.026
-0.0
060
-0.0
150.
0010
lm00
90n2
9324
78.3
4942
-69.
3802
2.63
6584
15.9
615
.97
2009
.521
50.
952
0.0
-0.1
19-0
.01
-0.0
780.
011
lm05
43n1
8447
*74
.712
33-7
1.05
282.
6377
616
.73
16.5
121
98.7
862
0.96
-0.0
030
-0.0
68-0
.001
0-0
.054
0.00
10lm
0220
n197
91*
84.8
0013
-67.
9317
22.
6411
8816
.70
16.5
123
05.7
351
0.97
2-0
.005
0-0
.038
-0.0
060
-0.0
280.
0010
lm03
35n2
4071
82.4
5012
-67.
2493
22.
6414
0316
.14
15.9
114
63.7
486
0.99
-0.0
090
-0.0
170.
0020
-0.0
-0.0
030
lm02
94l2
1960
73.9
8799
-67.
2495
82.
6414
2715
.39
15.1
715
75.6
394
0.96
3-0
.019
-0.0
31-0
.001
0-0
.002
00.
0040
lm02
00l6
405
80.5
8213
-67.
8414
62.
6490
4215
.77
15.5
823
29.6
599
0.98
7-0
.009
0-0
.022
-0.0
050
-0.0
140.
0010
lm01
30m
1478
0*70
.566
84-6
9.14
122.
6506
7417
.75
17.5
618
38.6
513
0.94
50.
0050
-0.0
6-0
.005
0-0
.041
0.00
50lm
0465
l267
3682
.048
34-6
5.88
179
2.65
4428
15.8
615
.63
1761
.832
30.
92-0
.034
-0.0
9-0
.01
-0.0
250.
0080
lm01
84k1
7447
76.9
537
-68.
4594
42.
6561
7316
.54
16.4
113
74.9
038
0.88
5-0
.088
-0.1
79-0
.043
-0.0
950.
0010
lm02
16l1
7243
82.5
3308
-68.
9827
82.
6573
9215
.88
15.7
414
24.8
947
0.92
4-0
.045
-0.1
06-0
.018
-0.0
360.
0010
lm00
13l2
1404
81.1
5178
-69.
6697
52.
6580
9716
.67
16.5
818
66.6
505
0.99
2-0
.019
-0.0
18-0
.0-0
.003
00.
0lm
0037
n105
99*
85.5
9315
-70.
3281
82.
6586
9816
.45
16.3
323
23.6
869
0.98
5-0
.003
0-0
.032
-0.0
020
-0.0
14-0
.0lm
0124
m15
092
72.4
8036
-69.
8495
72.
6591
2916
.47
16.3
822
31.5
516
0.96
8-0
.03
-0.0
36-0
.0-0
.0-0
.001
0lm
0173
m21
250*
76.5
2163
-68.
1156
32.
6613
3416
.02
15.7
111
39.7
472
0.97
6-0
.014
-0.0
49-0
.009
0-0
.039
0.0
lm02
30l9
562
86.3
1025
-67.
8684
52.
6626
5817
.05
16.8
917
75.9
264
0.89
6-0
.046
-0.1
38-0
.022
-0.0
590.
0020
lm01
73n1
3333
76.4
494
-68.
2276
2.66
5684
17.2
917
.14
1468
.607
81.
003
-0.0
14-0
.023
-0.0
050
-0.0
20.
0020
lm01
15k4
086
74.9
1607
-69.
7776
32.
6661
7715
.36
15.2
422
80.5
789
0.98
3-0
.025
-0.0
28-0
.002
00.
0-0
.004
0lm
0195
m16
673*
80.2
7267
-68.
4434
42.
6664
7616
.11
15.9
111
36.8
411
0.96
3-0
.004
0-0
.047
-0.0
040
-0.0
190.
0020
lm01
55m
2848
372
.700
91-6
8.52
691
2.66
7227
16.8
416
.58
1833
.661
00.
976
0.00
60-0
.044
-0.0
020
-0.0
29-0
.002
0lm
0344
m24
630
83.2
5301
-67.
1157
22.
6678
9615
.46
15.2
312
56.5
883
0.98
5-0
.006
0-0
.028
-0.0
050
-0.0
20.
0lm
0127
l964
273
.143
06-7
0.31
871
2.66
9394
16.8
816
.63
2471
.865
20.
975
-0.0
38-0
.035
-0.0
18-0
.033
0.00
10lm
0285
m10
287
73.3
7918
-67.
0160
82.
6697
2515
.30
15.1
221
99.7
855
0.96
-0.0
040
-0.0
39-0
.006
0-0
.015
0.00
40lm
0045
k104
45*
87.1
6535
-69.
8126
2.66
9896
15.7
815
.66
2269
.745
60.
950.
0-0
.086
0.00
10-0
.063
0.0
lm00
11m
2271
381
.372
01-6
9.18
227
2.67
4348
16.1
315
.86
1711
.936
20.
980.
0030
-0.0
34-0
.003
0-0
.019
0.00
10lm
0125
m55
8973
.748
55-6
9.77
929
2.67
6261
15.0
414
.77
1076
.695
00.
957
-0.0
010
-0.0
69-0
.002
0-0
.036
-0.0
010
lm01
74l1
2903
*74
.826
39-6
8.60
046
2.67
6506
17.5
317
.43
1848
.631
80.
920.
0010
-0.0
45-0
.002
0-0
.015
0.00
40lm
0330
n193
00*
81.3
2542
-66.
5302
32.
6772
6217
.72
17.7
619
68.6
406
0.97
60.
0030
-0.0
48-0
.005
0-0
.035
0.00
20lm
0685
n231
9177
.555
07-7
2.85
828
2.67
8273
17.2
517
.13
2214
.778
90.
926
-0.0
-0.1
2-0
.001
0-0
.068
-0.0
020
lm01
86n8
773
77.3
7151
-68.
9172
42.
6788
3215
.08
14.8
149
6.67
190.
947
-0.0
25-0
.076
-0.0
15-0
.051
0.00
60lm
0022
k389
0*82
.138
9-6
9.43
238
2.68
0612
16.5
716
.48
1941
.620
20.
98-0
.0-0
.036
-0.0
010
-0.0
230.
0020
lm00
92m
3797
*78
.430
77-6
9.43
449
2.68
3288
17.3
617
.31
1096
.687
70.
97-0
.004
0-0
.062
-0.0
010
-0.0
39-0
.004
0lm
0093
m11
981
79.4
2347
-69.
4660
62.
6873
716
.31
16.1
717
71.8
776
0.93
2-0
.046
-0.0
82-0
.019
-0.0
420.
0040
lm05
71n2
6162
80.6
4243
-70.
752.
6874
316
.07
15.8
435
1.81
870.
972
-0.0
080
-0.0
4-0
.006
0-0
.023
-0.0
lm01
77l2
1797
75.9
4157
-69.
0056
12.
6874
8916
.96
16.7
323
07.6
238
0.98
3-0
.025
-0.0
380.
0020
-0.0
010
-0.0
030
180
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0530
m21
215
71.5
4592
-70.
5860
82.
6876
3816
.26
16.0
223
05.6
051
0.95
4-0
.026
-0.0
71-0
.007
0-0
.015
-0.0
010
lm01
65k2
8784
73.9
2743
-68.
5188
52.
6917
5416
.85
16.8
311
07.8
097
0.88
7-0
.05
-0.1
6-0
.036
-0.0
820.
014
lm05
64k4
754
77.1
4207
-71.
1755
42.
6928
8816
.11
15.9
510
70.8
255
0.98
3-0
.004
0-0
.023
-0.0
040
-0.0
140.
0010
lm02
41k1
3248
*88
.963
94-6
7.74
821
2.69
5078
16.9
316
.73
2143
.826
10.
945
-0.0
010
-0.0
67-0
.002
0-0
.022
0.00
30lm
0165
k136
1274
.304
69-6
8.43
168
2.69
6423
15.1
414
.93
1928
.575
70.
967
-0.0
060
-0.0
5-0
.003
0-0
.034
-0.0
030
lm02
13k2
3159
*83
.448
48-6
8.13
261
2.70
0634
16.9
416
.82
1906
.844
80.
984
-0.0
030
-0.0
34-0
.006
0-0
.013
-0.0
060
lm02
15m
2414
83.6
6528
-68.
3654
62.
7016
1216
.01
15.7
914
83.6
936
0.97
1-0
.01
-0.0
11-0
.055
-0.0
170.
023
lm02
91l5
438
74.8
6958
-66.
4304
72.
7036
815
.88
15.7
418
09.7
745
0.90
9-0
.048
-0.1
37-0
.02
-0.0
550.
0020
lm02
13n3
0527
*83
.703
61-6
8.32
958
2.70
3828
17.1
517
.03
858.
6189
0.95
2-0
.003
0-0
.091
-0.0
060
-0.0
850.
0020
lm01
15k1
7125
75.0
8609
-69.
8496
32.
7078
4216
.52
16.4
311
54.8
513
0.89
1-0
.061
-0.1
4-0
.028
-0.0
60.
0060
lm01
64m
2684
473
.458
52-6
8.50
987
2.70
9069
17.2
317
.16
1898
.736
90.
959
-0.0
16-0
.062
-0.0
25-0
.032
0.01
3lm
0015
m15
054
81.7
0531
-69.
8325
52.
7098
7217
.03
16.9
912
24.5
329
0.96
9-0
.002
0-0
.025
-0.0
1-0
.007
00.
0070
lm00
12n1
4828
80.4
5366
-69.
6430
72.
7128
716
.09
15.9
318
78.6
691
0.97
1-0
.026
-0.0
42-0
.01
-0.0
22-0
.002
0lm
0103
k105
8276
.958
48-6
9.46
051
2.71
3007
16.0
916
.03
414.
7172
0.91
4-0
.055
-0.1
11-0
.025
-0.0
470.
0060
lm04
31n1
5433
77.3
05-6
5.17
407
2.71
4038
16.9
316
.76
2096
.874
30.
932
-0.0
53-0
.064
-0.0
11-0
.021
0.00
90lm
0311
n213
5278
.704
5-6
6.54
172.
7150
9716
.44
16.2
614
63.7
082
0.93
2-0
.059
-0.1
04-0
.026
-0.0
530.
0010
lm01
85n2
2544
*78
.190
87-6
8.69
732.
7182
17.3
517
.22
1851
.612
00.
963
-0.0
15-0
.064
-0.0
17-0
.051
-0.0
010
lm03
33m
2212
0*82
.202
73-6
6.73
199
2.72
0332
15.9
215
.66
1184
.674
80.
978
-0.0
070
-0.0
31-0
.002
0-0
.009
00.
0020
lm03
25k2
8914
*80
.037
64-6
7.12
965
2.72
169
16.6
316
.52
1493
.710
20.
932
-0.0
090
-0.0
63-0
.004
0-0
.004
00.
0010
lm01
72n6
253
75.2
7408
-68.
1923
52.
7276
6315
.53
15.2
977
5.85
990.
956
-0.0
16-0
.075
-0.0
050
-0.0
520.
0010
lm02
06k2
5944
80.8
1531
-68.
8697
42.
7314
616
.21
16.0
317
30.9
271
0.98
1-0
.027
-0.0
35-0
.001
0-0
.003
00.
0030
lm02
94l8
864
73.7
6054
-67.
1642
52.
7403
8815
.14
14.7
712
53.5
437
0.94
5-0
.009
0-0
.087
-0.0
060
-0.0
630.
0lm
0091
m28
603*
79.7
0007
-69.
2096
62.
7408
916
.96
16.8
111
93.6
169
0.95
20.
0020
-0.0
53-0
.002
0-0
.029
-0.0
030
lm01
23k1
7044
73.2
29-6
9.49
675
2.74
4816
15.5
215
.42
1581
.589
60.
963
-0.0
19-0
.033
0.00
100.
0020
0.00
30lm
0027
l194
2083
.109
67-7
0.38
774
2.74
5088
16.8
916
.82
1435
.763
80.
931
-0.0
61-0
.085
-0.0
18-0
.038
0.01
3lm
0020
k168
2681
.949
32-6
9.17
409
2.74
7223
15.3
515
.17
569.
5124
0.91
7-0
.043
-0.1
11-0
.022
-0.0
490.
0030
lm02
05m
4021
81.9
9126
-68.
3726
82.
7498
6617
.02
16.8
510
82.8
700
1.00
7-0
.027
-0.0
15-0
.007
0-0
.009
0-0
.003
0lm
0294
n747
974
.528
13-6
7.15
228
2.75
026
16.1
915
.97
2192
.686
50.
962
-0.0
26-0
.036
0.00
200.
00.
0030
lm02
04l1
8900
80.5
3603
-68.
6208
52.
7545
0317
.23
17.0
521
98.6
817
0.91
80.
0070
-0.0
840.
0090
-0.0
55-0
.009
0lm
0231
l120
15*
87.0
4159
-67.
8789
32.
7548
2416
.67
16.4
918
79.6
968
0.99
20.
0050
-0.0
250.
0020
-0.0
21-0
.001
0lm
0036
m17
521
84.4
2606
-70.
2157
52.
7558
5616
.42
16.2
649
1.59
810.
956
-0.0
15-0
.067
-0.0
070
-0.0
410.
0040
lm05
56n1
7386
*75
.721
5-7
1.79
254
2.75
5996
17.8
517
.67
2200
.767
50.
968
-0.0
11-0
.045
-0.0
060
-0.0
330.
0070
lm04
17n1
7063
74.2
1734
-66.
1814
92.
7602
8816
.55
16.3
918
20.6
634
0.96
-0.0
010
-0.0
5-0
.001
0-0
.026
0.00
10lm
0091
n214
5279
.642
53-6
9.39
339
2.76
5244
16.9
516
.84
2161
.754
30.
947
-0.0
77-0
.093
-0.0
28-0
.06
-0.0
040
lm06
11m
4959
89.1
808
-70.
4687
72.
7675
1416
.87
16.6
122
37.6
572
0.93
6-0
.004
0-0
.115
-0.0
020
-0.0
79-0
.002
0lm
0541
k200
99*
73.7
4083
-70.
5796
52.
7681
5617
.12
17.0
222
58.7
505
0.97
2-0
.008
0-0
.05
-0.0
030
-0.0
17-0
.002
0lm
0093
l260
3079
.190
29-6
9.69
22.
7722
5716
.76
16.7
723
49.5
849
0.97
5-0
.03
-0.0
23-0
.002
0-0
.002
0-0
.004
0lm
0025
k174
8982
.895
83-6
9.85
245
2.77
3556
16.9
516
.90
1480
.846
30.
937
-0.0
070
-0.0
94-0
.001
0-0
.046
-0.0
020
lm01
76k2
5619
75.0
7291
-68.
8768
42.
7744
8915
.73
15.5
018
84.6
086
0.92
5-0
.027
-0.0
77-0
.008
0-0
.015
0.01
1lm
0346
n230
0383
.175
1-6
7.62
429
2.77
7051
15.2
914
.97
1258
.592
60.
942
-0.0
010
-0.0
88-0
.005
0-0
.052
-0.0
020
lm01
77n1
0023
76.2
5629
-68.
9224
52.
7777
7516
.35
16.2
036
1.86
580.
962
-0.0
37-0
.053
-0.0
12-0
.022
-0.0
020
181
lm00
33k1
1425
84.8
4785
-69.
4691
52.
7808
3515
.79
15.7
336
5.75
260.
951
-0.0
2-0
.039
0.00
100.
0020
0.00
70lm
0604
l252
6885
.558
37-7
1.47
772
2.78
1504
16.2
916
.13
1819
.813
80.
955
-0.0
16-0
.03
0.00
30-0
.001
0-0
.0lm
0427
k156
8575
.526
56-6
6.07
629
2.79
1595
15.8
315
.53
1946
.681
50.
963
-0.0
22-0
.038
0.0
0.00
100.
0040
lm03
37k1
8241
81.9
6413
-67.
4289
52.
7939
9515
.50
15.3
122
07.6
279
0.98
80.
0040
-0.0
27-0
.001
0-0
.019
-0.0
030
lm05
80m
1660
4*81
.833
25-7
0.55
214
2.79
6134
16.6
816
.51
1894
.742
30.
964
-0.0
020
-0.0
46-0
.001
0-0
.036
0.00
20lm
0156
m24
0171
.936
-68.
7904
62.
7971
7216
.26
16.1
318
30.6
572
0.96
9-0
.02
-0.0
310.
0010
0.0
-0.0
010
lm03
44m
1620
0*83
.147
81-6
7.06
121
2.79
8582
16.2
616
.06
1820
.720
20.
984
-0.0
060
-0.0
3-0
.004
0-0
.023
-0.0
010
lm02
94l8
466
73.9
4168
-67.
1618
12.
8016
5816
.87
16.6
783
5.61
820.
991
-0.0
13-0
.022
-0.0
13-0
.011
0.00
10lm
0343
k468
383
.411
75-6
6.62
775
2.80
5072
15.2
515
.01
2580
.728
40.
91-0
.041
-0.1
3-0
.016
-0.0
610.
0060
lm01
62m
2487
8*73
.484
37-6
8.17
82.
8088
4816
.31
16.2
822
94.6
311
0.94
60.
0010
-0.0
74-0
.003
0-0
.029
0.00
10lm
0466
l164
61*
81.3
4921
-66.
2344
72.
8151
615
.73
15.7
020
21.5
871
0.97
3-0
.004
0-0
.021
-0.0
030
-0.0
030
0.00
10lm
0214
n174
17*
82.9
1098
-68.
6131
42.
8161
0817
.67
17.6
018
39.7
094
0.97
1-0
.011
-0.0
34-0
.004
0-0
.021
-0.0
040
lm03
36k7
065
80.8
5757
-67.
3433
12.
8212
5816
.06
15.9
614
47.8
177
0.95
7-0
.02
-0.0
40.
0010
0.00
100.
0050
lm01
91n4
635
80.2
1988
-67.
8643
52.
8226
1117
.01
16.8
820
31.5
042
0.90
8-0
.08
-0.1
43-0
.033
-0.0
66-0
.004
0lm
0351
n102
67*
85.7
2673
-66.
5861
12.
8255
601
17.1
317
.00
1189
.710
00.
977
-0.0
050
-0.0
23-0
.001
0-0
.004
00.
0010
lm01
06l1
1713
75.9
1194
-70.
3326
22.
8275
0115
.85
15.6
217
55.8
780
0.96
2-0
.011
-0.0
61-0
.008
0-0
.047
-0.0
lm00
14m
9900
*80
.389
68-6
9.81
157
2.83
114
17.6
217
.60
1442
.808
10.
971
-0.0
070
-0.0
45-0
.003
0-0
.041
-0.0
050
lm02
04k9
178*
80.6
2568
-68.
4060
52.
8392
7816
.25
16.2
119
27.7
495
0.96
50.
0-0
.038
-0.0
020
-0.0
070
0.00
10lm
0032
k156
6084
.044
61-6
9.53
401
2.84
1496
14.7
214
.52
1449
.782
20.
965
-0.0
050
-0.0
59-0
.004
0-0
.038
-0.0
1lm
0195
n547
279
.951
77-6
8.53
449
2.84
1972
16.8
716
.85
759.
8540
0.89
2-0
.083
-0.1
49-0
.039
-0.0
84-0
.005
0lm
0581
l290
1082
.620
01-7
0.76
699
2.84
3662
16.7
316
.71
2008
.560
10.
943
-0.0
5-0
.081
-0.0
2-0
.032
0.00
50lm
0020
n128
40*
82.3
8831
-69.
2866
72.
8512
7616
.98
16.7
323
45.5
803
0.95
4-0
.009
0-0
.053
-0.0
070
-0.0
140.
0030
lm00
34k1
2920
*84
.066
26-6
9.83
668
2.85
2214
116
.30
16.1
719
97.5
843
0.92
8-0
.005
0-0
.095
0.00
30-0
.035
0.00
20lm
0021
k137
7082
.917
11-6
9.13
302
2.85
3292
15.3
315
.09
797.
5801
0.88
-0.0
68-0
.171
-0.0
31-0
.086
0.00
10lm
0541
m10
971
74.4
8554
-70.
5098
22.
8619
3416
.96
16.7
721
88.6
643
0.95
2-0
.052
-0.0
68-0
.013
-0.0
290.
0010
lm00
31k1
9705
85.2
061
-69.
2183
62.
8675
3614
.91
14.9
719
77.6
787
0.91
6-0
.02
-0.0
86-0
.006
0-0
.024
0.00
30lm
0011
n104
45*
81.2
678
-69.
2638
2.86
7908
16.1
616
.07
727.
8740
0.97
-0.0
040
-0.0
36-0
.004
0-0
.013
0.0
lm04
24n2
3353
75.0
9632
-65.
8668
92.
8693
1215
.03
14.6
833
2.84
290.
948
-0.0
070
-0.0
85-0
.005
0-0
.051
0.00
20lm
0314
m22
740
77.7
2598
-67.
0924
2.87
1881
16.7
716
.81
1128
.683
80.
89-0
.076
-0.1
49-0
.038
-0.0
660.
0040
lm01
65k1
9767
*74
.304
45-6
8.46
583
2.87
351
16.9
916
.92
1407
.911
70.
97-0
.016
-0.0
51-0
.011
-0.0
47-0
.001
0lm
0321
k150
88*
80.2
1354
-66.
4235
32.
8764
5617
.00
16.8
311
22.6
202
0.99
5-0
.003
0-0
.016
-0.0
010
-0.0
060
0.00
10lm
0013
k297
8881
.088
15-6
9.56
005
2.88
2388
15.9
315
.95
2329
.656
70.
974
-0.0
29-0
.028
0.00
30-0
.002
00.
0010
lm00
31l2
1280
85.0
1322
-69.
3319
22.
8824
8916
.08
15.9
922
57.6
709
0.97
9-0
.002
0-0
.023
-0.0
11-0
.011
0.00
50lm
0285
m24
289
73.5
7847
-67.
1068
32.
8833
6116
.38
16.1
518
38.6
761
0.97
7-0
.002
0-0
.032
-0.0
040
-0.0
170.
0lm
0417
m19
623
74.2
255
-66.
0741
62.
8855
215
.85
15.5
718
86.5
721
0.95
7-0
.029
-0.0
47-0
.005
0-0
.008
00.
0040
lm01
05k3
1240
77.0
4771
-69.
9283
82.
8878
5417
.14
17.0
615
03.6
434
0.93
9-0
.042
-0.0
620.
0010
-0.0
040
0.00
90lm
0541
l179
0673
.856
15-7
0.78
171
2.89
5575
16.8
116
.74
1835
.688
30.
921
-0.0
69-0
.129
-0.0
31-0
.07
-0.0
010
lm03
31m
1772
382
.189
19-6
6.36
106
2.89
6212
16.9
216
.65
792.
7472
0.97
6-0
.004
0-0
.03
-0.0
070
-0.0
18-0
.001
0lm
0110
l205
2574
.090
64-6
9.34
248
2.89
896
16.4
616
.28
1881
.608
60.
950.
0060
-0.0
94-0
.002
0-0
.065
0.00
90lm
0103
k151
9877
.065
-69.
4846
2.89
9283
15.8
015
.96
2270
.737
10.
973
-0.0
-0.0
4-0
.0-0
.034
0.00
10lm
0364
k699
786
.162
38-6
7.00
003
2.90
0784
17.0
216
.87
456.
7497
0.95
80.
0010
-0.0
590.
0020
-0.0
290.
0010
182
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0166
l185
1173
.077
86-6
8.98
609
2.90
2615
.65
15.4
242
6.73
820.
962
-0.0
24-0
.036
0.00
300.
00.
0040
lm01
20n2
4579
*72
.503
89-6
9.35
576
2.90
7138
15.8
715
.82
1083
.817
50.
976
-0.0
070
-0.0
29-0
.004
0-0
.005
0-0
.0lm
0345
k233
1083
.835
1-6
7.10
524
2.90
8255
15.8
915
.65
1994
.588
80.
966
-0.0
030
-0.0
46-0
.027
-0.0
080
0.01
5lm
0327
m59
2780
.558
27-6
7.33
953
2.91
1755
15.8
815
.61
1290
.519
60.
918
-0.0
030
-0.1
38-0
.002
0-0
.081
-0.0
010
lm02
85n6
767
73.5
462
-67.
1495
42.
9117
617
.23
17.0
019
22.6
488
0.97
8-0
.011
-0.0
45-0
.006
0-0
.038
0.00
20lm
0701
l689
2*81
.739
71-7
2.03
963
2.91
2402
17.0
216
.89
1528
.672
00.
968
-0.0
040
-0.0
38-0
.004
0-0
.008
00.
0010
lm02
16n1
5995
83.1
3799
-68.
9625
62.
9135
1414
.86
14.7
420
56.4
677
0.87
5-0
.056
-0.1
76-0
.024
-0.0
750.
0lm
0614
l199
70*
87.5
7282
-71.
4431
92.
9165
2217
.16
17.3
422
04.8
174
0.95
8-0
.002
0-0
.046
0.00
20-0
.027
-0.0
030
lm03
23n7
828
80.3
9908
-66.
7974
22.
9168
0116
.43
16.2
440
5.80
070.
945
-0.0
030
-0.0
84-0
.001
0-0
.042
-0.0
020
lm00
24m
7552
82.6
9505
-69.
8000
12.
9172
0816
.12
16.0
014
80.8
463
0.88
7-0
.084
-0.1
59-0
.039
-0.0
790.
012
lm01
20m
1197
372
.670
68-6
9.12
053
2.91
7753
15.9
215
.72
1766
.881
50.
919
-0.0
46-0
.104
-0.0
14-0
.042
0.01
lm00
25k3
1765
82.9
931
-69.
9255
82.
9180
3916
.62
16.5
614
80.8
463
0.94
90.
0020
-0.0
8-0
.009
0-0
.05
-0.0
080
lm03
00k8
884
75.7
5457
-66.
3069
62.
9218
3416
.91
16.6
414
63.6
953
0.96
9-0
.009
0-0
.054
-0.0
020
-0.0
420.
0050
lm02
94m
2862
374
.274
29-6
7.12
564
2.92
2208
16.1
215
.98
1472
.638
60.
978
-0.0
010
-0.0
440.
0040
-0.0
280.
0lm
0426
n179
4975
.105
64-6
6.17
679
2.92
4628
16.4
716
.18
2187
.695
80.
982
-0.0
1-0
.024
-0.0
060
-0.0
120.
0020
lm02
96m
2340
674
.180
81-6
7.45
372.
9249
4216
.77
16.5
984
5.72
830.
979
-0.0
11-0
.032
-0.0
080
-0.0
230.
0010
lm03
03m
5318
76.9
2088
-66.
6270
42.
9260
8217
.10
16.9
381
9.79
950.
957
-0.0
030
-0.0
730.
0-0
.045
-0.0
010
lm00
21k2
4967
83.2
0222
-69.
2013
22.
9261
15.4
315
.19
1259
.600
70.
945
0.00
60-0
.082
0.00
10-0
.051
-0.0
010
lm01
10l2
1211
*73
.918
3-6
9.34
737
2.92
6536
16.8
916
.70
1771
.864
90.
961
-0.0
080
-0.0
69-0
.011
-0.0
540.
0010
lm03
35l8
729
81.8
3248
-67.
1595
82.
9316
1816
.39
16.2
780
9.68
470.
909
-0.0
11-0
.123
-0.0
050
-0.0
420.
0lm
0560
m74
9377
.458
08-7
0.49
391
2.93
4794
16.1
116
.17
1140
.597
50.
954
-0.0
43-0
.061
-0.0
12-0
.032
0.00
40lm
0312
n157
41*
77.9
4811
-66.
8564
2.93
5118
16.8
616
.55
2131
.805
70.
979
-0.0
080
-0.0
28-0
.004
0-0
.015
-0.0
020
lm01
12n2
1013
74.4
5324
-69.
6794
72.
9385
6115
.11
14.9
323
15.6
271
0.97
6-0
.013
-0.0
29-0
.002
0-0
.007
00.
0020
lm03
40k2
2602
*82
.881
6-6
6.42
372
2.94
0286
17.7
217
.52
1941
.775
00.
968
0.00
10-0
.057
-0.0
010
-0.0
170.
0010
lm00
41n7
760*
87.2
648
-69.
2617
32.
9454
0217
.39
17.3
612
72.6
320
0.96
9-0
.01
-0.0
39-0
.004
0-0
.011
0.00
10lm
0326
l110
0379
.359
85-6
7.52
361
2.94
932
17.2
217
.02
1855
.787
50.
962
-0.0
080
-0.0
55-0
.009
0-0
.027
-0.0
1lm
0051
n154
6889
.468
55-6
9.30
452
2.94
9872
17.0
516
.86
1883
.777
90.
952
-0.0
36-0
.049
-0.0
-0.0
060
0.00
30lm
0344
k132
9782
.770
59-6
7.04
496
2.95
0326
15.6
515
.44
2265
.805
00.
985
0.00
40-0
.015
-0.0
030
-0.0
050
-0.0
010
lm01
14k2
6929
74.0
5413
-69.
9213
12.
9509
0315
.96
15.8
011
37.8
006
0.96
6-0
.001
0-0
.044
-0.0
060
-0.0
22-0
.003
0lm
0230
l976
7*86
.119
41-6
7.86
997
2.95
3796
17.2
817
.09
384.
8400
0.96
2-0
.008
0-0
.054
-0.0
060
-0.0
43-0
.0lm
0207
m16
357
82.0
992
-68.
8051
22.
9565
6715
.30
15.0
417
59.8
484
0.90
8-0
.011
-0.1
31-0
.006
0-0
.076
-0.0
020
lm01
01k2
4223
*76
.998
18-6
9.20
342.
9590
616
.39
16.3
019
05.7
517
0.91
3-0
.01
-0.1
16-0
.001
0-0
.05
0.0
lm01
22m
2614
*72
.711
73-6
9.41
842
2.96
3894
16.0
415
.83
2172
.692
20.
969
0.00
40-0
.038
-0.0
010
-0.0
280.
0lm
0112
k210
2474
.260
42-6
9.55
692.
9663
0715
.44
15.2
642
8.62
440.
985
-0.0
19-0
.024
-0.0
010
0.00
10-0
.001
0lm
0347
m23
821
83.9
5327
-67.
4656
92.
9709
9415
.77
15.5
211
90.7
742
0.98
-0.0
1-0
.025
-0.0
080
-0.0
130.
0lm
0032
n105
7084
.625
91-6
9.62
399
2.97
1654
15.7
315
.57
403.
6255
0.98
8-0
.021
-0.0
18-0
.001
0-0
.002
0-0
.002
0lm
0090
k350
478
.103
37-6
9.07
876
2.97
2621
15.7
315
.61
380.
7049
0.98
4-0
.012
-0.0
44-0
.006
0-0
.026
0.00
10lm
0335
k267
5682
.003
23-6
7.11
539
2.97
543
16.3
616
.32
1964
.640
80.
895
-0.0
79-0
.168
-0.0
45-0
.085
-0.0
1lm
0444
n156
0778
.124
41-6
5.80
446
2.97
7039
17.0
316
.94
1793
.759
00.
948
-0.0
26-0
.037
0.00
300.
0020
0.00
10lm
0294
m48
2574
.532
03-6
6.98
277
2.97
779
15.1
814
.95
1306
.495
00.
959
-0.0
3-0
.058
-0.0
090
-0.0
20.
0010
lm03
31k2
3717
*81
.790
68-6
6.42
442
2.99
0145
416
.42
16.3
016
60.5
094
0.96
1-0
.014
-0.0
350.
0030
-0.0
010
0.00
80
183
lm00
93m
1791
4*79
.462
77-6
9.49
655
3.01
1134
116
.08
15.9
636
1.78
240.
886
-0.0
75-0
.159
-0.0
44-0
.083
0.00
60lm
0224
m10
741*
84.8
0999
-68.
4181
43.
0232
527
16.3
316
.23
1059
.921
70.
926
0.00
10-0
.083
0.0
-0.0
17-0
.0lm
0017
m23
847
81.5
1398
-70.
2537
13.
0245
3517
.02
16.8
951
1.53
740.
992
0.0
-0.0
36-0
.003
0-0
.018
-0.0
010
lm00
33k1
7847
*85
.064
8-6
9.50
791
3.02
5998
115
.54
15.4
219
97.5
843
0.97
6-0
.007
0-0
.042
-0.0
080
-0.0
250.
0040
lm05
41n1
5871
74.3
8819
-70.
7380
53.
0272
116
.46
16.2
510
77.7
004
0.98
3-0
.003
0-0
.016
-0.0
020
-0.0
060
-0.0
020
lm00
21n5
306
83.4
1862
-69.
2315
33.
0399
1614
.86
14.7
120
07.5
547
0.98
8-0
.01
-0.0
2-0
.0-0
.001
00.
0010
lm01
33n1
1237
*71
.466
63-6
9.61
311
3.04
2348
17.0
516
.94
1478
.573
90.
948
-0.0
020
-0.0
74-0
.001
0-0
.037
-0.0
1lm
0551
m22
887
76.6
378
-70.
5936
23.
0449
2915
.41
15.0
910
94.7
740
0.93
5-0
.034
-0.0
89-0
.012
-0.0
260.
0020
lm03
13m
1266
6*78
.796
19-6
6.67
068
3.04
777
17.4
817
.32
2298
.685
60.
938
0.00
50-0
.102
-0.0
070
-0.0
75-0
.004
0lm
0191
n374
380
.036
16-6
7.85
401
3.05
3936
16.3
716
.27
1162
.681
70.
942
-0.0
16-0
.056
-0.0
010
-0.0
020
0.00
40lm
0333
k294
7481
.859
84-6
6.77
636
3.05
7151
15.5
115
.33
1961
.749
30.
97-0
.015
-0.0
290.
0010
-0.0
010
0.00
40lm
0426
n226
20*
75.0
737
-66.
2125
53.
0586
2616
.37
16.0
815
93.6
165
0.98
3-0
.008
0-0
.028
-0.0
060
-0.0
160.
0010
lm03
30m
5632
81.4
9411
-66.
2831
3.06
1442
15.6
415
.36
1277
.543
70.
978
-0.0
090
-0.0
36-0
.015
-0.0
270.
0lm
0045
k150
0786
.914
72-6
9.84
105
3.06
3892
16.6
416
.78
327.
8286
0.91
4-0
.065
-0.1
3-0
.025
-0.0
710.
0080
lm00
33l2
4296
85.1
0421
-69.
6997
43.
0665
0915
.45
15.4
315
79.7
131
0.90
9-0
.014
-0.0
81-0
.0-0
.006
00.
016
lm01
05l1
3533
77.0
2341
-70.
0387
73.
0665
3616
.06
15.8
818
54.6
134
0.97
6-0
.019
-0.0
260.
0020
-0.0
020
0.00
30lm
0022
n144
8082
.567
15-6
9.64
186
3.06
8277
16.1
115
.95
2516
.865
20.
982
-0.0
040
-0.0
35-0
.005
0-0
.027
-0.0
030
lm05
64k2
0997
77.4
4903
-71.
2801
63.
0742
1915
.10
14.8
915
72.7
651
0.98
2-0
.005
0-0
.023
-0.0
020
-0.0
020
0.00
10lm
0020
k189
27*
82.0
6909
-69.
1891
83.
0817
6415
.73
15.5
687
8.60
140.
937
-0.0
040
-0.0
76-0
.001
0-0
.017
-0.0
lm05
47l6
434
74.1
7473
-71.
6922
83.
0817
9815
.87
15.6
916
20.5
483
0.98
6-0
.015
-0.0
13-0
.00.
00.
0030
lm01
25l2
5666
73.1
602
-70.
0558
3.08
8091
14.9
814
.72
1976
.560
60.
954
-0.0
16-0
.043
-0.0
010
-0.0
010
0.00
50lm
0454
k243
1579
.701
37-6
5.71
829
3.09
6796
15.7
115
.50
1615
.572
40.
972
-0.0
12-0
.038
-0.0
080
-0.0
17-0
.001
0lm
0172
n244
6875
.397
48-6
8.30
194
3.10
2677
16.4
316
.19
808.
8476
0.89
8-0
.055
-0.1
18-0
.024
-0.0
430.
0040
lm01
13n2
4057
75.4
7999
-69.
6838
13.
1062
4416
.80
16.6
715
91.6
232
0.92
40.
0020
-0.1
29-0
.002
0-0
.089
-0.0
070
lm00
95m
9501
79.5
1951
-69.
8052
73.
1070
1914
.94
14.6
818
18.7
747
0.96
-0.0
020
-0.0
65-0
.006
0-0
.044
0.00
60lm
0346
m33
9283
.107
83-6
7.32
369
3.11
3759
15.8
315
.67
1273
.562
50.
952
-0.0
28-0
.046
-0.0
-0.0
010
0.00
80lm
0026
m14
151
82.6
8247
-70.
1901
53.
1156
0916
.86
16.9
017
71.8
904
0.90
5-0
.034
-0.0
72-0
.003
0-0
.001
00.
016
lm03
34n2
3519
81.4
573
-67.
2570
53.
1197
0115
.80
15.5
511
16.8
374
0.95
7-0
.007
0-0
.067
-0.0
18-0
.032
-0.0
070
lm03
40m
2080
183
.065
23-6
6.39
168
3.12
0686
16.8
816
.66
1592
.639
60.
958
0.00
10-0
.046
0.00
10-0
.017
0.00
10lm
0033
m31
9685
.329
26-6
9.41
801
3.12
2574
15.2
915
.12
2047
.488
20.
945
-0.0
060
-0.0
88-0
.001
0-0
.057
-0.0
lm02
07m
2758
881
.918
38-6
8.87
609
3.12
647
15.8
115
.55
1059
.872
30.
952
0.00
20-0
.062
-0.0
11-0
.038
-0.0
080
lm01
12m
2187
574
.515
57-6
9.55
377
3.13
0149
16.1
115
.97
436.
8064
0.91
8-0
.017
-0.0
87-0
.001
0-0
.013
0.00
40lm
0034
m12
6384
.649
97-6
9.77
342
3.13
4554
16.1
816
.19
1235
.645
50.
976
-0.0
17-0
.023
-0.0
010
-0.0
0.00
10lm
0202
l153
1180
.825
47-6
8.25
012
3.13
9857
15.6
315
.43
2264
.629
80.
89-0
.044
-0.1
6-0
.029
-0.0
740.
0020
lm00
45m
1216
887
.518
45-6
9.87
298
3.14
0267
15.8
915
.63
1822
.763
50.
979
-0.0
17-0
.021
0.00
400.
0060
0.00
20lm
0364
k363
386
.177
55-6
6.97
543.
1419
3816
.07
15.9
112
66.6
517
0.94
4-0
.045
-0.0
65-0
.013
-0.0
260.
0040
lm00
24m
2426
482
.570
5-6
9.88
751
3.14
4057
16.0
315
.96
1916
.594
40.
983
-0.0
14-0
.018
-0.0
010
-0.0
0.00
10lm
0580
m20
047
82.1
2091
-70.
5727
33.
1450
4516
.11
15.8
213
00.5
510
0.88
8-0
.06
-0.1
34-0
.028
-0.0
620.
0020
lm03
45k4
036
83.5
982
-66.
9814
3.15
3308
15.8
915
.70
1317
.521
60.
988
-0.0
060
-0.0
180.
0-0
.009
0-0
.001
0lm
0037
k868
984
.956
45-7
0.16
619
3.15
4552
16.2
816
.17
2404
.553
40.
953
-0.0
77-0
.087
-0.0
3-0
.065
-0.0
060
lm03
33n1
6489
82.4
1114
-66.
8476
73.
1610
615
.07
14.7
323
35.6
579
0.93
7-0
.037
-0.0
81-0
.009
0-0
.021
0.00
10
184
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0106
m99
1776
.292
5-7
0.16
055
3.16
128
15.0
214
.83
2169
.755
10.
918
-0.0
33-0
.099
-0.0
11-0
.033
-0.0
lm03
33n1
0485
82.2
1101
-66.
8129
83.
1627
9614
.75
14.4
680
9.68
470.
979
-0.0
16-0
.026
-0.0
010
-0.0
010
-0.0
020
lm03
31n1
3474
82.4
6639
-66.
5854
43.
1636
3616
.21
15.9
922
04.6
430
0.89
2-0
.062
-0.1
42-0
.029
-0.0
630.
0020
lm02
14n2
7117
82.6
9834
-68.
6736
43.
1727
815
.00
14.8
515
32.6
636
0.98
9-0
.016
-0.0
170.
0-0
.0-0
.001
0lm
0397
l969
392
.423
64-6
7.53
223.
1771
1616
.71
16.5
539
6.83
720.
991
-0.0
28-0
.019
-0.0
020
0.00
10-0
.006
0lm
0092
k175
84*
78.1
4727
-69.
5407
73.
1920
9616
.21
16.1
622
94.6
856
0.98
4-0
.002
0-0
.033
-0.0
010
-0.0
080
-0.0
lm05
43m
3009
374
.332
89-7
0.97
212
3.19
3725
15.8
515
.74
1467
.662
30.
968
-0.0
26-0
.037
-0.0
040
-0.0
060
0.00
10lm
0090
l721
5*78
.075
33-6
9.25
455
3.19
449
16.6
616
.70
2184
.728
30.
979
-0.0
030
-0.0
41-0
.005
0-0
.03
-0.0
010
lm02
23k6
698*
85.2
0794
-68.
0392
33.
2050
2416
.35
16.2
023
96.5
282
0.98
2-0
.005
0-0
.017
-0.0
020
-0.0
080
0.00
30lm
0240
m16
931
88.3
2281
-67.
7650
23.
2095
9415
.86
15.8
115
94.7
469
0.96
40.
0060
-0.0
48-0
.026
-0.0
090
-0.0
15lm
0287
m42
3973
.699
51-6
7.32
634
3.21
3864
16.2
415
.98
2298
.631
30.
979
0.00
20-0
.027
-0.0
010
-0.0
14-0
.002
0lm
0093
k230
7579
.069
35-6
9.52
412
3.21
4621
15.8
615
.72
1503
.656
30.
926
-0.0
51-0
.093
-0.0
15-0
.033
0.00
50lm
0092
m16
608
78.4
7966
-69.
5337
13.
2195
2314
.56
14.2
917
66.8
702
0.85
9-0
.056
-0.1
66-0
.033
-0.0
82-0
.005
0lm
0583
l285
4082
.667
-71.
1131
13.
2210
615
.63
15.8
012
57.5
922
0.99
4-0
.006
0-0
.009
0-0
.013
-0.0
020
0.00
20lm
0123
l255
6373
.262
4-6
9.69
687
3.22
2946
15.3
015
.10
1071
.742
70.
937
-0.0
090
-0.0
460.
0060
-0.0
010
0.00
50lm
0012
k238
0980
.148
88-6
9.57
091
3.22
4639
16.5
416
.24
2178
.704
70.
929
-0.0
48-0
.087
-0.0
15-0
.03
-0.0
030
lm02
90l1
8998
73.8
8709
-66.
5420
83.
2248
0515
.32
15.1
511
93.5
685
0.93
4-0
.021
-0.0
66-0
.002
0-0
.007
00.
0080
lm01
15n1
3901
75.4
074
-69.
9811
73.
2249
2514
.83
14.6
022
65.6
246
0.89
8-0
.026
-0.1
23-0
.011
-0.0
280.
0010
lm03
96n1
7800
92.0
6155
-67.
5855
3.23
0491
17.1
616
.98
1982
.664
10.
96-0
.056
-0.0
36-0
.003
0-0
.002
0-0
.004
0lm
0455
k235
3280
.436
22-6
5.71
217
3.23
3372
15.8
815
.80
1823
.800
11.
005
-0.0
080
-0.0
17-0
.006
0-0
.015
-0.0
020
lm02
85l1
5911
73.1
9292
-67.
2065
3.23
396
16.0
915
.90
2257
.572
70.
904
-0.0
73-0
.147
-0.0
36-0
.085
-0.0
090
lm02
21n2
2693
85.6
782
-67.
9421
23.
2345
1816
.25
16.0
914
96.7
246
0.96
9-0
.024
-0.0
32-0
.001
0-0
.003
0-0
.002
0lm
0305
k407
2*76
.493
98-6
6.97
811
3.23
9846
17.3
317
.22
2081
.911
50.
995
0.0
-0.0
16-0
.001
0-0
.007
0-0
.001
0lm
0326
k221
1779
.366
45-6
7.44
853
3.24
0622
16.4
216
.19
1254
.598
90.
966
0.00
30-0
.061
0.00
30-0
.042
0.00
10lm
0344
k197
5582
.888
9-6
7.08
871
3.24
0951
14.5
114
.30
1941
.775
00.
958
-0.0
16-0
.05
-0.0
040
-0.0
12-0
.002
0lm
0123
m18
261
73.3
5284
-69.
5029
43.
2502
4716
.99
16.9
525
45.6
634
0.93
4-0
.016
-0.1
35-0
.012
-0.0
940.
011
lm02
14n1
2207
82.9
3724
-68.
5812
13.
2529
6916
.15
16.0
442
5.62
910.
977
-0.0
5-0
.034
-0.0
19-0
.03
0.00
20lm
0207
m82
8082
.002
01-6
8.75
682
3.25
6904
17.1
316
.71
1805
.879
00.
926
-0.0
55-0
.094
-0.0
1-0
.023
0.00
80lm
0566
l188
8377
.019
25-7
1.84
052
3.25
6957
16.8
816
.64
2258
.759
90.
956
-0.0
36-0
.058
0.00
20-0
.009
0-0
.004
0lm
0106
k149
2175
.855
21-7
0.19
912
3.26
1387
15.9
215
.76
491.
5882
0.96
8-0
.025
-0.0
370.
0030
-0.0
030
0.00
80lm
0207
n226
2581
.982
3-6
9.01
378
3.26
4492
15.8
515
.76
2314
.703
70.
944
-0.0
010
-0.0
730.
0030
-0.0
46-0
.004
0lm
0353
l184
8485
.177
81-6
6.87
581
3.26
9629
16.9
216
.96
1196
.690
20.
936
-0.0
53-0
.08
-0.0
29-0
.042
-0.0
030
lm04
35k2
0023
77.2
5556
-65.
6847
63.
2815
9516
.90
16.6
822
17.8
281
0.99
2-0
.011
-0.0
32-0
.008
0-0
.03
-0.0
010
lm00
13m
1452
0*81
.319
11-6
9.48
442
3.28
8232
16.3
016
.07
1296
.524
20.
973
0.00
10-0
.032
-0.0
020
-0.0
290.
0010
lm00
90n1
2880
*78
.264
13-6
9.28
665
3.28
9332
16.9
216
.93
1887
.634
70.
971
-0.0
020
-0.0
350.
0-0
.029
0.00
20lm
0114
n174
4474
.338
31-7
0.00
589
3.29
6076
16.1
115
.92
1374
.888
70.
99-0
.005
0-0
.064
-0.0
010
-0.0
53-0
.011
lm02
00l1
8257
80.5
0925
-67.
9272
3.29
6949
14.5
914
.40
1147
.816
20.
891
-0.0
28-0
.13
-0.0
15-0
.043
0.00
80lm
0366
n990
386
.801
93-6
7.52
169
3.30
0117
16.3
916
.21
1978
.622
70.
97-0
.032
-0.0
26-0
.002
00.
0010
-0.0
020
lm04
36l1
9007
76.2
8093
-66.
1938
63.
3011
2315
.18
14.8
719
45.6
937
0.98
-0.0
12-0
.017
-0.0
0.0
-0.0
lm00
93n2
8064
*79
.270
02-6
9.70
178
3.30
5841
917
.47
17.5
413
47.9
240
0.97
7-0
.012
-0.0
420.
0020
-0.0
410.
0040
lm00
91n2
3508
79.2
7861
-69.
3369
63.
3089
8315
.79
15.6
222
08.6
229
0.94
-0.0
17-0
.064
0.0
-0.0
020
0.00
20
185
lm01
57n5
026
72.8
0917
-68.
8809
63.
3113
1916
.72
16.5
818
59.5
651
0.95
9-0
.026
-0.0
36-0
.006
0-0
.007
00.
0080
lm03
35m
1168
382
.155
68-6
7.02
177
3.31
1557
15.5
415
.32
2001
.594
80.
981
-0.0
11-0
.014
-0.0
020
-0.0
010
0.00
70lm
0113
k240
7475
.008
63-6
9.53
223
3.31
7551
16.4
716
.39
1945
.658
30.
936
-0.0
14-0
.081
-0.0
38-0
.02
-0.0
24lm
0193
n144
40*
80.2
8239
-68.
2322
73.
3188
4416
.71
16.6
025
54.7
174
0.97
30.
0020
-0.0
32-0
.002
0-0
.011
0.00
10lm
0343
l222
3983
.744
18-6
6.94
113.
3211
8815
.91
15.7
022
38.6
138
0.96
-0.0
020
-0.0
5-0
.005
0-0
.027
-0.0
040
lm03
60k1
4673
86.1
7458
-66.
3541
13.
3261
8615
.94
15.7
612
73.6
097
0.98
-0.0
24-0
.024
-0.0
58-0
.016
0.02
1lm
0353
l258
2385
.540
38-6
6.92
105
3.32
6584
16.8
316
.73
1960
.718
40.
975
-0.0
040
-0.0
34-0
.004
0-0
.017
-0.0
lm05
51k1
3555
76.3
388
-70.
5525
53.
3341
9416
.01
15.7
570
5.74
910.
989
-0.0
030
-0.0
15-0
.0-0
.009
00.
0010
lm01
26m
1555
472
.529
38-7
0.20
161
3.35
0086
15.5
615
.42
2198
.780
00.
9-0
.011
-0.1
57-0
.007
0-0
.094
-0.0
090
lm03
17n1
5681
78.6
9001
-67.
5630
83.
3593
7115
.13
14.9
820
31.4
960
0.89
1-0
.018
-0.1
31-0
.01
-0.0
340.
0080
lm02
96n1
1158
74.3
0055
-67.
5285
13.
3593
7716
.37
16.1
816
29.5
409
0.94
7-0
.017
-0.0
97-0
.018
-0.0
64-0
.01
lm03
35n9
834*
82.4
8561
-67.
1600
53.
3629
4816
.85
16.5
716
54.5
282
0.97
9-0
.01
-0.0
37-0
.006
0-0
.031
-0.0
lm05
41n1
3040
74.5
9473
-70.
7119
63.
3671
816
.78
16.5
312
59.5
290
0.98
6-0
.006
0-0
.022
-0.0
060
-0.0
16-0
.001
0lm
0157
n615
772
.818
82-6
8.88
963.
3700
7415
.17
15.0
315
29.5
687
0.95
9-0
.019
-0.0
44-0
.002
0-0
.013
0.00
20lm
0023
k426
583
.104
66-6
9.42
709
3.37
023
15.6
615
.44
1538
.652
30.
917
-0.0
080
-0.1
44-0
.005
0-0
.086
-0.0
020
lm02
16m
2662
4*82
.801
84-6
8.87
256
3.37
1126
17.3
117
.25
1659
.548
60.
949
-0.0
060
-0.0
85-0
.006
0-0
.066
-0.0
040
lm03
66m
8525
*86
.626
4-6
7.35
921
3.37
1884
16.9
316
.81
2000
.592
10.
957
-0.0
020
-0.0
66-0
.001
0-0
.051
0.00
20lm
0342
k173
2182
.663
93-6
6.74
441
3.37
3808
15.4
315
.23
1468
.674
70.
959
-0.0
040
-0.0
5-0
.005
0-0
.021
0.00
30lm
0184
l243
4976
.660
06-6
8.65
452
3.37
5765
15.5
715
.44
1247
.558
70.
977
-0.0
41-0
.031
-0.0
41-0
.019
0.00
60lm
0345
k154
8983
.545
25-6
7.05
712
3.37
8755
15.3
115
.13
1968
.654
70.
98-0
.006
0-0
.024
-0.0
040
-0.0
080
0.00
10lm
0036
m19
194*
84.5
0262
-70.
2262
83.
3817
4217
.26
17.2
114
54.7
138
0.96
30.
0010
-0.0
31-0
.001
0-0
.017
-0.0
010
lm04
46k2
0008
77.8
7865
-66.
0485
93.
3820
6516
.67
16.5
421
83.7
359
0.99
1-0
.027
-0.0
150.
00.
0-0
.005
0lm
0180
l204
43*
77.0
89-6
7.93
533.
3835
0216
.75
16.6
011
98.6
496
0.97
3-0
.001
0-0
.039
-0.0
020
-0.0
160.
0010
lm05
95k6
058*
84.5
6346
-71.
1923
73.
3862
717
.22
17.1
812
81.6
027
0.97
8-0
.004
0-0
.037
-0.0
020
-0.0
210.
0020
lm00
93n3
3808
*79
.337
19-6
9.73
054
3.39
0984
17.0
516
.98
1078
.784
41.
002
-0.0
-0.0
3-0
.001
0-0
.018
-0.0
030
lm03
65n2
3864
87.6
3119
-67.
2635
63.
4003
0716
.92
16.6
916
57.5
424
0.94
-0.0
37-0
.069
-0.0
070
-0.0
160.
0030
lm00
22k4
406
81.9
1673
-69.
4356
63.
4039
9715
.00
14.7
816
53.5
704
0.89
-0.0
35-0
.135
-0.0
23-0
.057
0.00
80lm
0333
n183
9282
.354
35-6
6.85
994
3.40
4099
16.7
516
.59
2511
.828
50.
882
-0.0
55-0
.147
-0.0
29-0
.06
0.00
60lm
0030
l133
5183
.919
36-6
9.30
042
3.40
8736
14.5
614
.40
1763
.815
40.
9-0
.024
-0.1
21-0
.009
0-0
.032
0.00
30lm
0331
m23
548
82.1
2763
-66.
4002
13.
4128
8415
.34
15.0
822
49.8
462
0.97
1-0
.024
-0.0
30.
0-0
.001
00.
0030
lm00
30l4
784
84.1
129
-69.
2377
3.41
3421
15.7
915
.86
1879
.663
90.
981
-0.0
010
-0.0
31-0
.002
0-0
.022
-0.0
030
lm01
15k1
0662
75.0
248
-69.
8139
63.
4163
7516
.49
16.4
311
22.7
615
0.91
4-0
.053
-0.0
94-0
.018
-0.0
310.
0040
lm02
94m
1493
374
.258
77-6
7.04
443.
4207
0916
.74
16.6
819
47.6
718
0.96
-0.0
17-0
.035
0.00
20-0
.001
00.
0040
lm05
84n1
8193
82.0
8746
-71.
4121
33.
4265
1815
.10
14.9
415
28.6
761
0.86
6-0
.054
-0.1
69-0
.027
-0.0
860.
0020
lm04
66n1
3702
81.5
3741
-66.
1499
23.
4327
3414
.40
14.6
017
90.8
409
0.92
2-0
.017
-0.0
81-0
.011
-0.0
020
-0.0
lm02
85m
1334
973
.533
75-6
7.03
497
3.43
8956
16.3
016
.12
782.
6400
0.93
5-0
.009
0-0
.104
-0.0
060
-0.0
62-0
.002
0lm
0175
k304
0175
.837
32-6
8.52
178
3.44
0068
15.8
715
.79
1200
.650
30.
974
-0.0
23-0
.025
-0.0
020
0.0
0.00
10lm
0105
l704
777
.006
14-6
9.97
644
3.44
2404
16.9
216
.76
762.
6691
0.98
-0.0
030
-0.0
3-0
.022
-0.0
12-0
.007
0lm
0466
l185
0181
.258
29-6
6.18
943
3.44
5012
15.8
715
.85
2132
.831
50.
927
-0.0
26-0
.072
-0.0
010
-0.0
070
0.00
60lm
0187
l139
41*
77.9
9728
-68.
9502
43.
4477
6217
.36
17.4
949
6.67
190.
963
0.00
70-0
.04
-0.0
010
-0.0
190.
0020
lm02
25k2
6953
85.2
8308
-68.
5165
53.
4528
7916
.43
16.4
018
83.7
115
0.89
6-0
.06
-0.1
3-0
.027
-0.0
530.
0040
186
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0541
n183
2074
.751
07-7
0.75
661
3.45
9966
16.7
016
.47
1067
.741
30.
932
-0.0
47-0
.089
-0.0
16-0
.035
-0.0
020
lm01
75n2
1939
*76
.460
1-6
8.62
454
3.46
2514
16.2
516
.08
1453
.844
30.
968
0.00
10-0
.034
0.0
-0.0
040
0.00
30lm
0343
k222
9983
.822
34-6
6.73
423
3.46
6279
15.5
215
.28
933.
5105
0.98
7-0
.003
0-0
.023
-0.0
020
-0.0
080
-0.0
020
lm00
33k4
809
84.8
9519
-69.
4277
3.46
8732
16.7
716
.76
1970
.622
50.
973
-0.0
15-0
.019
-0.0
030
0.00
100.
0030
lm01
66l1
2483
73.0
8311
-68.
9403
53.
4687
7815
.42
15.2
521
98.6
216
0.97
7-0
.018
-0.0
240.
0020
0.00
400.
0040
lm02
21n7
928
85.8
9611
-67.
8446
73.
4688
0215
.24
14.9
421
92.8
314
0.99
5-0
.005
0-0
.02
-0.0
11-0
.014
-0.0
lm03
21m
6695
80.5
1609
-66.
2821
13.
4697
216
.11
15.7
077
6.75
600.
979
-0.0
020
-0.0
37-0
.005
0-0
.02
-0.0
040
lm02
02l2
4207
80.6
5683
-68.
3071
23.
4721
8616
.85
16.7
518
19.7
651
0.96
4-0
.026
-0.0
33-0
.001
00.
0030
0.00
30lm
0105
n273
6577
.646
79-7
0.05
544
3.47
6907
16.4
716
.26
1992
.549
60.
96-0
.028
-0.0
310.
00.
0010
0.00
50lm
0681
m21
371
77.6
2627
-71.
9858
13.
4869
6416
.07
15.8
115
91.6
457
0.98
-0.0
18-0
.021
-0.0
010
0.00
100.
0010
lm01
77l9
536
76.0
3674
-68.
9198
43.
4910
2616
.79
16.6
039
0.76
270.
975
-0.0
080
-0.0
26-0
.002
0-0
.014
-0.0
030
lm01
57n2
0802
72.5
0246
-69.
0025
13.
4917
6616
.24
16.0
614
94.5
699
0.96
8-0
.023
-0.0
39-0
.003
00.
0020
-0.0
030
lm03
44m
8000
83.1
3842
-67.
0082
23.
4962
8815
.36
15.1
422
51.6
815
0.95
60.
0070
-0.0
650.
0010
-0.0
4-0
.006
0lm
0195
m24
877
80.0
4894
-68.
4935
33.
5080
0816
.80
16.7
574
1.79
940.
974
-0.0
34-0
.043
-0.0
060
-0.0
-0.0
020
lm01
84l1
5997
77.0
3259
-68.
6054
73.
5092
4615
.72
15.5
313
88.8
150
0.97
3-0
.008
0-0
.031
-0.0
030
-0.0
14-0
.0lm
0180
l248
3676
.772
16-6
7.96
542
3.51
3017
15.3
715
.17
1555
.622
40.
972
-0.0
14-0
.022
0.00
200.
0010
0.00
60lm
0024
k235
11*
81.6
07-6
9.77
156
3.52
2356
16.2
816
.16
523.
6086
0.98
7-0
.005
0-0
.015
-0.0
020
-0.0
10.
0020
lm00
91k1
4479
78.9
015
-69.
1394
63.
5247
5916
.67
16.4
718
44.7
458
0.97
1-0
.086
-0.1
04-0
.025
-0.0
59-0
.003
0lm
0021
n294
3583
.654
34-6
9.36
785
3.53
1735
15.5
215
.24
2144
.805
10.
989
-0.0
080
-0.0
14-0
.006
0-0
.009
0-0
.001
0lm
0013
n300
0881
.286
76-6
9.71
265
3.53
8905
15.8
715
.70
1467
.725
60.
974
-0.0
22-0
.022
0.00
100.
0010
0.00
30lm
0337
k233
4281
.890
47-6
7.46
495
3.54
3441
14.9
814
.73
1442
.816
70.
985
-0.0
43-0
.03
-0.0
16-0
.028
-0.0
040
lm03
05m
2705
276
.829
96-6
7.11
363
3.54
5493
15.9
815
.75
1082
.832
80.
925
-0.0
46-0
.092
-0.0
16-0
.035
0.00
10lm
0303
k138
61*
76.7
6351
-66.
6787
93.
5456
917
.20
17.1
121
87.7
137
0.98
-0.0
010
-0.0
280.
0010
-0.0
12-0
.001
0lm
0095
n308
4779
.720
56-7
0.07
168
3.54
6722
16.9
116
.72
325.
8327
0.91
1-0
.094
-0.1
42-0
.047
-0.0
790.
0040
lm03
43k1
3626
83.6
8195
-66.
6821
13.
5491
3415
.99
15.8
014
63.7
628
0.93
1-0
.039
-0.0
81-0
.007
0-0
.021
0.00
30lm
0182
n124
29*
77.4
1051
-68.
2277
13.
5511
7817
.52
17.4
310
88.7
063
0.97
-0.0
030
-0.0
44-0
.002
0-0
.027
-0.0
040
lm05
56k5
652
75.1
5243
-71.
5250
83.
5531
2216
.62
16.5
212
65.5
806
0.95
8-0
.03
-0.0
54-0
.0-0
.005
00.
0030
lm03
44n2
4008
*83
.255
17-6
7.26
013.
5553
4215
.85
15.6
217
64.8
820
0.97
9-0
.001
0-0
.022
-0.0
030
-0.0
050
0.00
10lm
0090
m44
7978
.380
06-6
9.08
046
3.55
8236
16.6
516
.46
1342
.933
40.
968
-0.0
29-0
.04
-0.0
060
-0.0
110.
0010
lm02
30k5
872*
86.0
5593
-67.
8259
83.
5617
1816
.97
16.9
353
9.57
150.
956
-0.0
020
-0.0
42-0
.001
0-0
.014
0.00
20lm
0344
l215
9682
.796
21-6
7.25
583
3.58
4081
16.9
616
.82
1067
.803
00.
978
-0.0
28-0
.025
-0.0
0.00
200.
0070
lm03
41l2
1911
83.4
1158
-66.
5794
43.
5847
1616
.17
16.1
419
37.7
144
0.92
3-0
.065
-0.1
04-0
.029
-0.0
53-0
.001
0lm
0343
n204
4783
.998
97-6
6.93
869
3.58
5424
15.4
915
.20
507.
5786
0.98
7-0
.008
0-0
.019
-0.0
050
-0.0
090
-0.0
010
lm02
87m
1507
073
.365
58-6
7.40
108
3.58
6708
16.8
816
.78
2262
.847
00.
966
-0.0
31-0
.019
-0.0
030
0.00
400.
0090
lm03
74m
1672
4*88
.408
74-6
7.07
084
3.59
3318
16.8
016
.65
1784
.833
80.
978
-0.0
040
-0.0
29-0
.006
0-0
.018
-0.0
030
lm01
21l2
2345
73.0
4166
-69.
3346
23.
5953
9216
.67
16.5
214
24.7
830
0.94
-0.0
38-0
.062
-0.0
060
-0.0
150.
0030
lm03
23n1
1823
*80
.603
03-6
6.81
992
3.59
9714
16.6
916
.47
2025
.511
40.
982
-0.0
070
-0.0
19-0
.003
0-0
.007
0-0
.0lm
0110
l216
1374
.046
57-6
9.35
041
3.60
6183
15.5
815
.34
708.
8980
0.96
70.
0030
-0.0
640.
0030
-0.0
36-0
.002
0lm
0343
l158
4083
.656
09-6
6.85
268
3.60
9432
14.8
514
.61
540.
5105
0.92
4-0
.022
-0.0
670.
0-0
.004
00.
01lm
0340
l679
182
.663
04-6
6.45
076
3.61
2113
16.8
716
.78
1267
.593
00.
875
-0.1
07-0
.158
-0.0
5-0
.079
0.00
90lm
0366
l773
486
.224
26-6
7.50
409
3.61
3542
16.6
116
.45
1824
.769
50.
956
-0.0
12-0
.075
-0.0
060
-0.0
49-0
.0
187
lm01
63l2
4856
74.1
3186
-68.
2975
93.
6183
4716
.37
16.2
923
89.5
005
0.98
4-0
.001
0-0
.015
-0.0
060
-0.0
030
-0.0
010
lm00
15n3
0492
81.2
8868
-70.
0728
63.
6255
1316
.49
16.3
515
32.6
440
0.97
1-0
.008
0-0
.06
-0.0
070
-0.0
420.
0040
lm00
93k2
7461
79.2
0581
-69.
5460
83.
6282
9915
.62
15.4
393
1.49
890.
96-0
.005
0-0
.051
-0.0
050
-0.0
26-0
.001
0lm
0091
l251
5879
.110
48-6
9.34
246
3.63
4311
15.2
815
.24
1441
.748
90.
927
-0.0
3-0
.077
-0.0
15-0
.03
0.00
40lm
0560
m17
742
77.7
2478
-70.
5573
93.
6409
8916
.33
16.1
378
8.76
770.
956
-0.0
29-0
.042
0.00
10-0
.001
00.
0040
lm00
13m
2236
381
.343
14-6
9.52
733
3.64
6111
16.7
416
.73
1784
.774
80.
98-0
.015
-0.0
15-0
.00.
0040
0.00
40lm
0225
n759
285
.637
34-6
8.54
787
3.65
2101
15.7
415
.52
1108
.850
10.
948
-0.0
080
-0.0
86-0
.008
0-0
.063
0.00
60lm
0184
l495
7*76
.909
69-6
8.53
939
3.65
273
16.5
316
.62
1059
.851
20.
989
-0.0
020
-0.0
270.
0-0
.014
0.00
10lm
0303
n178
56*
76.9
238
-66.
8528
53.
6554
216
.54
16.3
212
01.5
979
0.98
3-0
.003
0-0
.026
-0.0
030
-0.0
190.
0010
lm03
43l1
6325
83.4
0523
-66.
8571
43.
6555
3315
.13
14.8
923
44.6
483
0.95
9-0
.002
0-0
.058
-0.0
14-0
.038
0.00
70lm
0184
k134
0976
.689
95-6
8.43
575
3.65
9249
16.1
616
.04
2057
.484
60.
969
-0.0
28-0
.032
-0.0
020
-0.0
090
0.00
20lm
0343
k228
5983
.586
19-6
6.73
907
3.66
4324
15.3
015
.07
1901
.848
30.
847
-0.0
38-0
.18
-0.0
21-0
.057
0.02
5lm
0207
m69
63*
81.8
4109
-68.
7502
73.
6773
3215
.35
15.1
213
74.9
246
0.94
-0.0
020
-0.0
8-0
.0-0
.023
-0.0
lm01
00l2
2336
*76
.063
4-6
9.35
643
3.67
9464
16.8
216
.85
2294
.664
70.
985
-0.0
010
-0.0
26-0
.001
0-0
.018
0.0
lm05
65k6
340
78.4
8164
-71.
1866
3.69
0546
14.7
914
.60
1142
.665
60.
97-0
.019
-0.0
3-0
.0-0
.001
00.
0030
lm00
33n1
8886
85.4
3758
-69.
6679
3.69
4692
14.7
014
.44
1950
.619
30.
987
-0.0
010
-0.0
15-0
.003
0-0
.003
00.
0010
lm03
44l1
9313
82.7
1621
-67.
2402
73.
6959
3515
.18
14.9
620
17.5
704
0.96
70.
0020
-0.0
51-0
.02
-0.0
2-0
.012
lm00
13n8
661
81.3
1174
-69.
6034
63.
7145
2616
.00
15.9
253
2.51
850.
971
-0.0
-0.0
37-0
.002
0-0
.02
0.0
lm00
33m
1706
385
.307
12-6
9.50
278
3.71
8525
14.8
414
.67
388.
8496
0.98
4-0
.01
-0.0
13-0
.002
0-0
.001
00.
0010
lm03
31n1
614
82.1
504
-66.
4287
83.
7206
916
.76
16.5
914
42.8
167
0.99
2-0
.018
-0.0
11-0
.013
-0.0
10.
0020
lm01
25n2
3449
73.4
2151
-70.
0405
43.
7387
1415
.31
15.1
119
76.5
606
0.88
1-0
.06
-0.1
51-0
.027
-0.0
70.
0030
lm05
51m
2068
1*76
.877
3-7
0.57
786
3.74
0874
17.6
117
.43
1838
.729
20.
961
0.00
60-0
.063
0.00
20-0
.047
0.0
lm02
83n1
5751
73.6
2331
-66.
8483
3.74
2176
16.6
216
.38
2255
.568
00.
961
-0.0
2-0
.065
-0.0
19-0
.044
-0.0
070
lm04
24n5
194
74.8
0668
-65.
7366
43.
7442
2614
.62
14.4
211
83.6
480
0.89
7-0
.018
-0.1
18-0
.018
-0.0
460.
0080
lm00
13n3
2504
81.2
7858
-69.
7254
93.
7450
0816
.28
16.1
712
66.5
735
0.98
7-0
.01
-0.0
13-0
.002
00.
0010
0.00
40lm
0291
l489
175
.000
36-6
6.42
614
3.75
1829
15.4
715
.14
2257
.860
50.
913
-0.0
41-0
.109
-0.0
15-0
.036
0.00
70lm
0027
k382
3*82
.861
65-7
0.13
678
3.76
1414
16.1
916
.10
511.
5406
0.95
8-0
.014
-0.0
39-0
.003
0-0
.005
00.
0030
lm01
01n2
5168
77.6
1906
-69.
3465
93.
7734
0815
.86
15.5
650
8.57
180.
977
0.01
2-0
.044
-0.0
11-0
.02
-0.0
14lm
0207
k168
3781
.734
28-6
8.80
786
3.77
5084
15.7
615
.48
428.
6362
1.0
-0.0
2-0
.003
0-0
.001
0-0
.006
0-0
.001
0lm
0092
m24
157
78.2
7531
-69.
5762
33.
7795
2815
.91
15.7
624
60.9
331
0.99
3-0
.036
-0.0
13-0
.01
-0.0
160.
0010
lm02
14n8
614
82.9
6898
-68.
5586
93.
7858
4516
.52
16.4
422
42.6
112
0.97
4-0
.009
0-0
.012
-0.0
51-0
.014
-0.0
21lm
0333
k491
481
.804
24-6
6.62
823.
7902
6915
.57
15.3
818
95.6
174
0.98
5-0
.006
0-0
.011
-0.0
18-0
.003
0-0
.009
0lm
0266
n880
892
.493
46-6
9.05
534
3.79
1436
16.6
116
.37
503.
7005
0.93
3-0
.053
-0.0
69-0
.009
0-0
.018
0.01
1lm
0020
m22
505
82.6
2036
-69.
1940
73.
7916
9115
.68
15.5
522
97.7
436
0.92
1-0
.029
-0.0
7-0
.0-0
.009
00.
012
lm02
85k2
2500
73.2
004
-67.
1005
13.
7927
815
.83
15.7
022
58.7
408
0.95
8-0
.018
-0.0
410.
0010
-0.0
030
0.00
50lm
0030
l159
0484
.160
62-6
9.32
033
3.79
7121
15.2
115
.21
2312
.749
10.
977
-0.0
11-0
.017
-0.0
0.0
0.00
60lm
0555
m16
884
76.5
4721
-71.
2783
63.
8007
6716
.44
16.3
019
87.5
504
0.90
7-0
.04
-0.1
15-0
.018
-0.0
39-0
.001
0lm
0550
m52
1275
.627
54-7
0.48
438
3.80
1039
15.8
815
.55
2204
.602
10.
974
-0.0
040
-0.0
35-0
.006
0-0
.017
0.00
10lm
0257
l893
191
.105
99-6
8.92
443
3.81
0748
15.5
315
.19
2264
.805
10.
933
0.01
-0.1
06-0
.004
0-0
.074
0.01
lm05
83l2
8572
82.3
6022
-71.
1147
13.
8228
9516
.57
16.5
512
66.6
017
0.98
4-0
.002
0-0
.024
-0.0
-0.0
14-0
.0lm
0050
n162
62*
88.3
4579
-69.
3054
73.
8284
881
16.8
516
.71
390.
7966
0.95
10.
018
-0.0
940.
0090
-0.0
840.
0010
188
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0125
k810
672
.823
49-6
9.80
212
3.84
3898
15.8
615
.80
1888
.570
70.
961
-0.0
27-0
.053
-0.0
080
-0.0
18-0
.001
0lm
0367
l133
3187
.241
67-6
7.55
966
3.84
6704
16.4
916
.28
1804
.860
10.
953
-0.0
49-0
.057
-0.0
080
-0.0
140.
0050
lm01
12l2
2418
*74
.077
03-6
9.69
282
3.85
1004
17.1
817
.04
1804
.762
10.
957
-0.0
010
-0.0
720.
0020
-0.0
660.
011
lm00
90n3
0909
78.3
2119
-69.
3889
43.
8520
9715
.73
15.6
417
11.9
284
0.98
8-0
.01
-0.0
18-0
.005
0-0
.013
-0.0
lm00
30l1
1056
84.2
0283
-69.
2832
93.
8535
5815
.33
15.1
443
3.67
990.
95-0
.016
-0.0
37-0
.056
-0.0
020
-0.0
21lm
0090
k101
70*
78.1
2455
-69.
1211
63.
8547
9616
.56
16.5
022
02.6
635
0.98
2-0
.004
0-0
.028
-0.0
040
-0.0
080
0.00
10lm
0175
n288
6976
.495
99-6
8.66
344
3.85
5031
16.3
716
.03
381.
8370
0.93
4-0
.039
-0.0
85-0
.011
-0.0
310.
0lm
0020
k155
8182
.066
69-6
9.16
523
3.86
3955
14.9
714
.77
1076
.890
30.
966
-0.0
030
-0.0
490.
0-0
.022
-0.0
010
lm00
26n7
027
82.3
5945
-70.
3028
53.
8704
8516
.17
16.2
866
5.84
440.
936
-0.0
44-0
.091
-0.0
28-0
.046
0.00
50lm
0024
k652
981
.831
58-6
9.68
507
3.87
2692
16.3
516
.17
931.
4717
0.94
9-0
.049
-0.0
65-0
.009
0-0
.02
-0.0
020
lm01
17m
1273
075
.629
58-7
0.18
216
3.87
3811
16.3
416
.22
2208
.749
80.
912
-0.1
-0.1
31-0
.05
-0.0
84-0
.004
0lm
0177
l975
475
.870
27-6
8.92
221
3.89
0098
15.4
814
.96
2300
.633
20.
917
-0.0
57-0
.12
-0.0
2-0
.058
0.00
60lm
0362
n518
286
.733
8-6
6.78
992
3.89
1688
16.1
615
.96
892.
6980
0.92
8-0
.009
0-0
.114
-0.0
080
-0.0
86-0
.01
lm01
12m
2139
474
.533
96-6
9.55
076
3.89
5853
15.3
515
.21
2389
.516
40.
96-0
.021
-0.0
36-0
.001
00.
00.
0010
lm00
10l2
3506
80.0
8352
-69.
3623
63.
9040
7716
.22
16.1
214
92.6
657
0.95
3-0
.023
-0.0
29-0
.001
00.
0030
0.00
30lm
0121
l272
0873
.122
09-6
9.36
341
3.90
7531
15.7
515
.63
1821
.706
40.
967
-0.0
15-0
.024
-0.0
45-0
.007
00.
019
lm03
54l2
3952
84.2
7038
-67.
2700
33.
9094
0415
.83
15.5
412
90.5
659
0.90
4-0
.078
-0.1
24-0
.041
-0.0
720.
0060
lm03
45n2
7198
84.2
7032
-67.
2701
13.
9094
7415
.70
15.4
610
59.9
019
0.89
6-0
.073
-0.1
24-0
.034
-0.0
550.
0050
lm00
55k6
835
88.9
7061
-69.
7922
3.91
5014
16.4
516
.36
510.
6379
0.95
9-0
.034
-0.0
340.
00.
0010
0.00
30lm
0165
n592
874
.569
77-6
8.53
736
3.92
6326
15.0
214
.82
1093
.774
00.
899
-0.0
35-0
.13
-0.0
14-0
.04
0.00
30lm
0120
m20
609
72.7
3139
-69.
1775
73.
9316
6516
.82
16.6
622
41.5
917
0.87
1-0
.053
-0.1
87-0
.035
-0.0
70.
0010
lm02
87m
2203
673
.601
84-6
7.44
495
3.94
5121
16.2
016
.03
2074
.934
10.
896
-0.0
81-0
.158
-0.0
41-0
.092
-0.0
050
lm01
87m
9985
78.1
6571
-68.
7674
83.
9453
1916
.76
16.5
984
2.65
350.
931
-0.0
77-0
.106
-0.0
3-0
.055
-0.0
040
lm03
45k9
648
83.7
3768
-67.
0169
93.
9482
3115
.44
15.2
419
55.7
165
0.96
6-0
.012
-0.0
320.
0010
0.00
300.
0010
lm04
43l6
372
78.8
1883
-65.
5297
43.
9491
8516
.65
16.4
712
67.5
402
0.96
2-0
.048
-0.0
52-0
.009
0-0
.017
-0.0
020
lm02
00l6
074
80.5
7817
-67.
8390
13.
9504
7815
.89
15.6
512
73.5
276
0.98
5-0
.002
0-0
.029
-0.0
010
-0.0
2-0
.003
0lm
0377
l548
189
.056
96-6
7.56
23.
9515
4116
.72
16.4
915
72.8
209
0.93
3-0
.041
-0.0
65-0
.008
0-0
.014
0.00
70lm
0091
m37
97*
79.4
4924
-69.
0710
83.
9545
17.1
316
.93
490.
7461
0.94
-0.0
010
-0.1
37-0
.006
0-0
.095
-0.0
030
lm03
31k2
1866
81.8
5552
-66.
3928
83.
9591
1316
.76
16.5
315
31.6
643
0.98
2-0
.015
-0.0
12-0
.041
-0.0
080
-0.0
19lm
0015
k865
880
.912
97-6
9.80
448
3.95
9962
16.1
716
.32
521.
5561
0.98
7-0
.011
-0.0
16-0
.001
00.
0010
0.00
10lm
0364
l141
9386
.158
85-6
7.20
871
3.95
9976
16.5
316
.39
2018
.584
60.
937
-0.0
52-0
.066
-0.0
12-0
.032
0.00
30lm
0331
l260
4281
.984
27-6
6.57
005
3.96
9029
15.9
515
.81
1805
.887
70.
871
-0.0
59-0
.153
-0.0
38-0
.062
0.01
3lm
0300
m22
019
75.9
5469
-66.
3924
63.
9865
2916
.62
16.3
615
49.6
231
0.97
3-0
.003
0-0
.009
0-0
.056
-0.0
2-0
.029
lm03
17k7
631
78.3
3439
-67.
3594
33.
9901
2615
.61
15.3
321
41.8
302
0.99
-0.0
-0.0
22-0
.025
-0.0
050
0.02
lm01
84n2
6760
77.4
8968
-68.
6582
34.
0224
2815
.38
15.2
015
47.6
132
0.87
7-0
.058
-0.1
68-0
.024
-0.0
710.
0080
lm00
12n4
832
80.2
8006
-69.
5904
4.02
7903
16.6
516
.30
2162
.751
60.
977
-0.0
49-0
.045
-0.0
040
-0.0
030
0.00
90lm
0021
l453
0*82
.869
46-6
9.23
199
4.03
7538
715
.06
14.8
016
21.5
653
0.91
7-0
.008
0-0
.11
-0.0
030
-0.0
370.
0020
lm06
00k2
5018
85.5
8539
-70.
6266
74.
0466
0714
.85
14.7
520
56.4
893
0.96
7-0
.019
-0.0
330.
0010
-0.0
0.00
40lm
0317
k229
7878
.156
81-6
7.47
264.
0519
1614
.67
14.4
111
45.6
945
0.97
-0.0
23-0
.027
0.00
10-0
.00.
0050
lm00
22k4
055
81.9
6774
-69.
4334
64.
0549
5116
.23
16.0
919
34.7
295
0.89
-0.0
58-0
.124
-0.0
25-0
.046
0.00
80lm
0224
m12
405
84.6
8721
-68.
4285
14.
0619
2816
.41
16.3
214
53.8
637
0.92
-0.0
34-0
.091
-0.0
1-0
.023
0.00
50
189
lm03
87l8
658
90.6
794
-67.
5258
44.
0647
3116
.82
16.6
216
54.5
882
0.98
3-0
.021
-0.0
20.
0010
0.0
0.00
20lm
0101
k237
8477
.111
18-6
9.20
004
4.06
9483
15.6
615
.48
491.
5882
0.97
-0.0
21-0
.012
-0.0
040
0.00
200.
012
lm02
23n1
9693
85.5
091
-68.
2701
54.
0754
5515
.32
15.1
416
61.5
381
0.93
9-0
.047
-0.0
96-0
.022
-0.0
440.
0030
lm01
74k1
6339
75.1
3969
-68.
4516
84.
0809
4815
.44
15.2
812
12.6
916
0.94
7-0
.01
-0.0
390.
0010
0.00
100.
015
lm02
43m
4872
89.4
1949
-68.
078
4.08
1141
15.2
214
.96
950.
4929
0.99
9-0
.012
-0.0
030
-0.0
010
-0.0
010
-0.0
040
lm03
43n2
1737
83.9
8722
-66.
8859
94.
0864
9214
.66
14.3
694
7.51
930.
988
-0.0
090
-0.0
14-0
.002
0-0
.005
0-0
.001
0lm
0357
k750
085
.565
95-6
7.35
875
4.09
4591
15.0
214
.77
1263
.623
40.
923
-0.0
25-0
.072
-0.0
030
-0.0
060
0.01
3lm
0691
m10
693
79.5
6567
-71.
9110
64.
0973
8916
.28
16.0
318
27.7
694
0.92
-0.0
48-0
.086
-0.0
11-0
.021
0.00
70lm
0337
k108
4782
.019
22-6
7.37
806
4.11
5728
14.8
514
.60
1875
.667
80.
889
-0.0
5-0
.165
-0.0
26-0
.07
0.00
70lm
0170
n123
0575
.522
14-6
7.88
198
4.11
6486
15.8
015
.58
1962
.691
10.
92-0
.011
-0.1
22-0
.005
0-0
.071
-0.0
030
lm05
85m
1341
982
.982
42-7
1.22
553
4.11
8108
16.8
516
.53
759.
8288
0.98
6-0
.062
-0.0
32-0
.026
-0.0
360.
0010
lm02
06n2
6379
80.9
7014
-69.
0272
24.
1276
6514
.78
14.4
517
88.8
132
0.91
2-0
.033
-0.1
13-0
.008
0-0
.04
0.0
lm03
43k2
1879
83.5
8343
-66.
7333
24.
1631
7915
.89
15.6
818
50.6
457
0.99
1-0
.004
0-0
.019
-0.0
040
-0.0
12-0
.001
0lm
0344
l216
5682
.788
69-6
7.25
619
4.16
4156
15.5
115
.30
1604
.622
40.
989
-0.0
050
-0.0
23-0
.009
0-0
.013
0.00
20lm
0101
k179
6876
.824
63-6
9.16
519
4.17
6462
15.3
315
.19
1792
.798
40.
868
-0.0
69-0
.173
-0.0
36-0
.079
0.00
70lm
0466
l160
7781
.342
82-6
6.16
931
4.17
9091
14.1
414
.13
1547
.682
50.
956
-0.0
050
-0.0
180.
0030
-0.0
060
0.00
40lm
0020
k869
182
.099
51-6
9.11
761
4.17
9714
.77
14.5
594
7.47
960.
966
-0.0
050
-0.0
37-0
.003
0-0
.015
0.00
20lm
0344
m20
206
82.9
4425
-67.
0883
54.
1814
1215
.24
15.0
715
67.7
128
0.93
2-0
.016
-0.0
550.
0020
0.00
100.
013
lm01
25n6
068
73.3
3501
-69.
9366
94.
1877
5615
.92
15.7
922
25.5
710
0.93
-0.0
33-0
.076
-0.0
1-0
.02
0.00
70lm
0110
m10
393
74.4
2887
-69.
1106
24.
1926
2516
.24
16.0
812
69.5
361
0.93
-0.0
74-0
.096
-0.0
27-0
.049
0.00
20lm
0103
k263
1177
.042
34-6
9.54
322
4.20
3111
16.3
016
.26
1891
.626
10.
9-0
.057
-0.1
16-0
.034
-0.0
510.
013
lm03
47n6
886*
84.0
5524
-67.
4972
24.
2108
5816
.07
15.9
712
91.5
689
0.98
4-0
.01
-0.0
4-0
.007
0-0
.034
-0.0
040
lm03
66l1
6862
86.2
1569
-67.
5757
74.
2325
2715
.74
15.5
517
60.8
354
0.98
6-0
.015
-0.0
14-0
.001
0-0
.001
0-0
.001
0lm
0346
k238
2582
.786
51-6
7.48
403
4.24
9299
14.9
014
.67
385.
6731
0.95
5-0
.014
-0.0
66-0
.034
-0.0
29-0
.019
lm01
77l1
6525
76.1
8763
-68.
9676
74.
2535
7716
.56
16.4
012
74.5
110
0.96
-0.0
050
-0.0
45-0
.001
0-0
.02
0.00
20lm
0313
m25
631
78.7
6599
-66.
7502
44.
2639
3416
.40
16.1
275
5.72
540.
983
-0.0
080
-0.0
14-0
.004
0-0
.01
0.00
20lm
0466
n219
5981
.513
27-6
6.21
313
4.27
3267
16.2
416
.04
1262
.522
70.
971
-0.0
24-0
.038
0.00
10-0
.001
00.
0030
lm00
94l2
5321
78.0
1319
-70.
0595
74.
2749
8216
.48
16.5
118
91.6
482
0.97
1-0
.016
-0.0
330.
0010
0.00
30-0
.001
0lm
0122
l155
8172
.060
89-6
9.66
111
4.28
4122
15.7
015
.51
2257
.566
90.
984
-0.0
050
-0.0
2-0
.005
0-0
.004
00.
0010
lm01
13l2
8118
*75
.282
82-6
9.70
783
4.30
563
16.2
616
.21
2516
.765
40.
973
-0.0
060
-0.0
26-0
.005
0-0
.002
00.
0lm
0376
m47
7388
.481
33-6
7.33
126
4.30
6026
15.9
115
.74
512.
7044
0.98
6-0
.018
-0.0
090
0.00
100.
00.
0020
lm01
25l6
652
73.1
0946
-69.
9420
84.
3134
6415
.72
15.5
421
40.8
024
0.95
2-0
.013
-0.0
40.
0010
0.00
200.
0090
lm02
97n1
4819
75.2
1066
-67.
5588
4.31
8638
15.5
515
.26
1934
.637
70.
989
-0.0
21-0
.014
-0.0
010
-0.0
-0.0
030
lm04
67k1
8222
82.1
4873
-66.
0321
54.
3202
2415
.97
15.7
941
6.62
770.
97-0
.009
0-0
.031
0.0
-0.0
0.00
10lm
0187
m17
967
78.3
8296
-68.
8134
4.32
3013
16.2
716
.00
1579
.681
30.
97-0
.012
-0.0
4-0
.024
-0.0
14-0
.008
0lm
0467
n178
5082
.431
97-6
6.19
001
4.32
4035
15.9
415
.68
2309
.713
00.
968
0.0
-0.0
61-0
.001
0-0
.04
-0.0
lm02
05n1
7550
81.9
3375
-68.
6001
64.
3320
4116
.77
16.5
214
55.7
692
0.94
2-0
.004
0-0
.092
-0.0
070
-0.0
61-0
.006
0lm
0344
n907
483
.150
2-6
7.16
532
4.33
4821
14.7
814
.54
825.
8571
0.92
1-0
.011
-0.1
04-0
.005
0-0
.044
-0.0
010
lm05
77k2
2178
80.3
2518
-71.
684
4.33
6319
16.1
815
.97
2161
.771
80.
927
-0.0
24-0
.068
0.00
10-0
.003
00.
0060
lm03
31k2
2811
81.8
0895
-66.
3997
4.33
7633
15.0
914
.91
1355
.927
30.
926
-0.0
32-0
.085
-0.0
050
-0.0
210.
0050
lm00
91n3
2274
79.3
2109
-69.
3828
24.
3396
2815
.92
15.8
893
1.49
890.
967
-0.0
15-0
.032
0.00
10-0
.00.
0020
190
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0211
k238
0383
.575
7-6
7.79
595
4.34
1552
15.7
215
.53
1116
.842
00.
973
-0.0
22-0
.018
0.0
0.00
200.
0060
lm03
17k2
1886
78.2
5325
-67.
4642
4.35
9786
14.8
414
.76
1935
.659
90.
929
-0.0
25-0
.086
-0.0
080
-0.0
220.
0050
lm03
44n1
1851
83.1
9611
-67.
1833
14.
4025
8515
.60
15.3
784
5.69
380.
99-0
.003
0-0
.012
0.0
-0.0
040
-0.0
010
lm03
37k2
5005
81.7
5818
-67.
4771
84.
4088
2215
.00
14.7
619
06.8
403
0.95
30.
0050
-0.0
67-0
.01
-0.0
390.
012
lm00
93m
1195
579
.374
73-6
9.46
628
4.42
2796
16.0
315
.87
1451
.737
60.
963
0.00
20-0
.057
-0.0
050
-0.0
33-0
.002
0lm
0292
l554
1*74
.122
64-6
6.79
039
4.44
2046
16.7
616
.58
2245
.621
60.
967
0.00
10-0
.05
-0.0
010
-0.0
320.
0020
lm00
34m
4602
*84
.663
94-6
9.80
398
4.45
4894
16.7
316
.80
2223
.628
80.
983
0.00
20-0
.022
-0.0
010
-0.0
16-0
.001
0lm
0290
m45
1074
.261
76-6
6.27
256
4.45
663
15.7
215
.58
382.
7421
0.87
3-0
.052
-0.1
41-0
.025
-0.0
520.
017
lm01
97m
2083
579
.942
83-6
8.83
562
4.48
8418
15.9
915
.78
397.
8481
0.99
4-0
.004
0-0
.012
-0.0
110.
00.
0040
lm00
90n2
0034
78.2
5898
-69.
3276
84.
5023
6315
.79
15.7
859
0.47
790.
978
0.00
10-0
.033
-0.0
22-0
.014
0.00
90lm
0021
l159
8582
.869
38-6
9.29
774
4.50
2779
14.8
314
.59
1082
.878
40.
867
-0.0
33-0
.175
-0.0
21-0
.057
0.00
60lm
0551
l214
1976
.056
41-7
0.73
615
4.50
3208
15.7
415
.52
837.
7661
0.98
-0.0
1-0
.019
-0.0
12-0
.006
0-0
.001
0lm
0243
m48
2489
.251
68-6
8.07
858
4.51
7961
15.8
415
.64
1987
.634
00.
964
-0.0
050
-0.0
46-0
.003
0-0
.027
-0.0
050
lm00
30l9
014
83.8
5675
-69.
2682
34.
5236
2215
.20
15.0
944
0.75
440.
967
-0.0
010
-0.0
39-0
.001
0-0
.019
-0.0
010
lm02
07m
1144
682
.147
97-6
8.77
459
4.52
6578
14.3
114
.03
741.
8064
0.86
70.
0010
-0.1
58-0
.007
0-0
.038
0.00
60lm
0182
n150
9977
.353
68-6
8.24
348
4.53
5109
15.5
915
.41
2263
.634
60.
983
-0.0
010
-0.0
17-0
.005
0-0
.003
0-0
.0lm
0283
m15
233
73.4
938
-66.
7020
54.
5408
4415
.45
15.1
517
83.7
591
0.93
3-0
.075
-0.1
15-0
.041
-0.0
750.
0020
lm00
21l1
5606
82.8
0078
-69.
2958
84.
5575
8115
.11
14.8
814
92.6
909
0.99
2-0
.004
0-0
.018
-0.0
040
-0.0
120.
0010
lm00
91l1
4577
78.9
1731
-69.
2871
94.
5666
5716
.40
16.5
917
91.7
729
0.96
3-0
.049
-0.0
67-0
.028
-0.0
43-0
.001
0lm
0027
n985
6*83
.481
8-7
0.31
804
4.56
889
17.2
917
.21
1883
.676
10.
947
-0.0
040
-0.0
860.
0020
-0.0
57-0
.003
0lm
0190
n218
6979
.392
04-6
7.93
565
4.57
1853
15.2
515
.04
2172
.765
80.
967
0.00
30-0
.043
-0.0
010
-0.0
240.
0020
lm01
14k1
9051
73.9
6926
-69.
8695
24.
5774
7115
.33
15.1
353
2.53
050.
873
-0.0
38-0
.152
-0.0
25-0
.054
0.00
10lm
0020
n196
1582
.673
97-6
9.32
445
4.58
5353
14.1
013
.94
754.
7607
0.90
9-0
.034
-0.0
92-0
.01
-0.0
080
-0.0
020
lm01
87m
1149
678
.387
39-6
8.77
464
4.59
1479
16.3
116
.07
1892
.839
00.
903
-0.0
9-0
.144
-0.0
42-0
.074
-0.0
020
lm00
33m
2170
085
.423
29-6
9.53
002
4.61
3339
15.1
915
.07
799.
8171
0.98
4-0
.005
0-0
.019
-0.0
050
-0.0
050
0.00
30lm
0133
n160
0071
.607
32-6
9.64
112
4.61
3573
16.4
216
.26
2305
.600
60.
994
-0.0
35-0
.018
0.00
10-0
.002
0-0
.004
0lm
0025
m30
936
83.3
2691
-69.
9173
74.
6368
4516
.37
16.3
510
92.6
860
0.89
1-0
.088
-0.1
39-0
.039
-0.0
680.
0080
lm02
11m
1885
9*83
.909
38-6
7.76
044
4.64
3221
916
.65
16.5
321
71.7
647
0.92
7-0
.011
-0.0
760.
0020
-0.0
080
-0.0
lm01
66m
2251
873
.367
13-6
8.84
454.
6587
9716
.63
16.4
918
11.7
418
0.98
50.
0020
-0.0
23-0
.008
0-0
.015
0.00
60lm
0550
k115
2375
.253
22-7
0.52
935
4.66
509
16.2
916
.02
1278
.541
50.
984
-0.0
060
-0.0
25-0
.006
0-0
.013
0.00
10lm
0185
n116
3678
.274
15-6
8.56
689
4.67
3342
16.3
716
.18
1255
.565
00.
946
-0.0
46-0
.068
-0.0
14-0
.031
0.00
20lm
0135
k140
0870
.902
69-6
9.83
939
4.67
4718
16.4
016
.38
737.
8651
0.97
7-0
.02
-0.0
20.
0020
0.00
100.
0010
lm03
50l4
429
84.4
6882
-66.
4321
84.
6868
9615
.42
15.2
720
09.6
418
0.98
1-0
.015
-0.0
160.
0010
0.00
300.
0030
lm01
35k9
012
71.2
563
-69.
8038
4.70
8726
16.2
216
.16
2254
.557
80.
992
-0.0
21-0
.011
-0.0
0.00
10-0
.002
0lm
0093
m30
768
79.3
3994
-69.
5646
74.
7211
5616
.56
16.4
214
40.8
605
0.90
9-0
.12
-0.1
35-0
.061
-0.0
880.
0060
lm02
25k1
8526
85.5
041
-68.
4653
24.
7506
9916
.19
16.0
115
47.7
200
0.97
6-0
.002
0-0
.01
-0.0
46-0
.006
0-0
.024
lm03
56m
1914
684
.794
8-6
7.43
387
4.75
5264
15.4
315
.22
2224
.790
30.
951
-0.0
020
-0.0
67-0
.011
-0.0
390.
0080
lm01
77m
1914
876
.591
68-6
8.82
087
4.76
0853
16.6
716
.48
802.
7677
0.98
1-0
.013
-0.0
25-0
.001
00.
0010
-0.0
010
lm05
51l2
0848
*76
.230
95-7
0.73
175
4.76
1963
615
.03
14.7
973
1.82
060.
986
-0.0
040
-0.0
16-0
.001
0-0
.004
00.
0lm
0333
n656
882
.251
58-6
6.78
851
4.77
0854
15.1
114
.84
1791
.790
80.
953
-0.0
22-0
.042
-0.0
010
0.00
200.
0050
lm05
43m
8169
74.5
4655
-70.
8411
44.
7778
6216
.01
15.7
619
26.6
584
0.94
9-0
.007
0-0
.078
-0.0
19-0
.044
0.00
90
191
lm01
80k1
6760
76.8
1278
-67.
7548
44.
7842
8815
.54
15.2
619
27.6
826
0.97
60.
0-0
.044
-0.0
070
-0.0
18-0
.004
0lm
0567
k232
5978
.473
29-7
1.64
955
4.80
3925
16.5
616
.38
1312
.507
90.
977
-0.0
27-0
.026
0.0
0.00
20-0
.004
0lm
0427
l127
6775
.272
-66.
1554
44.
8059
3216
.12
15.8
611
24.7
340
0.98
1-0
.006
0-0
.028
-0.0
010
-0.0
160.
0030
lm00
31n6
676
85.4
6572
-69.
2396
94.
8534
3115
.58
15.5
182
8.65
780.
954
0.00
50-0
.04
-0.0
14-0
.014
-0.0
070
lm02
94l2
5574
73.8
772
-67.
2727
44.
8554
5815
.50
15.3
219
47.6
718
0.97
1-0
.033
-0.0
370.
0030
0.0
-0.0
030
lm03
75l1
4140
89.0
3712
-67.
2052
54.
8706
5716
.50
16.3
680
6.73
110.
902
-0.0
87-0
.133
-0.0
49-0
.07
0.00
10lm
0311
n131
0878
.685
2-6
6.48
576
4.87
6315
15.6
315
.35
1569
.647
20.
962
-0.0
17-0
.068
-0.0
16-0
.055
-0.0
060
lm01
27k1
3132
73.1
4424
-70.
1884
4.89
2616
16.0
815
.96
1830
.667
30.
893
-0.0
61-0
.141
-0.0
38-0
.065
0.00
20lm
0216
l165
9082
.684
7-6
8.97
782
4.94
3171
15.9
315
.76
2263
.773
10.
981
-0.0
050
-0.0
25-0
.007
0-0
.015
-0.0
010
lm01
92n2
6066
*79
.022
75-6
8.31
199
4.94
5660
115
.38
15.3
139
7.84
810.
992
-0.0
060
-0.0
180.
0010
-0.0
090
-0.0
010
lm03
26n1
7046
*79
.460
31-6
7.56
801
4.95
1432
17.2
917
.07
1266
.556
30.
984
-0.0
050
-0.0
27-0
.006
0-0
.014
0.00
20lm
0476
k561
082
.743
42-6
5.94
116
4.95
1673
16.2
016
.09
1615
.591
90.
897
-0.0
12-0
.125
-0.0
1-0
.034
0.00
50lm
0344
l127
7382
.669
9-6
7.19
545
4.95
2487
15.4
315
.23
2095
.913
90.
980.
0050
-0.0
36-0
.004
0-0
.023
0.00
20lm
0185
l237
7277
.783
12-6
8.63
659
4.97
0047
15.7
315
.55
496.
6719
0.97
6-0
.023
-0.0
190.
0020
0.00
20-0
.001
0lm
0015
m26
793
81.5
8538
-69.
8949
74.
9706
0416
.08
15.8
411
93.6
422
0.96
8-0
.036
-0.0
170.
0020
0.00
200.
0020
lm01
21m
1164
273
.601
62-6
9.11
359
4.99
5179
15.4
615
.31
1153
.564
80.
877
-0.0
88-0
.171
-0.0
49-0
.079
0.01
7lm
0343
n257
4583
.953
7-6
6.91
106
4.99
707
14.6
914
.42
459.
7833
0.85
6-0
.033
-0.1
52-0
.017
-0.0
410.
014
lm01
12k2
2638
74.2
2448
-69.
5668
84.
9992
0714
.56
14.4
424
48.9
162
0.90
60.
0090
-0.0
430.
011
-0.0
25-0
.011
lm04
27k1
3855
75.5
5629
-66.
0060
55.
0164
6915
.86
15.6
222
10.7
725
0.91
-0.0
38-0
.088
-0.0
080
-0.0
250.
0060
lm03
45k8
617
83.8
0798
-67.
0097
85.
0195
5916
.20
15.9
420
85.9
135
0.99
6-0
.012
-0.0
050
-0.0
030
-0.0
040
0.00
40lm
0585
n191
26*
83.1
9272
-71.
4120
65.
0213
9217
.37
17.1
720
85.9
098
0.98
4-0
.0-0
.047
-0.0
060
-0.0
420.
0010
lm05
51m
1387
0*76
.504
67-7
0.53
596
5.03
2362
16.2
715
.91
1477
.654
80.
981
-0.0
080
-0.0
35-0
.008
0-0
.032
0.00
10lm
0224
k244
8784
.354
33-6
8.50
835.
0490
9715
.93
15.7
622
79.5
966
1.00
2-0
.008
0-0
.021
-0.0
040
-0.0
1-0
.0lm
0011
k236
3381
.126
98-6
9.18
929
5.08
3128
16.3
216
.37
2174
.779
40.
879
-0.0
66-0
.154
-0.0
36-0
.068
0.00
40lm
0093
k308
0579
.186
72-6
9.56
374
5.08
5768
16.3
916
.34
1900
.745
50.
9-0
.076
-0.1
46-0
.04
-0.0
73-0
.007
0lm
0012
n221
5180
.395
73-6
9.68
261
5.11
1026
16.6
416
.33
1082
.854
60.
966
-0.0
18-0
.03
0.00
100.
0030
0.00
40lm
0540
m13
587
73.4
6764
-70.
5342
15.
1180
7516
.11
15.8
019
42.6
161
0.98
3-0
.006
0-0
.024
-0.0
030
-0.0
170.
0lm
0355
l461
985
.475
74-6
7.13
673
5.13
2899
15.7
015
.53
1845
.848
60.
976
-0.0
3-0
.019
0.00
100.
00.
0060
lm01
23k2
357
72.8
2093
-69.
4152
5.15
6041
16.3
316
.32
2303
.603
80.
899
-0.0
76-0
.137
-0.0
42-0
.08
0.00
80lm
0191
l255
8979
.647
54-6
7.98
489
5.15
9253
15.6
715
.58
1745
.871
20.
886
-0.0
25-0
.12
-0.0
11-0
.03
0.00
90lm
0021
l307
7083
.060
41-6
9.37
757
5.17
1793
15.5
815
.37
1082
.878
40.
965
-0.0
16-0
.013
-0.0
76-0
.026
-0.0
34lm
0701
m12
218
81.9
3523
-71.
9413
25.
1720
2316
.45
16.4
516
24.5
706
1.00
4-0
.011
-0.0
060
0.00
100.
0010
-0.0
070
lm02
16k9
627
82.6
0651
-68.
7694
85.
2031
0614
.13
13.9
518
23.8
298
0.98
4-0
.014
-0.0
21-0
.0-0
.002
0-0
.001
0lm
0024
k279
7481
.698
32-6
9.80
184
5.20
4477
15.4
415
.32
1582
.644
10.
983
-0.0
17-0
.014
0.0
0.00
100.
0060
lm00
52n1
9538
88.2
6495
-69.
6868
85.
2254
415
.58
15.3
823
47.6
571
0.96
4-0
.019
-0.0
420.
0020
-0.0
020
0.00
20lm
0111
m91
7575
.643
76-6
9.09
596
5.25
5775
15.3
914
.99
1865
.594
10.
995
-0.0
070
-0.0
4-0
.002
0-0
.034
0.00
20lm
0100
m12
334
76.3
8395
-69.
1299
15.
2629
1216
.19
16.0
346
8.79
930.
896
-0.0
77-0
.141
-0.0
36-0
.072
0.00
80lm
0033
k756
985
.206
26-6
9.44
349
5.26
9115
.30
15.1
622
25.7
022
0.98
9-0
.004
0-0
.011
-0.0
040
-0.0
020
0.00
30lm
0333
l154
0481
.899
71-6
6.84
652
5.27
222
15.5
515
.42
2202
.780
80.
955
-0.0
19-0
.042
0.00
100.
0020
0.00
40lm
0612
l101
9487
.801
68-7
1.02
961
5.27
9445
16.4
516
.33
1547
.766
10.
991
-0.0
23-0
.012
-0.0
010
0.00
20-0
.001
0lm
0330
k429
080
.971
98-6
6.27
295
5.28
192
16.5
716
.43
1089
.819
30.
907
-0.0
98-0
.136
-0.0
49-0
.085
-0.0
020
192
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0587
l185
0782
.383
94-7
1.78
632
5.28
2775
15.9
615
.80
383.
7489
0.91
3-0
.085
-0.1
33-0
.035
-0.0
77-0
.001
0lm
0223
l645
985
.372
76-6
8.18
986
5.29
9378
15.3
415
.20
845.
6984
0.92
2-0
.023
-0.0
74-0
.002
0-0
.008
00.
0080
lm01
16k2
1077
74.1
7121
-70.
2441
25.
3096
815
.40
15.1
922
50.5
707
0.97
2-0
.028
-0.0
28-0
.001
00.
0010
0.00
20lm
0207
k170
5981
.647
94-6
8.80
979
5.31
1128
16.2
216
.14
851.
7868
1.01
1-0
.064
-0.0
34-0
.027
-0.0
390.
0020
lm01
21n2
8673
73.6
5569
-69.
3697
45.
3272
8316
.05
15.9
416
10.5
479
0.89
5-0
.032
-0.1
18-0
.015
-0.0
360.
0090
lm00
20m
1635
982
.467
83-6
9.15
634
5.33
5197
14.9
914
.76
1794
.861
10.
933
-0.0
26-0
.105
-0.0
35-0
.053
-0.0
13lm
0224
m12
591*
84.9
7701
-68.
4286
75.
3449
314
.79
14.5
912
89.6
036
0.98
40.
0010
-0.0
32-0
.002
0-0
.029
-0.0
lm00
33m
6304
85.2
3578
-69.
4383
45.
3695
4515
.48
15.2
922
26.8
657
0.98
1-0
.006
0-0
.03
-0.0
050
-0.0
2-0
.001
0lm
0245
k709
5*89
.092
02-6
8.39
552
5.37
7706
16.8
616
.74
1773
.878
80.
978
-0.0
020
-0.0
35-0
.002
0-0
.01
0.00
10lm
0031
l229
8785
.196
81-6
9.34
126
5.41
3977
14.2
014
.06
1786
.789
00.
93-0
.007
0-0
.111
-0.0
050
-0.0
61-0
.001
0lm
0216
n105
8982
.753
61-6
8.92
483
5.44
858
14.8
414
.64
1255
.614
10.
977
-0.0
15-0
.026
-0.0
020
0.0
-0.0
020
lm00
92m
1877
478
.421
81-6
9.54
597
5.45
7309
15.7
315
.55
378.
7175
0.94
2-0
.008
0-0
.073
0.00
20-0
.048
0.00
40lm
0294
l138
1874
.125
05-6
7.19
756
5.47
1904
15.7
215
.55
1277
.498
10.
987
-0.0
1-0
.013
-0.0
010
0.00
100.
0010
lm01
14k2
1690
74.0
5789
-69.
8867
85.
5079
9515
.32
15.1
455
5.55
320.
947
0.00
30-0
.097
-0.0
28-0
.058
0.01
7lm
0223
k273
5385
.285
51-6
8.16
349
5.52
9928
16.2
016
.11
1191
.762
90.
991
-0.0
12-0
.006
0-0
.00.
0-0
.0lm
0186
m23
446
77.1
8403
-68.
8567
55.
5342
7416
.50
16.3
718
27.7
468
0.96
6-0
.026
-0.0
37-0
.003
0-0
.008
0-0
.002
0lm
0346
l134
3882
.817
42-6
7.54
852
5.57
0352
14.3
914
.16
837.
7814
0.91
-0.0
34-0
.078
-0.0
050
-0.0
10.
019
lm02
07n1
5251
81.9
3445
-68.
9611
55.
5988
4615
.47
15.2
012
52.5
839
0.99
-0.0
030
-0.0
13-0
.003
0-0
.008
00.
0lm
0093
k267
3279
.185
02-6
9.54
251
5.60
3447
15.8
815
.79
821.
7920
0.96
70.
0080
-0.0
590.
0020
-0.0
49-0
.008
0lm
0357
k240
43*
85.5
6601
-67.
4781
35.
6293
3616
.74
16.6
638
4.87
000.
922
-0.0
15-0
.085
-0.0
050
-0.0
160.
0070
lm00
24k1
6099
81.7
7809
-69.
7368
85.
6388
0615
.78
15.6
836
1.85
430.
926
-0.0
77-0
.105
-0.0
34-0
.063
-0.0
010
lm00
21k2
1280
82.7
5955
-69.
1804
55.
6718
4715
.60
15.6
516
28.5
730
0.94
9-0
.001
0-0
.051
-0.0
1-0
.016
-0.0
020
lm00
21m
2641
1*83
.246
68-6
9.20
468
5.70
8342
15.1
114
.95
1195
.705
70.
968
-0.0
010
-0.0
56-0
.001
0-0
.045
-0.0
010
lm01
85k1
5339
77.9
7996
-68.
4390
55.
7266
2716
.31
16.2
736
7.72
680.
898
-0.0
71-0
.133
-0.0
36-0
.062
0.00
50lm
0543
l281
5373
.870
45-7
1.11
878
5.73
6595
15.9
115
.88
556.
5493
0.97
9-0
.025
-0.0
160.
0010
-0.0
010
0.00
60lm
0127
l106
0873
.206
34-7
0.32
542
5.78
278
16.1
116
.00
1896
.734
90.
925
-0.0
13-0
.086
-0.0
020
-0.0
22-0
.001
0lm
0105
l584
276
.979
95-6
9.96
545.
7858
116
.12
16.0
022
30.8
260
0.97
60.
0020
-0.0
18-0
.048
0.00
300.
03lm
0091
n262
4779
.402
42-6
9.35
065.
8132
5615
.41
15.3
051
8.51
810.
983
-0.0
18-0
.013
0.0
0.0
0.00
30lm
0466
n117
1081
.642
73-6
6.13
484
5.82
2653
15.2
715
.05
1910
.725
80.
97-0
.016
-0.0
71-0
.015
-0.0
340.
0020
lm01
05l1
1377
*76
.822
83-7
0.01
872
5.83
6118
215
.37
15.1
914
16.8
380
0.98
3-0
.006
0-0
.022
-0.0
030
-0.0
060
0.0
lm00
13m
2077
681
.442
72-6
9.51
774
5.87
4426
16.2
916
.35
1114
.739
50.
942
-0.0
83-0
.095
-0.0
51-0
.065
0.00
10lm
0010
l242
4279
.898
64-6
9.36
666
5.94
1613
15.3
815
.20
1367
.872
70.
968
-0.0
12-0
.034
0.0
-0.0
010
0.00
40lm
0021
k148
3283
.109
98-6
9.13
885.
9732
4315
.36
15.1
641
1.80
040.
991
-0.0
040
-0.0
15-0
.007
0-0
.008
00.
0010
lm04
27n1
6272
*76
.031
68-6
6.18
205
6.00
374
15.2
414
.95
1208
.650
90.
963
-0.0
23-0
.042
0.00
100.
0-0
.003
0lm
0355
m22
531
85.6
2223
-67.
1003
96.
0534
5215
.49
15.3
318
45.8
486
0.98
2-0
.017
-0.0
1-0
.001
00.
0020
0.00
40lm
0220
l193
6884
.448
76-6
7.94
483
6.05
5055
16.0
715
.95
1560
.775
30.
935
-0.0
38-0
.076
-0.0
080
-0.0
16-0
.001
0lm
0171
n545
176
.178
42-6
7.84
531
6.06
5706
14.9
614
.77
1929
.635
90.
898
-0.0
54-0
.147
-0.0
36-0
.082
-0.0
010
lm03
56l1
5776
84.5
512
-67.
5715
6.07
2745
15.8
915
.79
809.
7491
0.98
7-0
.013
-0.0
080
0.00
200.
00.
0030
lm01
20k2
1262
*72
.106
59-6
9.19
104
6.12
7084
16.5
016
.42
1468
.577
80.
971
-0.0
050
-0.0
52-0
.006
0-0
.039
-0.0
lm02
11l6
920
83.3
0612
-67.
8407
26.
1912
116
.22
16.1
318
83.6
801
0.97
3-0
.018
-0.0
18-0
.0-0
.001
00.
0020
lm05
60n1
8929
77.5
3186
-70.
7122
16.
1926
9716
.23
16.0
220
28.5
055
0.97
9-0
.007
0-0
.024
-0.0
1-0
.016
-0.0
020
193
lm01
01k2
2147
76.8
8401
-69.
1909
36.
2082
4114
.74
14.5
314
42.7
940
0.97
4-0
.027
-0.0
26-0
.001
0-0
.001
00.
0030
lm00
20n6
294*
82.5
9216
-69.
2478
86.
2292
581
14.7
614
.42
875.
5657
0.95
50.
0050
-0.0
840.
0020
-0.0
72-0
.014
lm00
20n2
1732
*82
.663
34-6
9.33
662
6.27
1038
16.6
916
.52
596.
4752
0.98
90.
0010
-0.0
20.
0020
-0.0
140.
0010
lm05
64k2
1288
77.2
8653
-71.
2819
16.
3066
6315
.53
15.4
179
2.71
470.
89-0
.075
-0.1
42-0
.038
-0.0
640.
012
lm04
66n6
181
81.5
6648
-66.
0918
26.
3327
2315
.64
15.5
536
3.81
970.
91-0
.069
-0.1
1-0
.025
-0.0
470.
013
lm01
73n1
6894
76.4
0417
-68.
2482
16.
3479
4114
.97
14.7
053
8.54
950.
98-0
.002
0-0
.016
-0.0
150.
0010
-0.0
050
lm05
40k1
6892
*72
.737
25-7
0.56
097
6.37
983
16.6
016
.55
1117
.776
30.
982
-0.0
010
-0.0
3-0
.0-0
.013
-0.0
lm03
44k2
2660
82.6
3513
-67.
1089
76.
4348
2815
.04
14.8
411
93.6
830
0.96
9-0
.022
-0.0
270.
0010
0.00
10-0
.0lm
0124
k251
2672
.188
-69.
9129
36.
4383
5815
.64
15.5
886
4.68
420.
982
-0.0
16-0
.014
-0.0
010
0.00
10-0
.0lm
0303
k235
9976
.572
03-6
6.73
731
6.46
3085
15.5
915
.46
445.
7635
0.91
6-0
.041
-0.0
99-0
.013
-0.0
270.
0020
lm01
94n2
5484
79.0
1997
-68.
6558
26.
4734
6515
.36
15.2
210
98.6
948
0.95
3-0
.007
0-0
.053
-0.0
060
-0.0
220.
0070
lm00
90k1
5089
*78
.003
57-6
9.15
152
6.51
6940
116
.53
16.3
958
3.49
910.
987
-0.0
-0.0
290.
0030
-0.0
25-0
.003
0lm
0091
n319
44*
79.4
1439
-69.
3804
46.
5175
316
.79
16.7
572
7.87
060.
96-0
.012
-0.0
5-0
.006
0-0
.017
-0.0
lm03
46n1
7567
82.9
8578
-67.
5837
76.
5323
3214
.09
13.8
515
82.6
577
0.95
70.
0020
-0.0
52-0
.005
0-0
.018
-0.0
030
lm00
35m
2307
985
.593
5-6
9.88
483
6.56
9401
15.6
615
.50
862.
7340
0.96
1-0
.017
-0.0
410.
0020
0.00
10-0
.001
0lm
0690
k952
678
.102
79-7
1.90
847
6.59
6262
15.7
315
.50
508.
6562
0.97
7-0
.017
-0.0
21-0
.002
00.
0020
-0.0
010
lm04
57l1
3469
80.5
2857
-66.
1587
6.64
0871
15.1
714
.96
2263
.654
90.
905
-0.0
6-0
.131
-0.0
3-0
.069
-0.0
030
lm03
35n2
3069
82.4
8431
-67.
2425
6.89
8566
16.2
616
.07
1768
.846
80.
973
-0.0
43-0
.03
-0.0
020
-0.0
040
-0.0
020
lm01
80m
2716
4*77
.519
15-6
7.81
345
6.91
3797
915
.45
15.1
022
94.6
680
0.98
2-0
.008
0-0
.028
0.00
10-0
.018
0.00
30lm
0364
k127
5186
.121
86-6
7.04
148
6.97
7975
15.9
215
.78
705.
8406
0.95
3-0
.048
-0.0
41-0
.006
0-0
.009
00.
0050
lm02
94l4
906*
73.8
4732
-67.
1382
77.
0961
5415
.37
15.1
717
82.7
369
0.98
90.
0-0
.013
-0.0
010
-0.0
060
0.00
10lm
0335
n254
77*
82.2
8467
-67.
2884
17.
1173
239
14.9
314
.70
1834
.767
70.
91-0
.003
0-0
.093
-0.0
030
-0.0
210.
0020
lm02
14n1
4689
*82
.893
89-6
8.59
669
7.15
0098
15.0
715
.16
2270
.650
90.
991
-0.0
030
-0.0
090
-0.0
150.
0010
0.00
30lm
0367
m14
504*
87.6
0799
-67.
4051
7.17
7252
16.9
016
.79
2338
.653
30.
995
0.00
10-0
.017
0.00
100.
0-0
.0lm
0427
n121
2275
.865
53-6
6.14
977
7.19
4033
15.7
315
.45
1942
.626
50.
984
-0.0
080
-0.0
22-0
.03
-0.0
-0.0
12lm
0241
n189
6089
.434
26-6
7.93
432
7.22
7958
15.8
715
.72
402.
6331
0.97
8-0
.033
-0.0
220.
0010
0.00
10-0
.002
0lm
0246
k659
588
.145
96-6
8.74
102
7.28
4157
15.6
015
.50
2028
.543
90.
942
-0.0
78-0
.092
-0.0
29-0
.049
-0.0
020
lm00
93k5
253*
78.9
7127
-69.
4327
17.
2843
8815
.71
15.7
418
35.7
526
0.92
5-0
.039
-0.1
36-0
.02
-0.0
47-0
.002
0lm
0585
l584
282
.782
41-7
1.33
556
7.28
6296
14.9
514
.74
1102
.783
20.
967
-0.0
16-0
.026
0.0
-0.0
0.00
80lm
0033
m20
529
85.4
7251
-69.
5225
17.
4647
7814
.26
14.0
718
18.8
043
0.96
2-0
.002
0-0
.052
-0.0
030
-0.0
240.
0050
lm00
14k7
299
80.1
7669
-69.
7988
47.
5367
4715
.88
15.7
922
59.5
285
0.97
4-0
.022
-0.0
240.
00.
0010
0.00
10lm
0427
k750
5*75
.427
66-6
5.95
939
7.68
4446
15.4
015
.15
2192
.695
30.
981
-0.0
060
-0.0
15-0
.03
-0.0
010
-0.0
090
lm04
35m
1238
177
.556
51-6
5.62
774
7.69
6551
16.0
415
.88
1886
.625
80.
89-0
.018
-0.1
380.
0060
-0.0
490.
018
lm01
80n9
316
77.1
2842
-67.
9297
17.
7540
9615
.40
15.2
215
89.6
684
0.97
2-0
.029
-0.0
280.
0010
0.00
20-0
.0lm
0356
m11
102
84.7
4967
-67.
3777
77.
7883
515
.73
15.6
620
53.5
103
0.99
-0.0
26-0
.011
0.00
100.
0010
-0.0
030
lm00
33n1
2413
85.2
6999
-69.
6302
67.
9421
2615
.02
14.9
231
5.89
580.
974
0.00
70-0
.051
-0.0
1-0
.029
-0.0
11lm
0326
n774
379
.816
72-6
7.49
871
8.01
5506
15.6
915
.55
1896
.759
30.
929
-0.0
38-0
.116
-0.0
28-0
.046
0.00
50lm
0156
m35
36*
71.6
5461
-68.
8327
28.
2780
8616
.51
16.5
121
55.7
386
0.90
9-0
.013
-0.1
29-0
.006
0-0
.054
0.00
50lm
0157
m46
89*
72.5
8175
-68.
7322
98.
4029
4616
.44
16.4
041
1.71
140.
972
0.00
10-0
.021
-0.0
020
-0.0
060
-0.0
010
lm03
54n1
6185
*84
.837
11-6
7.21
527
8.45
8416
.06
15.9
514
97.7
810
0.97
2-0
.003
0-0
.03
-0.0
080
-0.0
2-0
.002
0lm
0020
k102
8781
.940
49-6
9.12
858.
4630
3914
.74
14.5
615
66.6
321
0.92
3-0
.032
-0.1
01-0
.021
-0.0
440.
0010
194
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0467
k119
17*
82.0
9084
-65.
9874
8.46
4606
315
.03
14.8
115
38.6
456
0.98
3-0
.005
0-0
.017
-0.0
050
-0.0
090
0.00
10lm
0024
m14
9882
.299
74-6
9.76
834
8.48
5941
15.0
714
.98
1447
.826
30.
915
-0.0
9-0
.145
-0.0
53-0
.099
0.00
30lm
0033
m59
6085
.302
16-6
9.43
568
8.58
3074
13.8
313
.63
2263
.784
60.
984
-0.0
030
-0.0
2-0
.017
-0.0
030
0.00
60lm
0356
l214
8684
.357
04-6
7.61
704
8.81
6562
15.6
915
.54
1657
.533
70.
887
-0.0
25-0
.122
-0.0
12-0
.035
0.01
4lm
0541
l927
5*73
.900
85-7
0.67
855
8.85
0098
16.5
516
.45
1926
.658
40.
980.
0010
-0.0
210.
0-0
.008
00.
0lm
0173
m17
717
76.5
4398
-68.
0953
18.
8565
3713
.59
13.3
919
18.6
627
0.97
6-0
.004
0-0
.027
-0.0
15-0
.007
00.
0030
lm01
91n3
246*
80.1
2526
-67.
8465
514
.645
028
15.4
515
.39
1150
.656
60.
986
-0.0
010
-0.0
17-0
.001
0-0
.003
00.
0010
lm01
73n3
2162
*76
.486
71-6
8.33
424
21.0
4149
214
.93
15.1
175
9.84
320.
957
-0.0
090
-0.0
86-0
.011
-0.0
16-0
.01
Tabl
eA
.1:
Iden
tifica
tion,
mai
npr
oper
ties
and
Four
ier
para
met
ers
for
1768
HEB
sin
the
LMC
(Col
umn
1:ER
OS-
2id
entifi
catio
nof
the
star
;C
olum
n2:
Rig
htas
cens
ion
from
the
ERO
S-2
cata
logu
e;C
olum
n3:
Dec
linat
ion
from
the
ERO
S-2
cata
logu
e;C
olum
n4:
Perio
d(∗
-Sta
rsfo
rwhi
cha
new
perio
dw
asde
rived
inth
isst
udy.
See
text
fort
hede
tails
.);C
olum
n5:
Mea
nm
agni
tude
inth
eR
EROS
pass
band
;Col
umn
6:M
ean
mag
nitu
dein
the
BEROS
pass
band
;C
olum
n7:
Epoc
hof
the
prim
ary
min
imum
;C
olum
n8-
Col
umn
14:
Four
ierp
aram
eter
sof
the
light
curv
es).
195
ERO
S-2
idV
MC
idPe
riod
Ks,m
ax
REROS,m
ax
(day
)(m
ag)
(mag
)lm
0323
n205
46V
MC
J052
140.
98-6
6522
7.93
0.90
0708
17.1
1617
.057
lm03
44m
2651
0V
MC
J053
208.
76-6
7074
1.80
0.91
2445
17.2
6017
.161
lm00
23n1
1843
VM
CJ0
5331
9.72
-693
719.
700.
9125
6817
.314
17.1
43lm
0030
n213
91V
MC
J053
717.
63-6
9225
4.37
0.92
2672
16.7
5416
.644
lm02
26n2
0767
VM
CJ0
5382
5.02
-690
004.
550.
9239
4117
.497
17.5
60lm
0231
k906
3V
MC
J054
830.
84-6
7422
3.25
0.92
7999
16.9
9216
.883
lm02
14n1
0459
VM
CJ0
5312
7.29
-683
413.
650.
9389
7117
.652
17.6
35lm
0171
m16
733*
VM
CJ0
5044
4.08
-674
447.
890.
9390
0115
.982
15.7
48lm
0127
k121
34V
MC
J045
304.
25-7
0105
1.19
0.93
9454
16.7
0017
.384
lm03
42k1
8196
VM
CJ0
5313
4.88
-664
500.
100.
9414
4717
.195
16.9
15lm
0346
l149
81V
MC
J053
111.
35-6
7333
9.52
0.94
1548
16.3
7017
.043
lm04
66k2
3468
VM
CJ0
5253
6.95
-660
416.
630.
9430
3217
.170
17.0
85lm
0436
n210
36V
MC
J050
715.
90-6
6121
6.34
0.94
4593
17.1
9617
.059
lm02
17m
1920
8V
MC
J053
621.
59-6
8492
9.14
0.95
4486
16.0
9316
.951
lm00
30n1
9548
VM
CJ0
5375
2.94
-692
013.
540.
9552
6116
.975
16.9
24lm
0090
n162
43V
MC
J051
340.
27-6
9182
1.72
0.95
6439
16.7
7716
.634
lm03
40m
1585
2V
MC
J053
216.
72-6
6212
0.52
0.95
8465
17.3
8117
.349
lm00
15k6
383
VM
CJ0
5234
4.20
-694
735.
210.
9641
5917
.116
16.7
80lm
0542
k204
54V
MC
J045
137.
03-7
0575
2.57
0.96
5838
17.3
3517
.277
lm00
34k1
0238
VM
CJ0
5351
1.80
-694
913.
600.
9689
8816
.425
17.0
19lm
0355
n118
66V
MC
J054
408.
49-6
7104
2.57
0.96
9348
17.2
9217
.052
lm00
93k1
6356
VM
CJ0
5162
3.46
-692
920.
820.
9771
8616
.810
16.7
06lm
0321
l271
58V
MC
J052
054.
57-6
6343
4.22
0.97
7509
17.1
0417
.065
lm02
23n2
6953
VM
CJ0
5424
4.88
-681
844.
650.
9790
3417
.558
17.6
62lm
0023
k200
21V
MC
J053
227.
77-6
9303
7.28
1.01
1662
17.1
2816
.700
lm00
33m
1042
9V
MC
J054
125.
68-6
9274
5.13
1.01
9232
17.7
7417
.693
lm01
17l9
906
VM
CJ0
5001
1.97
-701
923.
121.
0200
3417
.152
17.1
05lm
0030
n226
49V
MC
J053
721.
60-6
9212
8.37
1.02
6528
16.5
3216
.624
lm00
25n1
7091
VM
CJ0
5341
4.41
-695
957.
921.
0280
8616
.682
17.3
15lm
0091
m27
064
VM
CJ0
5171
8.22
-691
213.
891.
0412
1417
.253
16.7
55lm
0093
n503
2V
MC
J051
820.
70-6
9345
4.13
1.04
2603
16.6
3416
.539
lm01
73m
9757
VM
CJ0
5045
5.74
-680
305.
151.
0468
816
.610
16.6
80lm
0424
n145
61V
MC
J045
939.
22-6
5481
9.86
1.04
7235
16.8
5316
.677
lm04
93n1
8692
VM
CJ0
5490
7.59
-652
842.
801.
0509
3116
.819
17.4
88lm
0031
m96
51V
MC
J054
224.
86-6
9061
0.38
1.05
1009
16.4
0816
.838
lm00
11l5
712
VM
CJ0
5234
9.29
-691
422.
121.
0512
3816
.539
16.6
07lm
0244
k107
48V
MC
J055
158.
84-6
8251
8.50
1.05
1608
17.5
0917
.600
lm05
40l1
5552
VM
CJ0
4513
9.44
-704
222.
551.
0521
6517
.312
17.4
74lm
0020
l855
3V
MC
J052
721.
55-6
9155
1.08
1.05
4358
17.1
0316
.790
196
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0367
n188
05V
MC
J054
943.
82-6
7360
2.65
1.05
5955
17.5
7617
.578
lm01
84n1
4844
VM
CJ0
5083
4.41
-683
535.
521.
0673
8616
.868
16.9
03lm
0570
m20
301
VM
CJ0
5190
7.13
-703
420.
271.
0702
1616
.315
16.1
09lm
0336
l212
94V
MC
J052
426.
44-6
7355
7.02
1.07
0847
17.8
7917
.697
lm03
34l2
0690
VM
CJ0
5233
0.93
-671
420.
321.
0713
3316
.975
16.9
20lm
0116
m17
752
VM
CJ0
4571
6.76
-701
251.
261.
0719
3216
.860
16.6
84lm
0335
l168
08V
MC
J052
714.
45-6
7124
1.07
1.07
3703
16.3
7716
.092
lm03
37k1
6442
VM
CJ0
5271
4.12
-672
502.
961.
0740
517
.683
17.5
26lm
0295
l193
34V
MC
J045
943.
51-6
7130
9.04
1.07
4702
17.0
5016
.855
lm02
07n1
9761
VM
CJ0
5285
5.52
-685
929.
931.
0748
9717
.305
17.0
66lm
0335
n642
2V
MC
J052
954.
30-6
7081
9.99
1.07
6161
17.3
6117
.193
lm01
84k2
0015
VM
CJ0
5070
9.23
-682
830.
381.
0797
4117
.332
17.3
28lm
0040
k162
25V
MC
J054
335.
85-6
9093
2.27
1.08
7516
17.3
4717
.281
lm03
74n6
047
VM
CJ0
5531
8.81
-670
841.
541.
0906
7717
.550
17.4
90lm
0301
m26
336
VM
CJ0
5073
0.31
-662
441.
931.
0907
8217
.581
17.6
22lm
0425
n260
27V
MC
J050
257.
84-6
5524
3.78
1.09
0849
17.7
1817
.760
lm05
84l1
1571
VM
CJ0
5264
3.38
-712
231.
691.
0919
8917
.231
17.6
32lm
0466
m12
019
VM
CJ0
5270
1.89
-655
854.
051.
0925
3716
.964
16.9
77lm
0207
l996
5V
MC
J052
651.
53-6
8552
9.03
1.09
4904
16.9
3316
.739
lm02
07l1
1656
VM
CJ0
5262
4.11
-685
614.
691.
0954
1917
.498
17.6
08lm
0093
n123
50V
MC
J051
847.
36-6
9370
5.07
1.10
0478
18.4
0717
.412
lm05
50k1
3137
VM
CJ0
5010
9.34
-703
227.
411.
1030
216
.570
16.9
97lm
0366
k174
09V
MC
J054
412.
68-6
7253
7.21
1.10
5186
16.3
3016
.498
lm03
64l1
3690
VM
CJ0
5445
1.36
-671
217.
701.
1056
1717
.282
17.0
56lm
0346
l811
1V
MC
J053
107.
21-6
7302
3.70
1.11
2761
17.4
1717
.115
lm02
43l1
6058
VM
CJ0
5551
5.72
-681
548.
491.
1128
0717
.310
17.4
21lm
0232
l172
59V
MC
J054
515.
80-6
8162
6.21
1.12
0751
17.2
7117
.205
lm04
57k1
8380
VM
CJ0
5222
6.94
-660
141.
911.
1273
4717
.341
17.3
57lm
0172
l662
6V
MC
J050
054.
84-6
8141
4.07
1.13
021
17.1
3216
.869
lm03
10k1
5114
VM
CJ0
5100
6.33
-662
105.
591.
1329
1817
.648
17.6
31lm
0325
l272
85V
MC
J052
041.
48-6
7162
5.15
1.13
5758
16.5
6316
.402
lm00
10k1
5429
VM
CJ0
5190
5.15
-690
917.
931.
1369
3116
.852
16.5
85lm
0556
m19
867
VM
CJ0
5031
0.90
-713
801.
601.
1395
2717
.425
17.4
69lm
0214
n961
6V
MC
J053
143.
12-6
8335
4.22
1.14
3016
17.1
7517
.346
lm02
45k7
908
VM
CJ0
5552
3.86
-682
408.
621.
1434
6717
.459
17.4
26lm
0455
l556
7V
MC
J052
215.
63-6
5441
6.74
1.14
3775
16.6
4716
.352
lm02
17n1
4277
*V
MC
J053
610.
78-6
8572
6.49
1.14
7572
16.3
2716
.312
lm04
67m
6802
VM
CJ0
5301
9.84
-655
639.
461.
1478
0216
.211
16.0
33lm
0571
l244
63V
MC
J052
213.
31-7
0443
9.71
1.14
8628
17.6
0317
.538
lm00
31n1
7224
VM
CJ0
5420
5.62
-692
226.
651.
1489
316
.641
16.3
18lm
0033
m26
708
VM
CJ0
5412
5.66
-693
338.
541.
1582
8417
.164
17.0
41
197
lm05
75n1
1053
VM
CJ0
5232
2.45
-712
622.
631.
1601
617
.267
17.2
16lm
0014
l200
54V
MC
J052
019.
46-7
0015
6.85
1.16
0262
17.8
2917
.524
lm04
66l1
9242
VM
CJ0
5253
8.13
-661
143.
481.
1635
8917
.652
17.4
87lm
0535
n112
77V
MC
J044
942.
73-7
1282
2.25
1.16
8449
16.7
6716
.958
lm01
03l1
3951
VM
CJ0
5085
1.76
-693
748.
691.
1745
0716
.745
16.5
44lm
0226
n241
68V
MC
J053
839.
17-6
9014
0.79
1.17
6008
16.2
7316
.196
lm04
57l1
9060
VM
CJ0
5211
3.24
-661
252.
391.
1761
0817
.248
17.3
01lm
0214
m29
033
VM
CJ0
5312
2.05
-683
134.
081.
1786
6316
.065
16.4
22lm
0540
l224
24V
MC
J045
123.
99-7
0453
6.93
1.18
1881
16.8
4516
.945
lm03
03l2
3428
VM
CJ0
5071
2.25
-665
310.
231.
1836
6917
.587
17.5
10lm
0021
k228
31V
MC
J053
134.
92-6
9112
1.79
1.18
4539
16.7
4216
.755
lm02
01k1
0778
VM
CJ0
5262
1.83
-674
226.
981.
1875
9616
.769
17.5
53lm
0312
k155
23V
MC
J050
955.
28-6
6435
5.14
1.18
8117
17.2
9217
.443
lm01
14m
2789
9V
MC
J045
712.
52-6
9544
3.81
1.19
1167
16.9
2216
.774
lm02
00k1
9885
VM
CJ0
5214
2.45
-674
951.
211.
1914
8317
.020
17.2
05lm
0366
k104
36V
MC
J054
457.
24-6
7222
9.27
1.19
3346
16.6
9516
.447
lm00
44k3
974
VM
CJ0
5442
8.89
-694
644.
071.
1936
816
.255
16.1
33lm
0344
m18
50V
MC
J053
215.
41-6
6580
3.46
1.19
3709
16.5
5416
.219
lm02
14n2
5393
VM
CJ0
5311
1.12
-683
947.
011.
2055
0516
.994
17.3
35lm
0115
n144
63V
MC
J050
256.
10-6
9585
4.83
1.20
6817
.187
16.9
52lm
0373
m20
395
VM
CJ0
5571
1.53
-664
418.
591.
2076
7217
.585
17.7
80lm
0230
m92
59V
MC
J054
543.
42-6
7424
7.82
1.20
7767
17.2
9017
.471
lm01
93n5
944
VM
CJ0
5210
1.69
-681
058.
621.
2077
7517
.370
17.3
14lm
0540
k226
86V
MC
J045
150.
15-7
0360
8.59
1.21
0708
17.8
0617
.667
lm03
02n1
2595
VM
CJ0
5051
8.64
-664
956.
271.
2131
5117
.168
17.0
91lm
0030
n681
5V
MC
J053
752.
89-6
9234
9.91
1.21
3239
16.3
7616
.212
lm02
55m
2113
2V
MC
J060
440.
97-6
8305
7.48
1.21
3994
17.6
0017
.565
lm00
33l8
069
VM
CJ0
5395
5.35
-693
606.
141.
2150
3916
.603
16.6
92lm
0423
m21
313
VM
CJ0
5030
6.73
-652
030.
781.
2157
417
.503
17.2
27lm
0240
l139
40V
MC
J055
157.
14-6
7535
1.67
1.22
005
17.2
4917
.318
lm05
52n2
8102
VM
CJ0
5013
8.11
-710
745.
891.
2248
8217
.587
17.4
68lm
0025
l199
40V
MC
J053
232.
13-7
0005
6.63
1.22
5202
17.3
6817
.387
lm03
46l1
3640
VM
CJ0
5301
5.09
-673
259.
821.
2253
1616
.563
16.3
62lm
0200
l205
61V
MC
J052
200.
96-6
7564
3.02
1.22
5852
16.2
1415
.884
lm01
84n2
2563
VM
CJ0
5084
1.72
-683
809.
041.
2264
7517
.163
17.2
79lm
0304
n298
42V
MC
J050
439.
61-6
7172
7.85
1.22
9024
16.7
2016
.475
lm00
90m
2646
6V
MC
J051
432.
59-6
9122
6.75
1.23
2396
17.0
9216
.816
lm03
36m
2147
0V
MC
J052
622.
67-6
7264
4.90
1.23
6096
17.5
2717
.393
lm03
44l5
959
VM
CJ0
5302
8.46
-670
858.
591.
2400
5717
.045
17.1
79lm
0090
m13
647
VM
CJ0
5130
8.32
-690
801.
681.
2405
3216
.511
16.5
23lm
0175
m17
458
VM
CJ0
5060
8.86
-682
652.
631.
2448
9716
.650
16.3
37
198
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0303
n105
23V
MC
J050
848.
42-6
6482
5.91
1.24
6321
17.5
5017
.673
lm03
42n2
4002
VM
CJ0
5315
8.91
-665
526.
331.
2484
717
.472
17.4
09lm
0304
n249
21V
MC
J050
357.
90-6
7153
8.31
1.24
9985
16.6
9716
.477
lm02
14n7
884
VM
CJ0
5311
2.15
-683
316.
021.
2503
0517
.020
16.9
25lm
0044
l247
15V
MC
J054
356.
05-7
0034
3.04
1.25
1463
17.3
9317
.590
lm00
20m
1400
7V
MC
J052
946.
13-6
9082
8.40
1.25
6518
15.7
8116
.643
lm01
82l1
3191
VM
CJ0
5075
6.93
-681
406.
121.
2565
2317
.041
16.8
96lm
0325
m15
768
VM
CJ0
5230
0.57
-670
238.
001.
2605
5116
.881
16.7
70lm
0671
l505
6V
MC
J045
819.
25-7
2072
7.05
1.27
1916
17.5
8017
.682
lm04
36k8
952
VM
CJ0
5052
7.83
-655
803.
421.
2755
9617
.600
17.7
25lm
0214
m29
858
VM
CJ0
5311
0.13
-683
153.
591.
2792
1817
.294
17.2
98lm
0583
m25
712
VM
CJ0
5314
4.06
-705
623.
791.
2804
2316
.441
16.9
34lm
0012
m20
602
VM
CJ0
5223
3.82
-693
255.
681.
2841
0116
.667
17.2
89lm
0197
n195
34V
MC
J052
043.
69-6
8592
3.38
1.28
4845
17.2
0917
.331
lm00
17m
1788
3V
MC
J052
701.
41-7
0125
2.43
1.28
9967
15.9
1516
.975
lm02
93l1
4089
VM
CJ0
4595
9.15
-665
005.
451.
2920
417
.617
17.6
42lm
0030
k663
4V
MC
J053
607.
01-6
9055
4.27
1.29
3848
15.9
0415
.966
lm03
66k1
9655
VM
CJ0
5443
4.04
-672
637.
091.
2954
7116
.897
16.7
91lm
0184
k112
57V
MC
J050
750.
94-6
8252
4.40
1.29
7875
17.0
6416
.852
lm02
07l9
702
VM
CJ0
5263
0.11
-685
524.
081.
3027
5315
.797
16.3
19lm
0200
l209
52V
MC
J052
204.
85-6
7565
4.07
1.30
4803
16.3
6616
.250
lm00
33k1
6643
VM
CJ0
5392
0.50
-693
006.
881.
3057
4315
.700
15.6
71lm
0033
k283
57V
MC
J053
941.
71-6
9342
4.83
1.30
6841
15.6
8415
.661
lm03
44k4
525
VM
CJ0
5311
2.67
-665
909.
151.
3108
0416
.848
16.6
12lm
0323
l773
8V
MC
J052
102.
34-6
6474
9.90
1.31
5224
16.9
1216
.910
lm03
21m
1335
8V
MC
J052
123.
12-6
6194
5.79
1.31
821
17.1
9217
.273
lm05
51k1
9078
VM
CJ0
5040
3.86
-703
547.
381.
3188
8217
.501
17.2
09lm
0466
m23
585
VM
CJ0
5254
7.02
-660
437.
181.
3189
5816
.578
16.5
76lm
0340
n223
83V
MC
J053
222.
31-6
6330
9.62
1.31
9689
17.6
7317
.616
lm03
66n1
4593
VM
CJ0
5473
5.62
-673
323.
511.
3213
3717
.842
17.6
93lm
0032
k203
13V
MC
J053
634.
89-6
9334
9.73
1.32
3792
16.6
8116
.990
lm00
12l1
7935
VM
CJ0
5195
1.14
-694
002.
581.
3239
8416
.143
16.3
14lm
0033
m68
50V
MC
J054
129.
05-6
9262
6.67
1.32
799
17.1
6817
.058
lm03
30l1
8021
VM
CJ0
5241
9.71
-663
140.
411.
3300
1116
.530
16.4
47lm
0210
k244
51V
MC
J052
920.
91-6
7491
7.62
1.33
7468
16.7
6216
.565
lm05
87n1
9385
VM
CJ0
5314
3.62
-714
716.
421.
3395
0916
.050
16.6
05lm
0056
n227
35V
MC
J055
425.
98-7
0243
4.41
1.34
1028
16.9
9216
.802
lm00
12l1
9396
VM
CJ0
5204
2.63
-694
032.
821.
3420
0116
.545
16.3
24lm
0045
n274
51V
MC
J054
956.
22-7
0034
1.04
1.34
273
16.3
9316
.104
lm01
25m
1744
7V
MC
J045
457.
57-6
9504
9.69
1.34
3061
17.2
8717
.580
lm00
32m
1907
9V
MC
J053
656.
06-6
9330
8.54
1.34
4214
16.5
5716
.284
199
lm00
90k1
5522
VM
CJ0
5112
0.53
-690
915.
241.
3452
3915
.618
16.8
17lm
0091
l131
41V
MC
J051
644.
35-6
9164
1.14
1.34
7207
16.4
7416
.586
lm00
40k2
5840
VM
CJ0
5433
2.02
-691
340.
551.
3528
1917
.495
17.5
27lm
0095
n217
86V
MC
J051
726.
24-7
0012
7.78
1.35
5226
17.2
5217
.009
lm00
33l1
2538
VM
CJ0
5404
3.71
-693
742.
601.
3562
6116
.456
16.9
32lm
0020
m26
75V
MC
J052
939.
57-6
9040
9.01
1.35
6457
17.0
7316
.855
lm05
41n1
0909
VM
CJ0
4573
9.17
-704
139.
451.
3578
1817
.792
17.7
00lm
0033
l204
81V
MC
J054
028.
88-6
9403
8.49
1.35
9961
16.6
6516
.988
lm02
25m
4465
VM
CJ0
5434
3.80
-682
229.
251.
3606
3416
.321
16.2
43lm
0325
k818
4V
MC
J052
039.
10-6
7000
6.14
1.36
1238
16.3
1216
.152
lm03
06m
1121
8V
MC
J050
438.
55-6
7220
9.43
1.36
289
16.9
3516
.811
lm03
31n1
1495
VM
CJ0
5292
1.37
-663
345.
531.
3631
6515
.899
15.5
78lm
0055
m20
627
VM
CJ0
5575
4.45
-695
256.
641.
3653
1217
.322
17.3
50lm
0610
k122
8V
MC
J055
210.
93-7
0292
4.54
1.36
879
17.0
3217
.379
lm02
16l7
335
VM
CJ0
5303
1.40
-685
436.
111.
3703
6717
.322
17.2
27lm
0331
l129
91V
MC
J052
647.
95-6
6291
3.64
1.37
0492
17.4
1917
.302
lm05
87k6
387
VM
CJ0
5293
6.28
-713
235.
421.
3722
4917
.065
16.9
36lm
0584
k140
35V
MC
J052
515.
64-7
1140
8.45
1.37
2777
16.3
8716
.326
lm04
26m
6757
VM
CJ0
5002
6.30
-655
633.
631.
3727
8516
.716
16.5
30lm
0194
l205
12V
MC
J051
413.
51-6
8380
0.65
1.37
3732
17.0
8416
.806
lm00
31n1
2282
VM
CJ0
5410
2.99
-692
257.
921.
3751
9616
.183
15.9
35lm
0575
n394
7V
MC
J052
251.
87-7
1212
3.87
1.37
5523
16.5
3316
.188
lm01
86n2
5699
VM
CJ0
5095
1.73
-690
204.
061.
3767
8716
.632
16.7
33lm
0601
l272
34V
MC
J054
650.
69-7
0454
9.22
1.37
8285
17.5
7317
.545
lm00
10n9
981
VM
CJ0
5223
2.91
-691
615.
751.
3790
9816
.694
16.5
94lm
0010
k356
3V
MC
J051
933.
33-6
9043
7.18
1.38
0453
16.9
8917
.031
lm01
61l2
2253
VM
CJ0
4563
3.71
-675
601.
331.
3806
8417
.113
17.0
60lm
0033
k164
25V
MC
J053
914.
93-6
9300
2.10
1.38
1841
15.5
8215
.813
lm01
87k2
5395
VM
CJ0
5111
4.93
-685
136.
091.
3844
7615
.549
16.7
40lm
0033
l898
2V
MC
J054
038.
40-6
9362
2.56
1.38
4664
17.4
2817
.215
lm03
37k2
4187
VM
CJ0
5270
9.25
-672
817.
381.
3972
2716
.701
16.5
45lm
0217
n123
76V
MC
J053
551.
97-6
8563
4.41
1.39
8198
16.5
0416
.326
lm01
27l2
0498
VM
CJ0
4525
2.28
-702
354.
701.
3985
3816
.717
16.6
86lm
0040
l120
70V
MC
J054
401.
24-6
9165
6.11
1.39
9558
16.2
4916
.703
lm05
97l1
9272
VM
CJ0
5390
7.04
-714
720.
391.
4024
5515
.955
15.8
22lm
0200
k210
51V
MC
J052
214.
89-6
7471
6.67
1.40
3365
17.8
4517
.654
lm04
57k2
4395
VM
CJ0
5210
9.04
-660
423.
061.
4067
117
.511
17.6
47lm
0306
l186
59V
MC
J050
320.
07-6
7344
4.75
1.40
7038
17.5
7217
.512
lm04
33m
7146
VM
CJ0
5095
6.35
-651
412.
851.
4136
4615
.385
16.2
25lm
0332
l249
89V
MC
J052
344.
17-6
6552
2.22
1.41
5919
17.5
9617
.426
lm03
32n2
1956
VM
CJ0
5255
8.72
-665
357.
581.
4162
6417
.047
16.9
44
200
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0226
k213
75V
MC
J053
725.
81-6
8514
0.49
1.41
8055
17.4
2317
.401
lm00
33m
1474
6V
MC
J054
115.
56-6
9291
9.24
1.42
0343
15.7
0815
.632
lm01
86n6
732
VM
CJ0
5095
1.23
-685
411.
921.
4204
3316
.113
16.1
22lm
0331
k223
19V
MC
J052
711.
08-6
6234
7.02
1.42
1485
16.2
3116
.034
lm04
27k7
569
VM
CJ0
5015
6.00
-655
734.
941.
4235
2616
.515
16.3
92lm
0090
l782
1V
MC
J051
253.
37-6
9152
9.98
1.42
5433
17.4
9317
.180
lm00
21n5
140
VM
CJ0
5340
2.01
-691
347.
181.
4292
8715
.900
15.9
45lm
0467
l111
96V
MC
J052
833.
77-6
6084
4.17
1.42
9906
16.5
0716
.287
lm00
30m
9744
VM
CJ0
5375
2.85
-690
945.
801.
4347
3815
.812
16.1
42lm
0216
m68
05V
MC
J053
051.
59-6
8444
3.33
1.43
6319
16.2
1216
.068
lm03
36n6
255
VM
CJ0
5260
4.45
-672
915.
151.
4380
0816
.188
16.2
30lm
0030
n526
6V
MC
J053
708.
54-6
9142
7.21
1.43
8845
15.9
1316
.142
lm03
27m
2371
7V
MC
J052
207.
69-6
7272
5.27
1.43
9496
16.0
3415
.954
lm00
30n1
9275
VM
CJ0
5374
1.57
-692
007.
661.
4415
0217
.476
17.5
78lm
0101
l489
8V
MC
J050
710.
82-6
9141
1.34
1.44
7797
17.1
6417
.072
lm01
05l4
144
VM
CJ0
5074
0.85
-695
658.
021.
4480
816
.157
15.9
18lm
0023
m46
35*
VM
CJ0
5342
9.30
-692
530.
241.
4503
3416
.983
16.8
71lm
0030
k139
20V
MC
J053
613.
98-6
9091
1.12
1.45
0827
15.6
0416
.053
lm00
40k2
5978
VM
CJ0
5435
6.21
-691
331.
321.
4512
1516
.289
16.2
35lm
0440
l719
2V
MC
J051
140.
79-6
5064
9.80
1.45
3087
17.5
0517
.525
lm03
37k1
9646
VM
CJ0
5275
5.58
-672
619.
021.
4539
2117
.518
17.4
90lm
0095
m18
525
VM
CJ0
5174
3.89
-695
109.
361.
4549
4116
.437
16.9
96lm
0090
k113
33V
MC
J051
156.
28-6
9074
2.90
1.45
6551
16.5
8717
.136
lm03
35m
2318
4V
MC
J052
858.
68-6
7052
9.33
1.45
7715
16.7
7016
.521
lm06
05n2
3731
VM
CJ0
5501
7.48
-712
635.
541.
4581
4915
.959
16.9
04lm
0021
l146
50V
MC
J053
247.
63-6
9171
7.60
1.46
2272
15.7
5815
.511
lm03
44m
2008
6V
MC
J053
207.
14-6
7051
4.52
1.46
2707
17.3
7717
.157
lm00
34k9
201
VM
CJ0
5363
4.21
-694
851.
861.
4639
0216
.764
16.4
55lm
0335
k268
31V
MC
J052
648.
70-6
7070
3.57
1.46
4774
17.5
6317
.317
lm00
33k9
023
VM
CJ0
5400
6.19
-692
712.
401.
4699
7616
.428
16.2
52lm
0092
n160
33V
MC
J051
433.
63-6
9391
9.03
1.47
342
16.0
6615
.612
lm02
14k2
5540
VM
CJ0
5301
4.20
-683
054.
971.
4768
4317
.558
17.5
44lm
0364
n985
5V
MC
J054
558.
79-6
7103
4.27
1.47
7007
17.7
3417
.622
lm00
20m
1481
2V
MC
J053
006.
95-6
9084
5.62
1.47
8725
16.2
0015
.924
lm01
73m
2275
2V
MC
J050
528.
36-6
8073
2.55
1.47
9232
16.9
4516
.668
lm01
73l2
9233
VM
CJ0
5033
5.63
-681
853.
851.
4801
1517
.028
16.7
90lm
0300
k223
31V
MC
J050
335.
08-6
6240
2.09
1.48
138
17.9
5817
.738
lm03
46k1
2896
VM
CJ0
5314
4.92
-672
341.
691.
4817
8416
.295
16.9
02lm
0333
m10
861
VM
CJ0
5281
8.84
-663
945.
551.
4821
4816
.212
15.9
90lm
0556
m65
25*
VM
CJ0
5024
4.20
-713
208.
391.
4934
9416
.116
16.0
67lm
0030
n125
00*
VM
CJ0
5371
1.38
-692
325.
861.
4997
8415
.983
15.7
44
201
lm03
46m
2339
8V
MC
J053
218.
78-6
7274
2.65
1.51
9681
16.5
1716
.428
lm00
56k8
196
VM
CJ0
5522
0.90
-700
913.
421.
5239
2617
.006
16.9
52lm
0125
l930
2V
MC
J045
306.
88-6
9572
4.58
1.52
6312
16.0
5116
.893
lm01
03m
2315
0V
MC
J050
908.
75-6
9313
5.47
1.52
7199
17.3
5617
.050
lm01
84l1
1316
VM
CJ0
5072
0.38
-683
440.
281.
5299
2217
.556
17.3
39lm
0040
l135
85V
MC
J054
401.
94-6
9173
3.61
1.53
4167
16.7
9717
.140
lm00
20k1
3620
VM
CJ0
5273
3.57
-690
908.
231.
5347
0216
.587
16.2
35lm
0196
k267
64V
MC
J051
520.
48-6
8525
0.05
1.53
8051
16.6
8416
.519
lm00
90m
4818
VM
CJ0
5135
9.87
-690
455.
711.
5419
2416
.336
16.2
24lm
0016
m17
269
VM
CJ0
5220
4.48
-701
232.
451.
5423
3817
.270
17.1
00lm
0573
n131
73V
MC
J052
259.
87-7
1012
6.56
1.54
5989
17.3
7317
.321
lm03
40l8
577
VM
CJ0
5305
0.61
-662
750.
561.
5463
6116
.794
16.5
51lm
0427
m21
459
VM
CJ0
5030
9.74
-660
353.
591.
5465
4717
.025
16.8
90lm
0026
k106
65V
MC
J052
718.
12-7
0102
0.06
1.54
8267
17.0
3816
.819
lm02
14k2
4604
VM
CJ0
5301
2.25
-683
032.
631.
5487
0615
.709
15.8
53lm
0090
n117
30V
MC
J051
344.
44-6
9164
7.91
1.55
4973
16.8
6116
.668
lm01
14l6
671
VM
CJ0
4560
8.39
-695
634.
461.
5558
7816
.077
16.4
64lm
0184
l966
0V
MC
J050
732.
58-6
8340
4.62
1.56
8984
16.2
4416
.099
lm02
14l2
5109
VM
CJ0
5293
0.93
-684
012.
841.
5755
7816
.596
17.3
91lm
0032
l228
74V
MC
J053
529.
76-6
9422
2.65
1.57
6927
15.7
5915
.406
lm03
37k2
3492
VM
CJ0
5272
0.43
-672
758.
771.
5786
2817
.247
17.2
09lm
0207
k154
72V
MC
J052
636.
95-6
8480
1.13
1.57
9423
15.3
9215
.651
lm00
23m
7584
VM
CJ0
5342
1.06
-692
631.
391.
5798
8716
.008
15.7
14lm
0434
m21
038
VM
CJ0
5061
0.75
-654
136.
071.
5855
4716
.551
16.2
49lm
0172
l157
09V
MC
J050
022.
92-6
8201
4.39
1.58
8034
17.4
6517
.348
lm05
40k9
199
VM
CJ0
4522
6.26
-703
024.
461.
5883
9616
.217
16.2
98lm
0335
n574
7V
MC
J052
859.
28-6
7081
1.51
1.58
8518
17.2
4317
.077
lm03
76m
1233
8V
MC
J055
408.
79-6
7231
6.93
1.59
1615
16.8
1516
.898
lm03
30n1
0876
VM
CJ0
5250
3.26
-662
825.
241.
5936
1216
.191
16.6
84lm
0210
l202
71V
MC
J052
945.
11-6
7561
7.49
1.59
4599
16.6
5016
.466
lm05
50n7
880
VM
CJ0
5031
2.39
-703
915.
871.
5968
5817
.242
17.0
10lm
0435
l575
2V
MC
J050
905.
46-6
5441
2.60
1.59
7033
17.5
8817
.604
lm03
44m
8291
VM
CJ0
5322
3.60
-670
037.
001.
5972
4316
.603
16.4
41lm
0031
m74
14V
MC
J054
227.
01-6
9051
4.40
1.60
5989
15.3
4515
.399
lm01
75k1
8167
VM
CJ0
5041
6.00
-682
709.
191.
6062
0616
.581
16.3
29lm
0044
l236
59V
MC
J054
320.
00-7
0031
9.30
1.60
7072
16.3
2916
.238
lm01
97k2
3467
VM
CJ0
5192
2.30
-685
056.
341.
6083
4716
.394
16.2
80lm
0325
n233
85V
MC
J052
144.
24-6
7145
6.26
1.60
901
17.1
1116
.982
lm01
61n2
4107
VM
CJ0
4580
2.92
-675
630.
701.
6114
7517
.580
17.5
23lm
0367
n683
5V
MC
J054
949.
23-6
7301
4.98
1.61
154
17.6
9917
.638
lm06
03l2
4970
VM
CJ0
5471
6.29
-710
559.
591.
6142
2717
.190
17.0
66
202
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0030
k132
05V
MC
J053
556.
53-6
9085
1.07
1.61
5205
15.6
2115
.905
lm05
50m
2019
6V
MC
J050
212.
68-7
0351
1.11
1.61
6823
17.3
3717
.137
lm04
25n1
5511
VM
CJ0
5023
7.74
-654
810.
171.
6233
8417
.744
17.5
96lm
0210
l188
28V
MC
J053
006.
02-6
7553
6.00
1.62
5897
17.4
7417
.450
lm07
10k1
0285
VM
CJ0
5314
3.64
-715
525.
171.
6278
4217
.415
17.5
53lm
0090
n299
58V
MC
J051
408.
45-6
9230
0.22
1.62
8407
17.4
8517
.095
lm03
44k1
0601
VM
CJ0
5301
2.11
-670
137.
351.
6286
0416
.646
16.5
35lm
0711
m42
18V
MC
J053
809.
16-7
1515
2.38
1.63
0559
16.1
5017
.089
lm05
84l6
042
VM
CJ0
5264
2.20
-712
027.
141.
6323
4416
.404
16.9
32lm
0424
n101
33V
MC
J045
954.
71-6
5462
1.02
1.63
539
15.7
6116
.247
lm00
93n2
4281
VM
CJ0
5170
6.36
-694
056.
921.
6357
9917
.515
17.1
13lm
0204
m18
679
VM
CJ0
5243
7.28
-682
732.
491.
6364
7217
.411
17.3
29lm
0201
n264
07V
MC
J052
835.
82-6
7571
3.84
1.63
867
17.4
5317
.510
lm03
33k9
915
VM
CJ0
5264
7.20
-663
933.
451.
6390
6816
.656
16.4
88lm
0090
m43
21V
MC
J051
424.
31-6
9044
4.21
1.64
1272
17.0
1316
.842
lm00
32m
2226
1V
MC
J053
724.
44-6
9341
9.40
1.64
4146
15.9
6315
.623
lm05
51l2
1081
VM
CJ0
5034
1.36
-704
404.
321.
6452
1115
.833
15.5
61lm
0101
l229
00V
MC
J050
740.
89-6
9203
1.03
1.65
3449
16.1
9615
.963
lm03
04n2
5535
VM
CJ0
5041
6.28
-671
551.
761.
6572
4515
.798
15.7
07lm
0033
k153
95V
MC
J054
014.
74-6
9293
5.55
1.65
801
15.8
5615
.767
lm00
30l4
662
VM
CJ0
5362
2.07
-691
412.
041.
6606
5116
.302
16.8
00lm
0344
l240
76V
MC
J053
034.
04-6
7162
2.54
1.66
2852
16.3
5316
.213
lm03
25k9
805
VM
CJ0
5211
6.52
-670
037.
651.
6643
5116
.290
16.0
79lm
0207
n185
37V
MC
J052
805.
77-6
8590
5.10
1.66
4777
15.6
8915
.555
lm05
83l2
2712
VM
CJ0
5292
4.87
-710
456.
801.
6655
6515
.818
15.5
14lm
0212
n205
73V
MC
J053
207.
19-6
8170
6.13
1.66
8092
16.6
8716
.830
lm02
16l8
793
VM
CJ0
5301
8.27
-685
515.
641.
6690
4315
.814
15.7
98lm
0127
n645
5V
MC
J045
414.
43-7
0174
1.35
1.66
9262
16.3
2516
.148
lm01
84k2
2807
VM
CJ0
5072
4.58
-682
932.
361.
6725
0516
.419
16.7
08lm
0030
m34
68V
MC
J053
740.
88-6
9044
1.50
1.67
4098
15.8
7715
.992
lm01
27m
8589
VM
CJ0
4550
3.04
-700
917.
181.
6766
1317
.068
17.0
80lm
0035
m23
233
VM
CJ0
5424
7.23
-695
305.
281.
6776
2515
.456
15.4
42lm
0344
l135
98V
MC
J053
031.
13-6
7120
3.93
1.68
5395
16.5
5616
.262
lm03
76n1
1230
VM
CJ0
5530
9.98
-673
210.
211.
6863
6817
.761
17.5
68lm
0340
n595
0V
MC
J053
209.
76-6
6262
7.63
1.69
2577
15.5
3915
.507
lm00
21m
1520
7V
MC
J053
320.
13-6
9081
2.64
1.69
5205
17.1
3417
.141
lm01
86m
1876
4V
MC
J050
929.
29-6
8493
5.24
1.69
7031
15.7
7215
.672
lm03
44k4
409
VM
CJ0
5300
6.15
-665
906.
661.
6970
5316
.337
16.1
83lm
0221
n123
98V
MC
J054
311.
88-6
7522
9.02
1.70
0592
17.2
4817
.199
lm02
14n4
693
VM
CJ0
5313
7.55
-683
202.
081.
7027
5417
.039
17.3
66lm
0207
m26
339
VM
CJ0
5272
2.36
-685
208.
121.
7150
1516
.191
15.9
56
203
lm03
44n5
050
VM
CJ0
5320
1.43
-670
825.
851.
7189
516
.739
16.5
94lm
0117
k265
36V
MC
J050
018.
07-7
0164
8.93
1.72
5788
16.9
7716
.787
lm03
66m
3543
VM
CJ0
5455
5.72
-671
923.
241.
7279
4217
.109
17.0
10lm
0333
k279
25V
MC
J052
737.
68-6
6460
0.67
1.73
1749
17.4
3317
.357
lm01
25k2
2446
VM
CJ0
4515
7.79
-695
306.
671.
7351
8616
.405
16.4
76lm
0710
k722
2V
MC
J053
027.
87-7
1540
8.47
1.74
6476
17.0
8817
.134
lm01
27l6
731
VM
CJ0
4525
1.09
-701
741.
331.
7481
5815
.547
15.3
05lm
0127
m93
30V
MC
J045
433.
62-7
0093
8.70
1.75
1161
15.7
7415
.864
lm02
05n1
5591
VM
CJ0
5272
0.98
-683
522.
881.
7536
9716
.514
16.2
25lm
0436
l145
85V
MC
J050
541.
42-6
6093
3.77
1.75
6971
15.8
9715
.963
lm01
84n9
824
VM
CJ0
5100
0.53
-683
353.
201.
7571
4315
.694
16.0
37lm
0020
m10
621
VM
CJ0
5295
6.91
-690
712.
601.
7588
7615
.247
15.2
36lm
0223
m18
449
VM
CJ0
5430
5.08
-680
646.
091.
7598
1616
.880
16.8
34lm
0090
l212
36V
MC
J051
151.
43-6
9204
9.38
1.76
0117
.343
17.0
15lm
0030
n222
78V
MC
J053
726.
68-6
9211
9.34
1.76
0563
16.7
3116
.629
lm02
17n2
4885
VM
CJ0
5360
9.55
-685
527.
461.
7624
0816
.294
16.0
96lm
0045
n247
54V
MC
J054
937.
26-7
0054
5.14
1.76
449
16.9
9216
.694
lm02
06k1
8004
VM
CJ0
5220
8.75
-684
900.
571.
7655
5916
.694
16.7
08lm
0304
n290
84V
MC
J050
357.
90-6
7171
2.57
1.77
2755
15.9
6215
.743
lm05
50k1
9577
VM
CJ0
5011
0.29
-703
512.
781.
7746
5116
.258
15.9
52lm
0291
m21
869
VM
CJ0
5001
8.99
-662
301.
691.
7748
1617
.366
17.2
00lm
0101
k866
9V
MC
J050
818.
75-6
9061
8.00
1.77
5599
16.4
5816
.273
lm00
12l1
6381
VM
CJ0
5193
9.82
-693
930.
371.
7790
215
.982
15.7
06lm
0031
m22
434
VM
CJ0
5422
6.89
-691
140.
761.
7790
4916
.929
17.0
87lm
0543
k125
03V
MC
J045
641.
13-7
0520
8.24
1.78
0468
17.0
2517
.055
lm02
17l1
7550
VM
CJ0
5333
2.41
-685
854.
051.
7842
0116
.738
16.7
60lm
0014
m14
940*
VM
CJ0
5214
9.02
-695
017.
371.
7856
3416
.944
16.8
97lm
0031
m11
024
VM
CJ0
5423
0.15
-691
313.
221.
7887
4117
.159
17.2
90lm
0344
l161
03V
MC
J053
031.
34-6
7130
6.04
1.79
294
15.5
6915
.568
lm00
53k1
1941
VM
CJ0
5563
5.72
-692
821.
721.
7997
3617
.231
17.4
49lm
0300
k545
0V
MC
J050
322.
38-6
6165
6.91
1.80
1747
16.1
1515
.966
lm04
67k1
1376
VM
CJ0
5281
9.72
-655
900.
261.
8021
7515
.677
15.5
18lm
0173
m15
001
VM
CJ0
5053
5.16
-680
448.
151.
8030
3517
.718
17.3
93lm
0010
l242
69V
MC
J052
025.
52-6
9220
0.41
1.80
3838
16.1
1315
.775
lm04
55n9
465
VM
CJ0
5233
2.51
-654
530.
841.
8047
2617
.457
17.1
95lm
0336
l200
11V
MC
J052
440.
50-6
7382
0.51
1.80
7377
17.0
5617
.057
lm03
42k4
708
VM
CJ0
5313
1.23
-663
804.
451.
8073
8917
.023
16.8
75lm
0340
l195
94V
MC
J053
113.
33-6
6350
6.98
1.80
9525
15.6
6115
.398
lm03
34l2
0839
VM
CJ0
5234
7.23
-671
749.
011.
8132
5516
.114
15.9
44lm
0323
m29
284
VM
CJ0
5212
1.36
-664
637.
351.
8148
7917
.290
17.4
29lm
0046
k175
69V
MC
J054
438.
66-7
0141
3.83
1.81
5216
16.8
2616
.822
204
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0257
m20
281*
VM
CJ0
6050
5.88
-685
110.
751.
8213
0617
.269
17.2
50lm
0583
l193
73V
MC
J052
949.
18-7
1034
7.39
1.82
2309
16.2
5315
.965
lm03
40m
6792
VM
CJ0
5321
1.55
-661
728.
731.
8254
7916
.564
16.4
54lm
0186
n118
96V
MC
J050
927.
62-6
8561
9.21
1.82
799
17.3
3516
.997
lm02
31l2
4501
VM
CJ0
5481
7.13
-675
727.
751.
8334
2616
.737
16.6
01lm
0305
l177
96V
MC
J050
708.
80-6
7123
1.16
1.83
3544
17.2
4917
.275
lm01
93n1
3361
VM
CJ0
5211
9.22
-681
332.
151.
8345
8917
.570
17.4
30lm
0114
k178
80V
MC
J045
620.
59-6
9514
4.31
1.84
2075
17.2
0616
.931
lm00
33k2
872
VM
CJ0
5395
2.21
-692
452.
911.
8426
4217
.165
17.0
43lm
0195
m11
246
VM
CJ0
5195
6.85
-682
450.
961.
8538
8617
.483
17.3
44lm
0095
m26
03*
VM
CJ0
5184
9.48
-694
604.
151.
8595
7617
.454
17.3
65lm
0424
m15
104
VM
CJ0
5003
0.23
-653
854.
611.
8610
2116
.284
16.0
79lm
0022
l136
31V
MC
J052
739.
83-6
9383
3.90
1.86
3346
16.3
9616
.553
lm04
55l1
7462
VM
CJ0
5212
9.04
-654
936.
531.
8661
6816
.837
16.8
66lm
0115
l932
1V
MC
J050
027.
66-6
9572
4.94
1.86
7104
17.0
2916
.888
lm02
91l2
5349
VM
CJ0
4590
0.43
-663
317.
111.
8742
4816
.856
16.8
52lm
0173
m20
587
VM
CJ0
5050
0.89
-680
650.
971.
8744
7817
.235
16.9
59lm
0540
m22
710
VM
CJ0
4534
8.79
-703
544.
281.
8766
8116
.531
16.6
18lm
0171
n188
34V
MC
J050
559.
23-6
7573
7.97
1.87
7095
16.5
4517
.043
lm02
26k6
378
VM
CJ0
5374
7.98
-684
446.
101.
8778
7316
.651
16.8
88lm
0550
k193
85V
MC
J050
014.
84-7
0350
7.65
1.87
8439
16.1
3016
.021
lm01
95m
9279
VM
CJ0
5211
4.37
-682
400.
271.
8800
8616
.651
16.4
91lm
0125
m29
599
VM
CJ0
4534
3.29
-695
513.
531.
8810
5517
.522
17.5
62lm
0335
l226
11V
MC
J052
655.
66-6
7150
0.28
1.88
6389
16.0
2615
.793
lm00
15l2
4985
VM
CJ0
5232
7.72
-700
253.
321.
8869
4716
.222
15.9
01lm
0012
n190
00V
MC
J052
214.
30-6
9395
5.73
1.88
7943
15.9
3015
.775
lm05
45n1
9142
VM
CJ0
4580
1.37
-712
450.
171.
8880
9516
.876
16.7
13lm
0184
n181
18V
MC
J050
941.
57-6
8363
8.07
1.89
0723
16.5
7016
.467
lm00
30l1
0277
VM
CJ0
5364
3.01
-691
639.
571.
8908
3817
.177
17.1
33lm
0011
n177
83V
MC
J052
630.
09-6
9181
1.54
1.90
002
17.3
2217
.273
lm02
12m
1916
9V
MC
J053
100.
08-6
8090
3.95
1.90
0405
15.5
9315
.575
lm04
66n2
0073
VM
CJ0
5261
9.77
-661
153.
801.
9005
0217
.029
17.1
01lm
0013
m74
66V
MC
J052
603.
43-6
9263
7.05
1.90
3719
15.7
7915
.369
lm02
17n1
7433
VM
CJ0
5354
1.09
-685
857.
901.
9068
9616
.026
16.2
09lm
0093
m28
032
VM
CJ0
5181
1.10
-693
255.
611.
9084
0616
.792
16.9
24lm
0455
l895
8V
MC
J052
203.
66-6
5454
9.37
1.90
9773
16.9
1116
.732
lm03
55n1
7331
VM
CJ0
5435
5.71
-671
728.
721.
9148
5817
.286
17.3
25lm
0424
n245
16V
MC
J050
012.
68-6
5525
8.00
1.91
5386
15.8
4515
.628
lm03
33n1
6187
VM
CJ0
5284
9.50
-665
051.
911.
9173
716
.075
15.8
99lm
0014
k224
35V
MC
J052
036.
79-6
9530
2.65
1.91
8806
16.7
5116
.491
lm00
91l5
423
VM
CJ0
5161
2.97
-691
412.
151.
9238
7716
.246
16.6
17
205
lm03
01l2
2532
VM
CJ0
5055
1.70
-663
237.
271.
9251
0116
.176
15.9
93lm
0187
k173
40V
MC
J051
133.
78-6
8484
0.14
1.92
5776
16.8
1316
.835
lm03
06m
3943
VM
CJ0
5034
6.96
-671
920.
361.
9272
4116
.452
16.7
00lm
0333
k393
0V
MC
J052
734.
68-6
6371
7.69
1.93
1105
16.8
0016
.721
lm06
12l1
0791
VM
CJ0
5511
7.34
-710
200.
471.
9314
2816
.789
16.8
00lm
0040
l108
57V
MC
J054
326.
23-6
9162
5.48
1.93
296
15.3
1515
.609
lm04
36m
1006
9*V
MC
J050
638.
56-6
5585
0.58
1.93
3416
.791
16.6
16lm
0214
l242
28V
MC
J052
951.
41-6
8395
3.31
1.94
0698
16.2
4716
.101
lm01
75m
1986
4V
MC
J050
637.
38-6
8273
7.16
1.94
6591
16.4
9816
.217
lm03
31l1
9382
VM
CJ0
5275
9.07
-663
137.
081.
9513
5815
.888
15.6
61lm
0033
m22
177
VM
CJ0
5415
0.32
-693
157.
751.
9542
9115
.544
15.5
67lm
0032
l129
16V
MC
J053
547.
17-6
9383
1.87
1.96
0459
15.8
0015
.698
lm01
91n9
387*
VM
CJ0
5211
1.63
-675
534.
671.
9627
516
.791
16.5
70lm
0030
k121
30*
VM
CJ0
5361
7.19
-690
822.
451.
9628
416
.938
16.8
87lm
0024
m78
51V
MC
J052
924.
86-6
9480
8.06
1.96
6268
17.3
4517
.033
lm01
70l1
4651
VM
CJ0
4594
7.76
-675
339.
111.
9678
1817
.381
17.3
92lm
0294
n623
0*V
MC
J045
752.
57-6
7084
1.93
1.96
9416
.963
16.9
44lm
0091
m30
316
VM
CJ0
5171
5.96
-691
319.
621.
9787
6116
.717
16.3
90lm
0090
l129
95*
VM
CJ0
5121
6.17
-691
728.
321.
9823
4215
.283
16.4
95lm
0020
k121
15*
VM
CJ0
5275
7.42
-690
830.
001.
9894
7614
.578
14.2
21lm
0101
n239
16*
VM
CJ0
5094
0.09
-692
027.
991.
9900
614
.679
14.2
56lm
0025
n153
53*
VM
CJ0
5344
0.77
-695
921.
451.
9908
1416
.523
16.4
35lm
0031
n230
92*
VM
CJ0
5415
9.42
-692
053.
142.
0188
3217
.297
17.0
68lm
0015
n101
53*
VM
CJ0
5254
7.65
-695
735.
202.
0201
9616
.519
16.9
82lm
0344
l255
18V
MC
J053
026.
56-6
7165
8.34
2.02
3458
16.5
7616
.471
lm05
83k6
016
VM
CJ0
5295
9.41
-705
054.
112.
0243
8916
.299
16.1
21lm
0306
l804
1*V
MC
J050
306.
00-6
7300
9.81
2.02
5378
17.6
4517
.533
lm03
66l1
5212
VM
CJ0
5444
3.45
-673
347.
502.
0294
3115
.879
15.7
61lm
0307
l175
42V
MC
J050
702.
43-6
7350
0.13
2.03
4164
15.7
8515
.612
lm00
33k1
1169
VM
CJ0
5401
4.85
-692
758.
722.
0439
6315
.281
15.1
16lm
0296
m14
458
VM
CJ0
4570
2.64
-672
344.
422.
0440
7215
.662
15.4
64lm
0427
n127
88*
VM
CJ0
5041
2.98
-660
913.
592.
0484
9217
.539
17.6
49lm
0184
n113
34V
MC
J050
844.
93-6
8342
6.34
2.04
8845
17.0
6817
.031
lm03
23k1
6171
VM
CJ0
5202
6.98
-664
150.
182.
0509
6416
.971
16.9
33lm
0207
k277
93*
VM
CJ0
5270
5.79
-685
233.
292.
0549
9416
.884
16.9
54lm
0214
l232
57V
MC
J053
025.
55-6
8392
9.91
2.05
6505
17.4
4817
.489
lm04
67m
1302
7*V
MC
J052
945.
12-6
5592
8.13
2.05
7866
16.5
0216
.296
lm00
30l1
2866
VM
CJ0
5360
1.42
-691
748.
252.
0587
5615
.503
15.5
29lm
0101
m21
049
VM
CJ0
5102
7.09
-691
036.
552.
0591
9815
.558
15.6
62lm
0217
n111
96V
MC
J053
554.
09-6
8555
9.45
2.05
9265
16.2
0916
.038
lm00
31l2
6732
VM
CJ0
5400
2.00
-692
210.
742.
0607
8717
.366
17.1
28
206
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0015
m33
370*
VM
CJ0
5255
8.88
-695
547.
522.
0640
4616
.518
16.3
45lm
0581
l215
36*
VM
CJ0
5302
9.23
-704
332.
072.
0641
1617
.366
17.1
71lm
0021
l660
9V
MC
J053
203.
23-6
9143
6.59
2.06
4204
15.6
8515
.455
lm01
03n1
9330
*V
MC
J051
017.
91-6
9393
2.44
2.06
4678
16.9
1216
.612
lm01
82k1
6150
*V
MC
J050
720.
77-6
8072
9.73
2.06
5838
16.2
2216
.175
lm03
40m
1595
0V
MC
J053
156.
66-6
6212
4.11
2.06
6753
15.8
4315
.751
lm00
13k3
0220
*V
MC
J052
410.
69-6
9334
5.42
2.07
2228
15.6
7916
.779
lm00
30k1
6342
VM
CJ0
5363
5.07
-691
028.
122.
0728
5216
.113
16.0
73lm
0030
n202
33V
MC
J053
654.
77-6
9225
8.32
2.07
7922
16.0
5015
.832
lm05
87l1
8183
*V
MC
J053
025.
40-7
1465
9.83
2.07
7996
16.3
9816
.632
lm03
64n1
2802
VM
CJ0
5470
0.75
-671
146.
562.
0788
1816
.716
16.7
39lm
0376
m19
861
VM
CJ0
5543
1.36
-672
910.
332.
0828
9916
.815
16.8
52lm
0216
l176
02V
MC
J053
020.
11-6
8590
7.74
2.08
8156
16.2
7516
.076
lm03
74l1
5319
VM
CJ0
5515
5.42
-671
312.
722.
0905
4716
.607
16.5
21lm
0021
n140
65V
MC
J053
445.
71-6
9165
2.11
2.09
1973
16.9
7716
.816
lm00
17k1
8680
*V
MC
J052
322.
73-7
0132
4.01
2.09
4048
16.7
5717
.051
lm04
26n2
3242
*V
MC
J050
005.
65-6
6130
2.21
2.09
473
16.7
1016
.582
lm05
43m
1126
7*V
MC
J045
829.
12-7
0513
1.81
2.09
621
16.4
1016
.645
lm00
20k1
8818
VM
CJ0
5273
9.64
-691
118.
352.
1014
9115
.917
15.5
96lm
0184
k771
4V
MC
J050
740.
70-6
8240
8.60
2.10
2557
15.5
5715
.333
lm00
90n2
8977
VM
CJ0
5133
6.22
-692
241.
422.
1087
2516
.542
16.1
76lm
0210
n248
68V
MC
J053
153.
66-6
7573
8.38
2.11
375
16.6
2616
.497
lm05
85k2
867
VM
CJ0
5304
0.80
-711
011.
102.
1137
9917
.228
17.1
99lm
0184
k277
93*
VM
CJ0
5074
0.40
-683
120.
022.
1163
5217
.237
17.3
01lm
0340
l801
5V
MC
J053
059.
30-6
6273
5.08
2.11
7866
15.9
2315
.787
lm00
20l9
163
VM
CJ0
5281
8.55
-691
605.
472.
1274
0316
.139
16.0
34lm
0214
k135
90V
MC
J052
926.
63-6
8261
5.25
2.13
3649
17.1
1117
.140
lm03
27m
5562
VM
CJ0
5221
5.41
-672
012.
932.
1370
4616
.306
16.1
70lm
0335
n145
42V
MC
J052
930.
89-6
7112
3.90
2.13
9656
17.2
9817
.110
lm00
93n2
2090
*V
MC
J051
739.
94-6
9401
2.33
2.14
0468
16.6
2517
.282
lm05
74m
1665
7V
MC
J051
947.
00-7
1145
4.76
2.14
0756
16.0
8415
.889
lm01
15k2
3126
VM
CJ0
4593
4.87
-695
305.
662.
1422
1817
.251
17.1
00lm
0013
l323
65V
MC
J052
339.
33-6
9433
4.38
2.14
5755
15.8
4415
.965
lm00
31l9
480*
VM
CJ0
5395
3.09
-691
530.
242.
1493
9417
.356
16.8
15lm
0365
l953
2V
MC
J054
818.
80-6
7100
9.18
2.14
9591
17.3
3017
.263
lm03
31m
1149
6V
MC
J052
926.
30-6
6190
0.38
2.15
1473
16.0
2515
.877
lm01
75m
1431
0V
MC
J050
634.
35-6
8254
4.08
2.15
4499
15.4
5014
.998
lm02
04k1
1078
*V
MC
J052
221.
57-6
8250
3.49
2.15
745
16.8
0916
.852
lm03
75k1
9793
VM
CJ0
5551
8.04
-670
541.
262.
1586
9116
.387
16.3
41lm
0016
n213
06*
VM
CJ0
5222
7.26
-702
341.
902.
1593
3416
.965
16.7
21lm
0344
k168
54V
MC
J053
027.
16-6
7040
9.15
2.16
4252
16.1
4215
.939
207
lm00
31m
1900
1V
MC
J054
103.
31-6
9102
1.77
2.16
5249
16.6
6916
.969
lm03
21m
8452
VM
CJ0
5222
4.18
-661
737.
442.
1682
2116
.724
16.7
44lm
0214
n107
75*
VM
CJ0
5315
9.53
-683
419.
682.
1757
2817
.488
17.3
45lm
0012
m16
798
VM
CJ0
5223
5.33
-693
143.
322.
1833
5416
.043
15.6
24lm
0205
n257
42V
MC
J052
840.
72-6
8413
6.80
2.18
4881
15.4
4415
.233
lm02
94n1
3388
VM
CJ0
4574
4.69
-671
120.
122.
1881
4115
.849
15.6
79lm
0366
l637
5*V
MC
J054
436.
51-6
7293
2.75
2.18
9006
17.2
8717
.147
lm05
43m
9484
*V
MC
J045
730.
80-7
0510
0.20
2.18
9417
.229
17.2
24lm
0191
n226
5V
MC
J051
951.
52-6
7500
5.72
2.19
3241
16.9
1416
.868
lm00
13m
2028
3V
MC
J052
603.
17-6
9305
2.56
2.19
3383
15.4
5515
.219
lm05
41n4
981
VM
CJ0
4583
9.79
-703
826.
472.
1958
7616
.891
16.7
15lm
0300
m25
571
VM
CJ0
5043
4.81
-662
559.
992.
2007
4715
.958
15.8
09lm
0610
k411
3V
MC
J055
126.
09-7
0320
8.81
2.21
4823
17.0
7717
.076
lm00
20k1
1440
VM
CJ0
5281
5.05
-690
811.
692.
2201
6915
.109
14.9
63lm
0203
n153
93V
MC
J052
722.
65-6
8140
7.98
2.22
5954
15.6
7915
.476
lm05
81k6
931
VM
CJ0
5303
5.14
-702
923.
352.
2275
9516
.830
16.9
39lm
0230
m41
55V
MC
J054
722.
01-6
7402
7.42
2.22
9129
17.0
4717
.026
lm00
33m
2476
2V
MC
J054
118.
77-6
9325
6.97
2.23
0059
16.4
7116
.208
lm03
03n1
2403
VM
CJ0
5072
0.40
-664
917.
752.
2344
7816
.658
15.5
93lm
0335
k267
60V
MC
J052
657.
47-6
7070
1.31
2.23
4913
16.1
4915
.925
lm01
03l1
1316
VM
CJ0
5085
5.37
-693
659.
622.
2353
8716
.967
16.7
17lm
0301
n983
2V
MC
J050
730.
80-6
6272
9.86
2.24
2879
15.9
8616
.055
lm01
27n2
1487
VM
CJ0
4543
4.59
-702
425.
972.
2446
5916
.931
16.9
80lm
0200
k250
34V
MC
J052
207.
88-6
7485
6.17
2.24
4789
16.5
8616
.515
lm01
93m
1493
5V
MC
J051
954.
07-6
8045
5.35
2.24
9797
15.1
4915
.035
lm00
20k2
4295
VM
CJ0
5283
1.27
-691
340.
712.
2507
0116
.443
16.0
38lm
0331
l174
55V
MC
J052
759.
22-6
6305
2.92
2.25
4984
16.2
5616
.820
lm04
66l1
5239
VM
CJ0
5251
7.86
-660
946.
102.
2586
416
.430
16.2
21lm
0021
l327
91V
MC
J053
218.
71-6
9231
8.54
2.25
996
17.0
2016
.683
lm00
33l8
128*
VM
CJ0
5400
1.58
-693
606.
812.
2622
7815
.604
15.8
75lm
0117
m10
584
VM
CJ0
5012
5.12
-701
013.
802.
2682
615
.645
15.5
72lm
0294
m26
342
VM
CJ0
4581
6.03
-670
641.
292.
2712
5417
.272
17.0
62lm
0100
n569
0V
MC
J050
637.
75-6
9142
1.91
2.27
321
16.6
4016
.639
lm00
30n1
8202
VM
CJ0
5375
8.63
-691
941.
382.
2737
9816
.169
16.0
36lm
0551
k220
31V
MC
J050
346.
11-7
0371
1.18
2.27
601
17.4
7917
.092
lm00
93m
1894
0V
MC
J051
739.
28-6
9300
7.67
2.27
7221
16.5
6116
.373
lm01
73l1
3985
VM
CJ0
5034
2.58
-681
351.
742.
2785
916
.326
16.1
28lm
0092
m20
117*
VM
CJ0
5140
1.93
-693
311.
092.
2794
216
.821
16.6
73lm
0161
m20
878
VM
CJ0
4581
9.44
-674
622.
352.
2795
816
.318
16.3
16lm
0117
m15
641
VM
CJ0
5022
3.60
-701
205.
802.
2838
16.5
0116
.233
lm05
43n2
7195
VM
CJ0
4585
4.80
-710
613.
142.
2933
1717
.055
17.1
55
208
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0184
k135
61*
VM
CJ0
5072
5.44
-682
612.
682.
2941
7216
.195
16.4
77lm
0337
k201
28V
MC
J052
739.
26-6
7263
2.76
2.30
0298
15.7
8915
.461
lm00
90l1
3156
VM
CJ0
5123
6.57
-691
731.
712.
3012
6616
.375
16.3
34lm
0355
n122
09V
MC
J054
300.
35-6
7105
9.52
2.30
3794
17.1
5617
.063
lm03
66l2
1345
VM
CJ0
5444
7.47
-673
801.
432.
3285
2416
.527
16.7
07lm
0200
l194
91V
MC
J052
157.
43-6
7561
2.75
2.32
9272
15.6
2215
.825
lm01
86n1
4790
VM
CJ0
5082
5.60
-685
731.
182.
3330
2516
.949
16.9
78lm
0030
m41
63V
MC
J053
730.
75-6
9051
7.52
2.33
3416
14.7
7415
.119
lm00
20k2
403*
VM
CJ0
5283
0.37
-690
422.
922.
3358
7217
.161
17.1
82lm
0033
n254
48V
MC
J054
150.
30-6
9422
4.53
2.34
0327
16.4
6616
.151
lm01
15k2
8730
*V
MC
J050
031.
77-6
9545
6.05
2.34
1022
16.3
4616
.606
lm01
86k5
622
VM
CJ0
5074
9.03
-684
438.
352.
3418
9816
.765
16.5
44lm
0033
l897
8V
MC
J053
953.
42-6
9362
6.39
2.34
4895
15.5
6615
.693
lm01
03k4
043
VM
CJ0
5082
7.80
-692
528.
632.
3454
4115
.660
15.7
07lm
0426
m23
482
VM
CJ0
5001
8.72
-660
346.
732.
3455
7315
.291
15.1
29lm
0437
n826
7*V
MC
J050
931.
45-6
6065
4.35
2.35
3292
17.3
5017
.419
lm02
23n3
0265
VM
CJ0
5433
0.07
-681
949.
072.
3555
3115
.590
15.5
16lm
0091
n165
20V
MC
J051
714.
46-6
9175
6.24
2.36
1363
15.9
9615
.783
lm00
31m
1930
5V
MC
J054
108.
15-6
9102
8.57
2.36
1448
16.4
3716
.551
lm02
94n9
088
VM
CJ0
4574
3.46
-670
945.
932.
3656
8216
.854
16.7
45lm
0033
m29
238*
VM
CJ0
5420
8.84
-693
429.
712.
3694
4216
.885
17.0
10lm
0355
n198
96*
VM
CJ0
5424
2.12
-671
358.
552.
3717
516
.901
17.3
33lm
0205
l592
8V
MC
J052
635.
34-6
8321
2.58
2.37
907
16.6
7516
.898
lm00
12l2
4572
*V
MC
J051
944.
94-6
9422
1.32
2.38
0817
.663
17.2
08lm
0367
m17
417*
VM
CJ0
5493
4.20
-672
541.
732.
3814
6216
.588
16.5
83lm
0541
m17
201
VM
CJ0
4573
3.88
-703
304.
222.
3818
1316
.262
16.1
38lm
0427
m16
915
VM
CJ0
5040
8.27
-660
119.
212.
3828
6817
.446
17.2
99lm
0035
n291
74V
MC
J054
101.
78-7
0050
4.83
2.38
5178
15.6
4415
.633
lm01
87l1
7648
VM
CJ0
5121
8.60
-685
832.
422.
3905
3217
.122
16.9
92lm
0297
k160
68V
MC
J045
947.
96-6
7243
1.53
2.39
4267
15.4
2315
.329
lm00
15m
1296
4*V
MC
J052
620.
61-6
9492
1.75
2.39
4782
17.0
7017
.013
lm05
56k7
966
VM
CJ0
5000
6.52
-713
236.
562.
3982
0816
.372
16.3
93lm
0230
l159
82V
MC
J054
419.
25-6
7544
9.55
2.39
8351
16.9
3016
.847
lm03
05n1
3969
VM
CJ0
5074
1.97
-671
313.
432.
3992
4615
.987
15.8
84lm
0093
m64
82V
MC
J051
715.
38-6
9261
4.89
2.40
0068
17.3
1717
.044
lm00
30k7
421
VM
CJ0
5362
0.35
-690
615.
752.
4038
4216
.625
16.6
37lm
0323
n207
98*
VM
CJ0
5224
0.22
-665
225.
022.
4086
7217
.196
17.3
08lm
0033
m27
772
VM
CJ0
5413
2.23
-693
401.
792.
4112
1616
.610
16.5
73lm
0346
k171
36V
MC
J053
044.
42-6
7253
6.18
2.41
8824
15.6
8115
.447
lm00
30l1
5810
VM
CJ0
5360
4.55
-691
910.
422.
4193
9915
.816
15.8
55lm
0056
l258
26V
MC
J055
148.
54-7
0260
2.02
2.41
9986
16.9
0517
.063
209
lm00
15n1
7499
VM
CJ0
5265
3.58
-695
949.
422.
4310
9816
.613
16.5
56lm
0325
m19
625*
VM
CJ0
5212
8.05
-670
416.
102.
4319
2816
.048
15.8
60lm
0325
n971
8V
MC
J052
234.
47-6
7093
2.29
2.43
6797
16.5
8016
.635
lm00
13n2
2558
VM
CJ0
5250
3.44
-694
030.
012.
4374
4515
.196
15.7
73lm
0344
l183
57V
MC
J053
048.
33-6
7140
1.96
2.44
2181
16.8
7816
.549
lm05
50m
2326
6V
MC
J050
219.
33-7
0362
5.59
2.44
3675
15.3
7815
.331
lm03
40l2
2963
VM
CJ0
5310
5.42
-663
443.
422.
4471
9916
.090
15.8
43lm
0331
n553
3V
MC
J052
826.
55-6
6290
9.99
2.44
858
16.2
3215
.864
lm00
35k5
826
VM
CJ0
5404
2.32
-694
724.
782.
4572
8116
.051
16.0
31lm
0374
n649
9V
MC
J055
354.
03-6
7085
2.89
2.45
9114
17.0
9317
.072
lm03
44k5
068
VM
CJ0
5305
8.85
-665
922.
682.
4656
0816
.514
16.2
81lm
0093
m42
96V
MC
J051
756.
07-6
9252
8.88
2.46
9981
16.2
6215
.990
lm05
45m
6699
VM
CJ0
4590
2.42
-711
057.
712.
4712
3816
.576
16.6
92lm
0024
l508
3V
MC
J052
823.
84-6
9563
2.32
2.47
1267
16.3
3216
.272
lm00
95m
3281
4V
MC
J051
759.
42-6
9553
8.84
2.47
4934
16.9
2216
.816
lm03
21m
1701
8*V
MC
J052
131.
47-6
6211
4.59
2.48
037
16.1
9415
.982
lm03
44k2
4636
VM
CJ0
5314
0.72
-670
719.
322.
4832
4915
.696
15.4
75lm
0550
n149
03V
MC
J050
157.
58-7
0420
7.47
2.48
7136
16.2
7516
.052
lm04
27l1
0110
VM
CJ0
5010
7.92
-660
803.
002.
4892
5416
.778
16.6
26lm
0331
k101
98V
MC
J052
736.
30-6
6184
1.88
2.49
0214
16.4
9416
.416
lm00
10l1
7439
*V
MC
J051
956.
06-6
9191
5.10
2.49
3082
15.8
6815
.516
lm03
07k1
3715
VM
CJ0
5060
1.20
-672
331.
322.
4950
7416
.354
16.4
95lm
0542
l173
56V
MC
J045
153.
01-7
1040
4.47
2.49
5564
16.4
4316
.536
lm04
57n6
420
VM
CJ0
5232
1.04
-660
529.
142.
4956
5415
.752
15.5
15lm
0572
k323
8*V
MC
J051
801.
78-7
0491
0.02
2.49
5964
17.4
2817
.426
lm00
40k1
1551
*V
MC
J054
423.
15-6
9073
5.61
2.49
9232
16.8
9016
.878
lm00
32l2
0643
VM
CJ0
5360
2.65
-694
130.
942.
4993
9215
.790
15.3
80lm
0015
m19
643
VM
CJ0
5263
6.54
-695
125.
312.
5036
216
.890
16.5
69lm
0010
m68
43V
MC
J052
114.
52-6
9054
0.53
2.50
5974
15.9
9015
.665
lm03
03m
2160
4V
MC
J050
726.
63-6
6433
5.17
2.50
701
16.3
4316
.219
lm03
46m
1650
4V
MC
J053
159.
21-6
7244
9.84
2.50
8841
16.1
2215
.965
lm02
16l2
1415
VM
CJ0
5304
0.80
-690
051.
782.
5094
0716
.145
15.9
90lm
0540
n138
69V
MC
J045
359.
49-7
0412
6.63
2.51
2757
16.0
4915
.954
lm02
56m
2373
4*V
MC
J060
052.
16-6
8531
1.89
2.51
3574
17.5
3117
.743
lm05
96l1
9261
VM
CJ0
5334
3.35
-714
846.
382.
5153
9217
.026
17.2
90lm
0020
l266
44V
MC
J052
714.
33-6
9230
0.29
2.51
6899
16.7
5816
.369
lm01
80l6
512
VM
CJ0
5080
6.56
-675
027.
242.
5169
0915
.788
15.5
98lm
0186
n553
4V
MC
J050
858.
28-6
8534
3.40
2.52
9495
16.2
1816
.106
lm02
06m
2848
9V
MC
J052
409.
32-6
8522
6.75
2.53
1791
16.9
6316
.764
lm00
97n1
5434
VM
CJ0
5173
9.82
-702
127.
552.
5325
1816
.240
16.0
23lm
0015
m13
576
VM
CJ0
5253
2.18
-694
939.
022.
5341
1716
.534
16.4
79
210
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0023
k356
4V
MC
J053
124.
61-6
9252
8.08
2.53
6665
17.0
5116
.915
lm00
10l4
210
VM
CJ0
5192
1.83
-691
410.
072.
5519
6716
.991
16.5
86lm
0466
n153
47V
MC
J052
554.
98-6
6094
4.34
2.55
2722
16.4
8216
.734
lm02
12n1
8380
VM
CJ0
5305
4.27
-681
617.
552.
5538
9317
.090
17.1
25lm
0010
k172
35V
MC
J052
045.
22-6
9100
1.22
2.55
6111
16.1
7415
.967
lm03
33l2
4619
VM
CJ0
5280
4.34
-665
405.
972.
5567
0615
.857
15.6
88lm
0105
m14
713*
VM
CJ0
5095
3.12
-694
956.
112.
5589
116
.742
16.6
09lm
0581
m21
519
VM
CJ0
5310
7.06
-703
435.
432.
5594
2116
.895
16.8
73lm
0457
k246
67V
MC
J052
131.
27-6
6042
7.77
2.56
1858
16.5
8616
.504
lm01
00m
1626
6V
MC
J050
628.
93-6
9091
7.59
2.56
5832
16.5
8916
.501
lm01
70m
4805
VM
CJ0
5005
5.48
-674
051.
342.
5662
3216
.082
15.9
75lm
0307
m15
491
VM
CJ0
5085
9.82
-672
351.
192.
5697
516
.613
16.5
58lm
0020
k246
55V
MC
J052
833.
25-6
9134
9.10
2.57
9334
16.1
2715
.693
lm06
02l6
118
VM
CJ0
5423
8.05
-705
955.
392.
5809
4515
.454
15.5
24lm
0355
n264
48V
MC
J054
336.
43-6
7162
1.64
2.59
2838
15.1
8114
.955
lm03
31k1
8134
VM
CJ0
5273
1.92
-662
201.
922.
5956
4816
.818
16.5
68lm
0012
m28
14V
MC
J052
134.
84-6
9253
4.58
2.59
8916
.955
15.6
15lm
0366
n144
28V
MC
J054
712.
66-6
7332
0.55
2.60
1096
17.2
5617
.158
lm04
27m
1652
8V
MC
J050
306.
40-6
6011
8.95
2.60
8226
16.3
9616
.229
lm03
40n5
836
VM
CJ0
5322
9.63
-662
624.
022.
6144
5915
.861
15.6
18lm
0040
k234
76V
MC
J054
339.
83-6
9122
9.04
2.61
5418
15.9
2115
.801
lm01
16l1
9585
*V
MC
J045
604.
34-7
0231
0.12
2.61
797
16.7
7916
.656
lm02
12m
2009
9*V
MC
J053
129.
10-6
8092
3.84
2.62
1128
16.8
8816
.860
lm03
03n1
6128
VM
CJ0
5071
7.83
-665
037.
512.
6211
9617
.007
16.8
74lm
0020
l981
3V
MC
J052
741.
15-6
9162
0.23
2.63
1352
15.9
3115
.630
lm00
90n2
9324
VM
CJ0
5132
3.89
-692
249.
102.
6365
8415
.338
15.6
40lm
0543
n184
47*
VM
CJ0
4585
1.03
-710
310.
072.
6377
616
.640
16.6
31lm
0335
n240
71V
MC
J052
948.
04-6
7145
7.62
2.64
1403
16.0
8216
.054
lm02
00l6
405
VM
CJ0
5221
9.71
-675
029.
292.
6490
4215
.819
15.7
13lm
0465
l267
36V
MC
J052
811.
63-6
5525
4.69
2.65
4428
15.9
0615
.748
lm01
84k1
7447
VM
CJ0
5074
8.91
-682
734.
192.
6561
7316
.474
16.3
48lm
0216
l172
43V
MC
J053
007.
92-6
8585
8.46
2.65
7392
15.7
5915
.857
lm00
13l2
1404
VM
CJ0
5243
6.47
-694
011.
322.
6580
9716
.763
16.4
65lm
0037
n105
99*
VM
CJ0
5422
2.44
-701
941.
932.
6586
9816
.342
16.3
73lm
0173
m21
250*
VM
CJ0
5060
5.24
-680
656.
432.
6613
3416
.156
15.8
96lm
0230
l956
2V
MC
J054
514.
46-6
7520
6.17
2.66
2658
17.0
0716
.937
lm01
73n1
3333
VM
CJ0
5054
7.84
-681
339.
332.
6656
8416
.898
17.1
69lm
0195
m16
673*
VM
CJ0
5210
5.51
-682
636.
762.
6664
7616
.093
16.0
01lm
0127
l964
2V
MC
J045
234.
39-7
0190
7.80
2.66
9394
17.0
0016
.824
lm00
11m
2271
3V
MC
J052
529.
30-6
9105
5.92
2.67
4348
16.1
6215
.892
lm03
30n1
9300
*V
MC
J052
518.
11-6
6314
8.77
2.67
7262
17.2
7817
.587
211
lm01
86n8
773
VM
CJ0
5092
9.22
-685
502.
672.
6788
3215
.329
14.9
92lm
0092
m37
97*
VM
CJ0
5134
3.39
-692
603.
752.
6832
8817
.152
17.0
36lm
0093
m11
981
VM
CJ0
5174
1.69
-692
757.
612.
6873
716
.196
16.0
51lm
0571
n261
62V
MC
J052
234.
21-7
0450
0.11
2.68
743
16.2
1015
.959
lm02
91l5
438
VM
CJ0
4592
8.72
-662
549.
782.
7036
815
.546
15.6
71lm
0015
m15
054
VM
CJ0
5264
9.31
-694
957.
172.
7098
7216
.265
16.7
54lm
0012
n148
28V
MC
J052
148.
91-6
9383
5.05
2.71
287
15.5
6715
.834
lm01
03k1
0582
VM
CJ0
5075
0.07
-692
737.
892.
7130
0715
.903
15.8
76lm
0431
n154
33V
MC
J050
913.
18-6
5102
7.16
2.71
4038
16.8
0516
.792
lm01
85n2
2544
*V
MC
J051
245.
86-6
8415
0.78
2.71
8217
.001
17.1
62lm
0333
m22
120*
VM
CJ0
5284
8.66
-664
355.
072.
7203
3216
.086
15.8
81lm
0172
n625
3V
MC
J050
105.
81-6
8113
2.55
2.72
7663
15.6
1215
.428
lm02
06k2
5944
VM
CJ0
5231
5.68
-685
211.
412.
7314
615
.972
16.1
99lm
0091
m28
603*
VM
CJ0
5184
8.11
-691
234.
852.
7408
916
.697
16.6
28lm
0020
k168
26V
MC
J052
747.
85-6
9102
6.64
2.74
7223
15.4
8615
.124
lm02
05m
4021
VM
CJ0
5275
7.96
-682
221.
722.
7498
6616
.835
16.9
15lm
0294
n747
9V
MC
J045
806.
79-6
7090
8.39
2.75
026
16.2
3516
.142
lm02
04l1
8900
VM
CJ0
5220
8.66
-683
715.
492.
7545
0316
.978
17.0
82lm
0231
l120
15*
VM
CJ0
5480
9.96
-675
243.
962.
7548
2416
.644
16.6
20lm
0556
n173
86*
VM
CJ0
5025
3.20
-714
733.
122.
7559
9617
.677
17.7
53lm
0091
n214
52V
MC
J051
834.
35-6
9233
5.98
2.76
5244
16.8
5416
.585
lm05
41k2
0099
*V
MC
J045
457.
81-7
0344
6.63
2.76
8156
16.9
9816
.966
lm00
93l2
6030
VM
CJ0
5164
5.73
-694
131.
532.
7722
5716
.614
16.5
36lm
0025
k174
89V
MC
J053
135.
02-6
9510
8.99
2.77
3556
16.8
9616
.657
lm00
33k1
1425
VM
CJ0
5392
3.48
-692
808.
772.
7808
3515
.803
15.6
84lm
0427
k156
85V
MC
J050
206.
39-6
6043
4.80
2.79
1595
15.8
6615
.789
lm03
37k1
8241
VM
CJ0
5275
1.41
-672
544.
082.
7939
9515
.692
15.4
86lm
0580
m16
604*
VM
CJ0
5271
9.98
-703
307.
272.
7961
3416
.590
16.5
80lm
0466
l164
61*
VM
CJ0
5252
3.82
-661
403.
992.
8151
615
.526
15.8
00lm
0214
n174
17*
VM
CJ0
5313
8.66
-683
647.
522.
8161
0817
.576
17.5
60lm
0336
k706
5V
MC
J052
325.
82-6
7203
6.30
2.82
1258
16.3
3216
.027
lm01
91n4
635
VM
CJ0
5205
2.76
-675
151.
432.
8226
1116
.741
16.8
11lm
0106
l117
13V
MC
J050
338.
84-7
0195
7.81
2.82
7501
16.2
1615
.736
lm00
14m
9900
*V
MC
J052
133.
54-6
9484
2.47
2.83
114
16.8
7217
.343
lm02
04k9
178*
VM
CJ0
5223
0.17
-682
421.
932.
8392
7816
.141
16.1
87lm
0032
k156
60V
MC
J053
610.
74-6
9320
2.25
2.84
1496
14.9
0614
.629
lm01
95n5
472
VM
CJ0
5194
8.46
-683
204.
412.
8419
7216
.635
16.6
81lm
0581
l290
10V
MC
J053
028.
83-7
0460
1.15
2.84
3662
16.1
0316
.567
lm00
20n1
2840
*V
MC
J052
933.
20-6
9171
1.93
2.85
1276
16.7
9616
.744
lm00
34k1
2920
*V
MC
J053
615.
92-6
9501
2.08
2.85
2214
16.3
6116
.118
lm00
21k1
3770
VM
CJ0
5314
0.14
-690
758.
942.
8532
9215
.365
15.0
22
212
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0541
m10
971
VM
CJ0
4575
6.56
-703
035.
192.
8619
3416
.639
16.7
88lm
0031
k197
05V
MC
J054
049.
55-6
9130
5.78
2.86
7536
14.5
5414
.699
lm00
11n1
0445
*V
MC
J052
504.
33-6
9154
9.51
2.86
7908
15.9
9915
.903
lm04
24n2
3353
VM
CJ0
5002
3.14
-655
201.
052.
8693
1215
.226
14.9
45lm
0321
k150
88*
VM
CJ0
5205
1.31
-662
524.
782.
8764
5616
.913
16.8
83lm
0013
k297
88V
MC
J052
421.
11-6
9333
6.19
2.88
2388
15.3
1815
.740
lm00
31l2
1280
VM
CJ0
5400
3.22
-691
954.
742.
8824
8916
.016
15.9
54lm
0105
k312
40V
MC
J050
811.
48-6
9554
2.47
2.88
7854
16.9
3016
.912
lm05
41l1
7906
VM
CJ0
4552
5.52
-704
654.
222.
8955
7516
.706
16.6
54lm
0331
m17
723
VM
CJ0
5284
5.42
-662
139.
942.
8962
1216
.971
16.8
17lm
0103
k151
98V
MC
J050
815.
66-6
9290
4.84
2.89
9283
14.5
1615
.669
lm03
27m
5927
VM
CJ0
5221
4.03
-672
022.
412.
9117
5515
.845
15.7
50lm
0216
n159
95V
MC
J053
233.
12-6
8574
5.57
2.91
3514
14.7
3714
.755
lm03
23n7
828
VM
CJ0
5213
5.79
-664
750.
802.
9168
0116
.353
16.3
22lm
0024
m75
52V
MC
J053
046.
75-6
9475
9.25
2.91
7208
16.0
3315
.910
lm00
25k3
1765
VM
CJ0
5315
8.40
-695
532.
192.
9180
3916
.607
16.4
02lm
0300
k888
4V
MC
J050
301.
07-6
6182
4.94
2.92
1834
16.9
8616
.773
lm04
26n1
7949
VM
CJ0
5002
5.36
-661
036.
892.
9246
2816
.640
16.4
93lm
0303
m53
18V
MC
J050
741.
04-6
6373
7.41
2.92
6082
16.9
0417
.004
lm00
21k2
4967
VM
CJ0
5324
8.62
-691
204.
112.
9261
15.5
6815
.169
lm03
35l8
729
VM
CJ0
5271
9.81
-670
934.
722.
9316
1816
.321
16.2
33lm
0340
k226
02*
VM
CJ0
5313
1.67
-662
525.
782.
9402
8617
.639
17.5
66lm
0051
n154
68V
MC
J055
752.
51-6
9181
6.23
2.94
9872
16.9
1216
.939
lm03
44k1
3297
VM
CJ0
5310
4.94
-670
241.
962.
9503
2615
.950
15.6
44lm
0114
k269
29V
MC
J045
613.
03-6
9551
6.83
2.95
0903
16.0
2815
.847
lm02
30l9
767*
VM
CJ0
5442
8.71
-675
211.
902.
9537
9617
.370
17.2
04lm
0207
m16
357
VM
CJ0
5282
3.83
-684
818.
762.
9565
6715
.388
15.1
38lm
0101
k242
23*
VM
CJ0
5075
9.60
-691
211.
862.
9590
616
.432
16.0
86lm
0032
n105
70V
MC
J053
830.
23-6
9372
6.24
2.97
1654
15.6
5615
.666
lm00
90k3
504
VM
CJ0
5122
4.83
-690
443.
592.
9726
2115
.425
15.4
90lm
0335
k267
56V
MC
J052
800.
78-6
7065
5.56
2.97
543
16.3
4816
.169
lm02
94m
4825
VM
CJ0
4580
7.70
-665
858.
212.
9777
915
.299
15.1
18lm
0331
k237
17*
VM
CJ0
5270
9.79
-662
528.
282.
9901
4516
.373
16.2
56lm
0093
m17
914*
VM
CJ0
5175
1.12
-692
947.
463.
0111
3415
.903
15.7
81lm
0017
m23
847
VM
CJ0
5260
3.40
-701
513.
523.
0245
3516
.977
16.8
08lm
0033
k178
47*
VM
CJ0
5401
5.61
-693
028.
353.
0259
9815
.641
15.4
79lm
0541
n158
71V
MC
J045
733.
22-7
0441
6.94
3.02
721
16.5
9616
.370
lm00
21n5
306
VM
CJ0
5334
0.51
-691
353.
323.
0399
1614
.750
14.6
73lm
0191
n374
3V
MC
J052
008.
69-6
7511
4.37
3.05
3936
16.0
9916
.219
lm03
33k2
9474
VM
CJ0
5272
6.38
-664
635.
103.
0571
5115
.673
15.4
80lm
0426
n226
20*
VM
CJ0
5001
7.70
-661
245.
513.
0586
2616
.521
16.3
89
213
lm03
30m
5632
VM
CJ0
5255
8.56
-661
659.
313.
0614
4215
.631
15.5
78lm
0033
l242
96V
MC
J054
025.
06-6
9415
9.18
3.06
6509
15.2
7015
.317
lm00
22n1
4480
VM
CJ0
5301
6.06
-693
830.
083.
0682
7715
.906
15.9
36lm
0020
k189
27*
VM
CJ0
5281
6.59
-691
120.
993.
0817
6415
.820
15.5
23lm
0547
l643
4V
MC
J045
641.
99-7
1413
2.41
3.08
1798
15.8
6415
.847
lm01
25l2
5666
VM
CJ0
4523
8.51
-700
320.
933.
0880
9114
.810
14.8
79lm
0172
n244
68V
MC
J050
135.
42-6
8180
7.15
3.10
2677
16.2
8316
.284
lm00
95m
9501
VM
CJ0
5180
4.70
-694
818.
923.
1070
1914
.833
14.7
06lm
0346
m33
92V
MC
J053
225.
87-6
7192
5.35
3.11
3759
15.8
8515
.830
lm00
26m
1415
1V
MC
J053
043.
79-7
0112
4.46
3.11
5609
16.1
0516
.685
lm03
34n2
3519
VM
CJ0
5254
9.78
-671
525.
643.
1197
0115
.945
15.7
28lm
0340
m20
801
VM
CJ0
5321
5.66
-662
329.
933.
1206
8616
.735
16.7
75lm
0033
m31
96V
MC
J054
119.
07-6
9250
5.08
3.12
2574
15.3
3915
.190
lm02
07m
2758
8V
MC
J052
740.
43-6
8523
4.40
3.12
647
15.9
4915
.757
lm00
34m
1263
VM
CJ0
5383
6.03
-694
624.
123.
1345
5415
.950
16.1
01lm
0202
l153
11V
MC
J052
318.
13-6
8150
0.47
3.13
9857
15.7
0915
.474
lm00
24m
2426
4V
MC
J053
016.
91-6
9531
4.69
3.14
4057
15.8
1515
.893
lm05
80m
2004
7V
MC
J052
829.
08-7
0342
1.01
3.14
5045
15.9
8715
.912
lm03
33n1
6489
VM
CJ0
5293
8.72
-665
051.
633.
1610
615
.112
14.9
87lm
0333
n104
85V
MC
J052
850.
66-6
6484
6.84
3.16
2796
14.9
3514
.720
lm03
31n1
3474
VM
CJ0
5295
1.96
-663
507.
503.
1636
3616
.222
16.0
38lm
0214
n271
17V
MC
J053
047.
68-6
8402
5.42
3.17
278
15.0
3714
.983
lm00
92k1
7584
*V
MC
J051
235.
40-6
9322
6.84
3.19
2096
16.1
5516
.001
lm05
43m
3009
3V
MC
J045
719.
93-7
0581
9.96
3.19
3725
15.7
2915
.769
lm00
90l7
215*
VM
CJ0
5121
8.08
-691
516.
423.
1944
917
.271
16.3
60lm
0240
m16
931
VM
CJ0
5531
7.48
-674
553.
673.
2095
9415
.041
15.8
11lm
0093
k230
75V
MC
J051
616.
67-6
9312
6.91
3.21
4621
15.7
7815
.580
lm00
92m
1660
8V
MC
J051
355.
15-6
9320
1.13
3.21
9523
14.4
2914
.199
lm05
83l2
8540
VM
CJ0
5304
0.13
-710
647.
283.
2210
615
.039
15.5
96lm
0012
k238
09V
MC
J052
035.
75-6
9341
5.24
3.22
4639
16.6
2216
.254
lm01
15n1
3901
VM
CJ0
5013
7.80
-695
852.
433.
2249
2514
.790
14.6
50lm
0455
k235
32V
MC
J052
144.
72-6
5424
3.91
3.23
3372
15.9
2115
.826
lm02
21n2
2693
VM
CJ0
5424
2.79
-675
631.
743.
2345
1816
.252
16.1
85lm
0305
k407
2*V
MC
J050
558.
59-6
6584
1.61
3.23
9846
17.3
3117
.221
lm03
44k1
9755
VM
CJ0
5313
3.34
-670
519.
393.
2409
5114
.726
14.4
67lm
0214
n122
07V
MC
J053
144.
95-6
8345
2.55
3.25
2969
16.1
1616
.131
lm02
07m
8280
VM
CJ0
5280
0.48
-684
524.
603.
2569
0416
.553
16.9
88lm
0106
k149
21V
MC
J050
325.
22-7
0115
7.08
3.26
1387
15.9
5815
.829
lm02
07n2
2625
VM
CJ0
5275
5.80
-690
049.
783.
2644
9215
.554
15.7
64lm
0435
k200
23V
MC
J050
901.
35-6
5410
5.20
3.28
1595
16.9
8516
.844
lm00
13m
1452
0*V
MC
J052
516.
61-6
9290
3.95
3.28
8232
16.5
3416
.120
214
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0090
n128
80*
VM
CJ0
5130
3.43
-691
712.
003.
2893
3216
.954
16.6
87lm
0114
n174
44V
MC
J045
721.
21-7
0002
1.41
3.29
6076
16.0
4816
.019
lm02
00l1
8257
VM
CJ0
5220
2.22
-675
537.
823.
2969
4914
.592
14.4
18lm
0366
n990
3V
MC
J054
712.
45-6
7311
8.21
3.30
0117
16.4
9616
.406
lm04
36l1
9007
VM
CJ0
5050
7.38
-661
138.
423.
3011
2315
.346
15.2
06lm
0091
n235
08V
MC
J051
706.
93-6
9201
3.17
3.30
8983
15.6
7515
.489
lm03
35m
1168
3V
MC
J052
837.
35-6
7011
8.46
3.31
1557
15.6
8915
.450
lm01
93n1
4440
*V
MC
J052
107.
83-6
8135
6.02
3.31
8844
16.4
7216
.612
lm02
96n1
1158
VM
CJ0
4571
2.12
-673
143.
073.
3593
7716
.442
16.3
02lm
0335
n983
4*V
MC
J052
956.
56-6
7093
6.23
3.36
2948
17.0
1116
.766
lm05
41n1
3040
VM
CJ0
4582
2.81
-704
242.
903.
3671
816
.654
16.6
84lm
0023
k426
5V
MC
J053
225.
15-6
9253
7.33
3.37
023
15.6
1815
.399
lm02
16m
2662
4*V
MC
J053
112.
47-6
8522
1.51
3.37
1126
17.1
7017
.271
lm03
66m
8525
*V
MC
J054
630.
32-6
7213
3.22
3.37
1884
16.9
8316
.919
lm03
42k1
7321
VM
CJ0
5303
9.31
-664
439.
863.
3738
0815
.640
15.3
98lm
0180
l204
43*
VM
CJ0
5082
1.43
-675
607.
123.
3835
0216
.780
16.5
99lm
0093
n338
08*
VM
CJ0
5172
0.98
-694
350.
273.
3909
8416
.918
16.8
35lm
0365
n238
64V
MC
J055
031.
50-6
7154
8.89
3.40
0307
16.7
6816
.732
lm03
33n1
8392
VM
CJ0
5292
5.08
-665
135.
833.
4040
9916
.590
16.6
28lm
0030
l133
51V
MC
J053
540.
66-6
9180
1.62
3.40
8736
14.5
4514
.374
lm03
31m
2354
8V
MC
J052
830.
64-6
6240
0.92
3.41
2884
15.4
4115
.211
lm00
30l4
784
VM
CJ0
5362
7.18
-691
415.
463.
4134
2115
.279
15.6
49lm
0584
n181
93V
MC
J052
821.
01-7
1244
3.87
3.42
6518
14.9
7614
.891
lm04
66n1
3702
VM
CJ0
5260
8.98
-660
900.
113.
4327
3413
.797
14.3
97lm
0105
l704
7V
MC
J050
801.
50-6
9583
5.42
3.44
2404
16.9
4216
.749
lm04
66l1
8501
VM
CJ0
5250
1.99
-661
122.
283.
4450
1215
.658
15.8
86lm
0187
l139
41*
VM
CJ0
5115
9.43
-685
701.
733.
4477
6216
.611
17.1
79lm
0541
n183
20V
MC
J045
900.
32-7
0452
3.67
3.45
9966
16.6
6616
.520
lm00
33k4
809
VM
CJ0
5393
4.84
-692
539.
503.
4687
3216
.467
16.6
71lm
0221
n792
8V
MC
J054
335.
09-6
7504
1.08
3.46
8802
15.3
2215
.206
lm03
21m
6695
VM
CJ0
5220
3.88
-661
655.
513.
4697
216
.019
15.9
66lm
0202
l242
07V
MC
J052
237.
66-6
8182
5.71
3.47
2186
16.7
6616
.764
lm03
44m
8000
VM
CJ0
5323
3.23
-670
029.
723.
4962
8815
.544
15.3
25lm
0195
m24
877
VM
CJ0
5201
1.82
-682
937.
053.
5080
0816
.524
16.6
70lm
0184
l159
97V
MC
J050
807.
87-6
8361
9.94
3.50
9246
15.7
6215
.635
lm01
80l2
4836
VM
CJ0
5070
5.32
-675
755.
643.
5130
1715
.436
15.2
47lm
0024
k235
11*
VM
CJ0
5262
5.67
-694
617.
083.
5223
5617
.061
16.1
23lm
0091
k144
79V
MC
J051
536.
44-6
9082
1.97
3.52
4759
16.0
6816
.214
lm00
21n2
9435
VM
CJ0
5343
7.12
-692
204.
363.
5317
3515
.672
15.3
27lm
0013
n300
08V
MC
J052
508.
84-6
9424
5.66
3.53
8905
15.9
6315
.695
lm03
37k2
3342
VM
CJ0
5273
3.73
-672
754.
183.
5434
4115
.154
14.9
60
215
lm03
05m
2705
2V
MC
J050
719.
25-6
7064
9.37
3.54
5493
15.9
9115
.820
lm03
03k1
3861
*V
MC
J050
703.
27-6
6404
3.72
3.54
569
16.9
8617
.131
lm00
95n3
0847
VM
CJ0
5185
2.99
-700
418.
303.
5467
2216
.410
16.5
56lm
0556
k565
2V
MC
J050
036.
62-7
1313
0.23
3.55
3122
16.5
7516
.575
lm00
90m
4479
VM
CJ0
5133
1.24
-690
449.
803.
5582
3616
.448
16.3
60lm
0230
k587
2*V
MC
J054
413.
46-6
7493
3.88
3.56
1718
16.7
9416
.898
lm03
44l2
1596
VM
CJ0
5311
1.09
-671
521.
003.
5840
8116
.846
16.9
02lm
0323
n118
23*
VM
CJ0
5222
4.77
-664
911.
743.
5997
1416
.607
16.6
46lm
0340
l679
1V
MC
J053
039.
12-6
6270
2.79
3.61
2113
16.7
2416
.687
lm03
66l7
734
VM
CJ0
5445
3.76
-673
014.
683.
6135
4216
.574
16.6
12lm
0163
l248
56V
MC
J045
631.
69-6
8175
1.39
3.61
8347
16.3
3916
.260
lm00
15n3
0492
VM
CJ0
5250
9.30
-700
422.
453.
6255
1316
.099
16.2
42lm
0093
k274
61V
MC
J051
649.
40-6
9324
6.00
3.62
8299
15.7
0615
.420
lm00
91l2
5158
VM
CJ0
5162
6.57
-692
032.
773.
6343
1115
.230
14.9
84lm
0013
m22
363
VM
CJ0
5252
2.38
-693
138.
533.
6461
1116
.116
16.5
30lm
0184
l495
7*V
MC
J050
738.
34-6
8322
1.67
3.65
273
15.5
9716
.379
lm03
03n1
7856
*V
MC
J050
741.
74-6
6511
0.66
3.65
542
16.5
5016
.482
lm01
84k1
3409
VM
CJ0
5064
5.59
-682
609.
233.
6592
4916
.052
16.0
11lm
0207
m69
63*
VM
CJ0
5272
1.82
-684
500.
863.
6773
3215
.420
15.2
66lm
0033
n188
86V
MC
J054
145.
08-6
9400
4.48
3.69
4692
14.9
3514
.661
lm03
44l1
9313
VM
CJ0
5305
1.88
-671
425.
063.
6959
3515
.400
15.1
45lm
0013
n866
1V
MC
J052
514.
83-6
9361
2.54
3.71
4526
16.1
4915
.821
lm00
33m
1706
3V
MC
J054
113.
76-6
9301
0.14
3.71
8525
14.9
0914
.781
lm03
31n1
614
VM
CJ0
5283
6.11
-662
543.
993.
7206
916
.695
16.6
51lm
0125
n234
49V
MC
J045
341.
21-7
0022
6.31
3.73
8714
15.2
4915
.100
lm00
13n3
2504
VM
CJ0
5250
6.88
-694
331.
873.
7450
0816
.173
16.1
01lm
0291
l489
1V
MC
J050
000.
09-6
6253
4.19
3.75
1829
15.4
5015
.303
lm00
27k3
823*
VM
CJ0
5312
6.76
-700
813.
183.
7614
1416
.125
16.0
18lm
0101
n251
68V
MC
J051
028.
64-6
9204
7.85
3.77
3408
15.9
9215
.667
lm02
07k1
6837
VM
CJ0
5265
6.27
-684
828.
763.
7750
8416
.072
15.7
41lm
0092
m24
157
VM
CJ0
5130
6.10
-693
434.
503.
7795
2815
.978
15.7
15lm
0214
n861
4V
MC
J053
152.
56-6
8333
1.43
3.78
5845
16.5
1616
.487
lm03
33k4
914
VM
CJ0
5271
2.99
-663
741.
463.
7902
6915
.647
15.5
05lm
0020
m22
505
VM
CJ0
5302
8.96
-691
138.
423.
7916
9115
.516
15.4
47lm
0030
l159
04V
MC
J053
638.
60-6
9191
3.02
3.79
7121
14.9
6915
.126
lm05
50m
5212
VM
CJ0
5023
0.64
-702
903.
583.
8010
3915
.647
15.7
98lm
0257
l893
1V
MC
J060
425.
47-6
8552
8.09
3.81
0748
15.6
3115
.492
lm05
83l2
8572
VM
CJ0
5292
6.46
-710
653.
283.
8228
9516
.581
16.5
15lm
0125
k810
6V
MC
J045
117.
66-6
9480
8.09
3.84
3898
15.8
1115
.761
lm03
67l1
3331
VM
CJ0
5485
8.00
-673
334.
623.
8467
0416
.475
16.4
75lm
0090
n309
09V
MC
J051
317.
10-6
9232
0.48
3.85
2097
15.9
2315
.519
216
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0030
l110
56V
MC
J053
648.
74-6
9165
9.46
3.85
3558
15.4
7715
.185
lm00
90k1
0170
*V
MC
J051
229.
86-6
9071
6.00
3.85
4796
16.0
2616
.316
lm00
20k1
5581
VM
CJ0
5281
6.01
-690
954.
653.
8639
5515
.043
14.7
91lm
0026
n702
7V
MC
J052
926.
19-7
0181
0.40
3.87
0485
15.2
1316
.019
lm01
17m
1273
0V
MC
J050
231.
16-7
0105
6.10
3.87
3811
16.2
4116
.249
lm00
10l2
3506
VM
CJ0
5202
0.04
-692
144.
273.
9040
7715
.990
15.9
94lm
0187
m99
85V
MC
J051
239.
82-6
8460
3.34
3.94
5319
16.5
8816
.573
lm02
00l6
074
VM
CJ0
5221
8.76
-675
020.
513.
9504
7816
.068
15.8
23lm
0091
m37
97*
VM
CJ0
5174
7.87
-690
416.
053.
9545
16.6
9916
.741
lm03
31k2
1866
VM
CJ0
5272
5.35
-662
334.
393.
9591
1316
.789
16.6
34lm
0015
k865
8V
MC
J052
339.
15-6
9481
6.29
3.95
9962
15.5
2315
.966
lm03
64l1
4193
VM
CJ0
5443
8.11
-671
231.
413.
9599
7616
.415
16.4
62lm
0331
l260
42V
MC
J052
756.
25-6
6341
2.32
3.96
9029
15.8
9415
.772
lm03
00m
2201
9V
MC
J050
349.
13-6
6233
2.69
3.98
6529
16.6
6216
.518
lm01
84n2
6760
VM
CJ0
5095
7.57
-683
929.
834.
0224
2815
.046
15.1
60lm
0012
n483
2V
MC
J052
107.
20-6
9352
5.30
4.02
7903
16.4
7716
.378
lm00
21l4
530*
VM
CJ0
5312
8.69
-691
354.
954.
0375
3914
.860
14.7
66lm
0600
k250
18V
MC
J054
220.
50-7
0373
6.59
4.04
6607
14.7
9714
.770
lm01
01k2
3784
VM
CJ0
5082
6.75
-691
200.
024.
0694
8315
.601
15.4
68lm
0337
k108
47V
MC
J052
804.
62-6
7224
1.05
4.11
5728
14.8
3214
.687
lm01
70n1
2305
VM
CJ0
5020
5.40
-675
254.
894.
1164
8615
.697
15.6
63lm
0206
n263
79V
MC
J052
352.
88-6
9013
8.35
4.12
7665
14.5
6114
.682
lm03
44l2
1656
VM
CJ0
5310
9.29
-671
522.
294.
1641
5615
.602
15.4
87lm
0101
k179
68V
MC
J050
717.
92-6
9095
4.16
4.17
6462
15.3
1315
.063
lm04
66l1
6077
VM
CJ0
5252
2.27
-661
009.
944.
1790
9114
.002
14.1
64lm
0020
k869
1V
MC
J052
823.
88-6
9070
3.31
4.17
9714
.826
14.6
03lm
0344
m20
206
VM
CJ0
5314
6.63
-670
518.
414.
1814
1215
.354
15.1
62lm
0125
n606
8V
MC
J045
320.
39-6
9561
2.33
4.18
7756
15.8
9215
.792
lm01
03k2
6311
VM
CJ0
5081
0.19
-693
235.
804.
2031
1116
.204
16.0
97lm
0366
l168
62V
MC
J054
451.
73-6
7343
3.15
4.23
2527
15.7
5815
.798
lm03
46k2
3825
VM
CJ0
5310
8.79
-672
902.
674.
2492
9915
.143
14.8
94lm
0466
n219
59V
MC
J052
603.
19-6
6124
7.50
4.27
3267
16.1
5816
.274
lm03
76m
4773
VM
CJ0
5535
5.50
-671
952.
504.
3060
2615
.938
15.9
61lm
0125
l665
2V
MC
J045
226.
31-6
9563
1.61
4.31
3464
15.6
4415
.630
lm02
97n1
4819
VM
CJ0
5005
0.61
-673
332.
284.
3186
3815
.615
15.5
55lm
0467
k182
22V
MC
J052
835.
72-6
6015
5.83
4.32
0224
16.0
2716
.003
lm01
87m
1796
7V
MC
J051
332.
00-6
8484
8.77
4.32
3013
16.2
5516
.175
lm04
67n1
7850
VM
CJ0
5294
3.72
-661
124.
344.
3240
3516
.022
15.9
24lm
0205
n175
50V
MC
J052
744.
16-6
8360
1.02
4.33
2041
16.6
0416
.557
lm03
31k2
2811
VM
CJ0
5271
4.17
-662
358.
984.
3376
3315
.095
14.9
17lm
0091
n322
74V
MC
J051
717.
14-6
9225
8.26
4.33
9628
15.6
7415
.644
217
lm03
37k2
5005
VM
CJ0
5270
1.99
-672
838.
244.
4088
2215
.134
14.9
49lm
0093
m11
955
VM
CJ0
5172
9.97
-692
758.
494.
4227
9615
.980
15.8
27lm
0034
m46
02*
VM
CJ0
5383
9.39
-694
814.
134.
4548
9416
.415
16.6
44lm
0197
m20
835
VM
CJ0
5194
6.37
-685
008.
914.
4884
1815
.997
15.9
68lm
0090
n200
34V
MC
J051
302.
18-6
9193
9.75
4.50
2363
15.7
0515
.567
lm00
21l1
5985
VM
CJ0
5312
8.68
-691
751.
774.
5027
7914
.658
14.4
62lm
0030
l901
4V
MC
J053
525.
69-6
9160
5.91
4.52
3622
15.1
6515
.075
lm02
07m
1144
6V
MC
J052
835.
52-6
8462
8.74
4.52
6578
14.2
4514
.121
lm00
21l1
5606
VM
CJ0
5311
2.20
-691
745.
074.
5575
8115
.246
14.9
22lm
0091
l145
77V
MC
J051
540.
18-6
9171
4.02
4.56
6657
15.5
2316
.114
lm01
14k1
9051
VM
CJ0
4555
2.65
-695
210.
474.
5774
7115
.389
15.1
17lm
0020
n196
15V
MC
J053
041.
78-6
9192
8.06
4.58
5353
13.9
5513
.838
lm01
87m
1149
6V
MC
J051
333.
04-6
8462
9.11
4.59
1479
16.1
5616
.186
lm00
33m
2170
0V
MC
J054
141.
63-6
9314
8.16
4.61
3339
15.1
7215
.123
lm00
25m
3093
6V
MC
J053
318.
56-6
9550
2.89
4.63
6845
15.9
9916
.114
lm05
50k1
1523
VM
CJ0
5010
0.77
-703
145.
344.
6650
916
.117
16.2
13lm
0185
n116
36V
MC
J051
305.
86-6
8340
1.04
4.67
3342
16.0
9916
.201
lm00
93m
3076
8V
MC
J051
721.
64-6
9335
2.95
4.72
1156
16.4
3516
.301
lm03
33n6
568
VM
CJ0
5290
0.40
-664
718.
784.
7708
5415
.162
15.0
57lm
0543
m81
69V
MC
J045
811.
23-7
0502
8.09
4.77
7862
15.8
3215
.888
lm01
80k1
6760
VM
CJ0
5071
5.05
-674
517.
104.
7842
8815
.624
15.3
70lm
0427
l127
67V
MC
J050
105.
30-6
6092
0.15
4.80
5932
16.1
9516
.063
lm00
31n6
676
VM
CJ0
5415
1.77
-691
422.
824.
8534
3115
.530
15.4
14lm
0127
k131
32V
MC
J045
234.
68-7
0111
8.42
4.89
2616
15.9
6815
.920
lm02
16l1
6590
VM
CJ0
5304
4.33
-685
840.
574.
9431
7116
.073
15.9
81lm
0476
k561
0V
MC
J053
058.
40-6
5562
8.62
4.95
1673
16.0
0316
.098
lm03
44l1
2773
VM
CJ0
5304
0.75
-671
143.
774.
9524
8715
.649
15.4
17lm
0185
l237
72V
MC
J051
108.
01-6
8381
2.13
4.97
0047
15.7
6515
.602
lm00
15m
2679
3V
MC
J052
620.
48-6
9534
1.86
4.97
0604
16.0
8315
.836
lm04
27k1
3855
VM
CJ0
5021
3.54
-660
022.
155.
0164
6915
.733
15.7
72lm
0011
k236
33V
MC
J052
430.
51-6
9112
1.03
5.08
3128
15.6
4215
.955
lm00
93k3
0805
VM
CJ0
5164
4.81
-693
349.
665.
0857
6816
.052
16.0
90lm
0012
n221
51V
MC
J052
134.
93-6
9405
7.58
5.11
1026
16.5
0516
.414
lm05
40m
1358
7V
MC
J045
352.
25-7
0320
2.59
5.11
8075
16.1
5516
.058
lm00
21l3
0770
VM
CJ0
5321
4.56
-692
239.
465.
1717
9315
.758
15.3
42lm
0216
k962
7V
MC
J053
025.
55-6
8461
0.42
5.20
3106
14.3
5214
.173
lm00
33k7
569
VM
CJ0
5404
9.56
-692
636.
295.
2691
15.3
2415
.254
lm03
33l1
5404
VM
CJ0
5273
5.95
-665
047.
685.
2722
215
.500
15.4
82lm
0612
l101
94V
MC
J055
112.
35-7
1014
6.54
5.27
9445
16.3
0216
.442
lm03
30k4
290
VM
CJ0
5235
3.25
-661
622.
885.
2819
216
.228
16.2
48lm
0116
k210
77V
MC
J045
641.
08-7
0143
9.31
5.30
968
15.5
0215
.397
218
APPENDIX A. PROPERTIES OF THE “HOT” ECLIPSING BINARIES IN THE LMClm
0207
k170
59V
MC
J052
635.
55-6
8483
5.76
5.31
1128
15.9
6116
.102
lm00
20m
1635
9V
MC
J052
952.
31-6
9092
2.56
5.33
5197
15.0
6614
.762
lm00
33m
6304
VM
CJ0
5405
6.63
-692
618.
255.
3695
4515
.562
15.4
29lm
0031
l229
87V
MC
J054
047.
30-6
9202
8.25
5.41
3977
14.1
5714
.029
lm02
16n1
0589
VM
CJ0
5310
0.88
-685
529.
855.
4485
815
.022
14.8
66lm
0092
m18
774
VM
CJ0
5134
1.27
-693
245.
365.
4573
0915
.767
15.5
17lm
0114
k216
90V
MC
J045
613.
93-6
9531
2.52
5.50
7995
15.3
7115
.193
lm01
86m
2344
6V
MC
J050
844.
21-6
8512
4.83
5.53
4274
16.4
3616
.435
lm03
46l1
3438
VM
CJ0
5311
6.19
-673
254.
595.
5703
5214
.541
14.3
55lm
0207
n152
51V
MC
J052
744.
32-6
8574
0.53
5.59
8846
15.6
5815
.461
lm00
93k2
6732
VM
CJ0
5164
4.41
-693
233.
125.
6034
4715
.713
15.6
84lm
0021
k212
80V
MC
J053
102.
31-6
9104
9.89
5.67
1847
14.8
2415
.352
lm00
21m
2641
1*V
MC
J053
259.
22-6
9121
6.78
5.70
8342
15.2
0114
.868
lm05
43l2
8153
VM
CJ0
4552
8.97
-710
707.
805.
7365
9515
.668
15.8
66lm
0127
l106
08V
MC
J045
249.
58-7
0193
1.94
5.78
278
15.7
8816
.007
lm01
05l5
842
VM
CJ0
5075
5.21
-695
755.
575.
7858
116
.274
15.9
34lm
0091
n262
47V
MC
J051
736.
67-6
9210
2.17
5.81
3256
15.3
0315
.194
lm04
66n1
1710
VM
CJ0
5263
4.25
-660
805.
775.
8226
5315
.351
15.2
74lm
0013
m20
776
VM
CJ0
5254
6.29
-693
104.
045.
8744
2615
.564
16.0
89lm
0010
l242
42V
MC
J051
935.
67-6
9215
9.86
5.94
1613
15.3
2515
.144
lm00
21k1
4832
VM
CJ0
5322
6.44
-690
819.
305.
9732
4315
.421
15.1
77lm
0427
n162
72*
VM
CJ0
5040
7.60
-661
055.
516.
0037
415
.241
15.1
55lm
0171
n545
1V
MC
J050
442.
87-6
7504
3.17
6.06
5706
14.8
3114
.727
lm01
01k2
2147
VM
CJ0
5073
2.18
-691
127.
036.
2082
4114
.721
14.5
42lm
0020
n629
4*V
MC
J053
022.
13-6
9145
2.06
6.22
9258
14.8
1214
.546
lm00
20n2
1732
*V
MC
J053
039.
25-6
9201
2.07
6.27
1038
16.5
2816
.509
lm04
66n6
181
VM
CJ0
5261
5.95
-660
530.
756.
3327
2315
.585
15.6
01lm
0173
n168
94V
MC
J050
537.
05-6
8145
3.66
6.34
7941
15.0
2014
.901
lm05
40k1
6892
*V
MC
J045
056.
98-7
0333
9.68
6.37
983
16.3
5216
.485
lm03
44k2
2660
VM
CJ0
5303
2.44
-670
632.
496.
4348
2815
.086
15.0
07lm
0303
k235
99V
MC
J050
617.
31-6
6441
4.50
6.46
3085
15.4
6015
.470
lm01
94n2
5484
VM
CJ0
5160
4.83
-683
921.
276.
4734
6515
.244
15.2
72lm
0090
k150
89*
VM
CJ0
5120
0.84
-690
905.
166.
5169
416
.594
16.2
93lm
0091
n319
44*
VM
CJ0
5173
9.56
-692
249.
576.
5175
316
.252
16.4
47lm
0346
n175
67V
MC
J053
156.
59-6
7350
1.72
6.53
2332
14.2
1214
.094
lm00
35m
2307
9V
MC
J054
222.
53-6
9530
5.37
6.56
9401
15.5
7815
.541
lm04
57l1
3469
VM
CJ0
5220
6.87
-660
931.
676.
6408
7115
.167
15.0
66lm
0335
n230
69V
MC
J052
956.
24-6
7143
3.05
6.89
8566
16.0
1016
.148
lm03
35n2
5477
*V
MC
J052
908.
36-6
7171
8.38
7.11
7324
14.6
9514
.756
lm02
14n1
4689
*V
MC
J053
134.
55-6
8354
8.30
7.15
0098
14.5
6615
.083
lm03
67m
1450
4*V
MC
J055
025.
93-6
7241
8.38
7.17
7252
16.8
0916
.904
219
lm04
27n1
2122
VM
CJ0
5032
7.76
-660
859.
757.
1940
3315
.733
15.7
11lm
0093
k525
3*V
MC
J051
553.
21-6
9255
7.89
7.28
4388
15.1
9915
.312
lm05
85l5
842
VM
CJ0
5310
7.72
-712
008.
047.
2862
9614
.828
14.8
61lm
0033
m20
529
VM
CJ0
5415
3.44
-693
121.
057.
4647
7814
.263
14.1
85lm
0014
k729
9V
MC
J052
042.
42-6
9475
5.97
7.53
6747
15.6
7815
.706
lm04
27k7
505*
VM
CJ0
5014
2.67
-655
734.
137.
6844
4615
.468
15.3
73lm
0435
m12
381
VM
CJ0
5101
3.60
-653
740.
017.
6965
5115
.718
15.8
74lm
0180
n931
6V
MC
J050
830.
82-6
7554
6.93
7.75
4096
15.3
4215
.292
lm00
33n1
2413
VM
CJ0
5410
4.81
-693
749.
227.
9421
2614
.854
14.9
63lm
0020
k102
87V
MC
J052
745.
76-6
9074
2.63
8.46
3039
14.6
7814
.503
lm04
67k1
1917
*V
MC
J052
821.
82-6
5591
4.77
8.46
4606
15.1
8815
.062
lm00
24m
1498
VM
CJ0
5291
1.89
-694
606.
178.
4859
4114
.973
14.8
83lm
0033
m59
60V
MC
J054
112.
57-6
9260
8.68
8.58
3074
13.8
6213
.746
lm05
41l9
275*
VM
CJ0
4553
6.25
-704
042.
588.
8500
9816
.362
16.4
62lm
0173
m17
717
VM
CJ0
5061
0.62
-680
543.
318.
8565
3713
.349
13.4
92lm
0191
n324
6*V
MC
J052
030.
06-6
7504
7.48
14.6
4502
814
.983
15.3
39lm
0173
n321
62*
VM
CJ0
5055
6.86
-682
003.
3821
.041
492
12.7
3414
.658
Tabl
eA
.2:
Prop
ertie
sof
999
HEB
sin
the
LMC
,whi
chha
vea
coun
terp
art
inth
eV
MC
cata
logu
e(C
olum
n1:
ERO
S-2
iden
tifica
tion
ofth
est
ar;
Col
umn
2:V
MC
iden
tifica
tion;
Col
umn
3:Pe
riod
from
the
ERO
S-2
cata
logu
e(∗
-St
ars
for
whi
cha
new
perio
dw
asde
-riv
edin
this
stud
y.Se
ete
xtfo
rthe
deta
ils.);
Col
umn
4:K
sm
agni
tude
atm
axim
umlig
ht;
Col
umn
5:R
EROS
mag
nitu
deat
max
imum
light
).
220
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