R. Hudec, F. Munz, J. R. Hudec, F. Munz, J. ŠŠtrobltrobl, P. , P. KubánekKubánek, P. Sobotka, R. Urban, P. Sobotka, R. Urban

Astronomical Institute, Academy of SciencesAstronomical Institute, Academy of Sciences251 65 Ondrejov, Czech Republic251 65 Ondrejov, Czech Republic

&&ISDC, Versoix, SwitzerlandISDC, Versoix, Switzerland

IBWS Oct 25-28, 2006IBWS Oct 25-28, 2006

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Identification of INTEGRAL Sources Identification of INTEGRAL Sources with Astronomical Archival Plateswith Astronomical Archival Plates

((and by CCD imagingand by CCD imaging))

Identification of Sources Only a fraction of 209 sources seen by INTEGRAL are either known

sources or have been identified and classified already. From the 56 newly by INTEGRAL detected sources (IGR sources),

only ~ 20% have already firm classification, mostly with Cataclysmic variables (CVs), AGN, High Mass X-ray Binaries, Low Mass X-ray Binaries, Black Hole Candidates, and Anomalous X-ray Pulsars (Bird et al. 2006).

One of the methods applied in the past is the identification by optical spectroscopy, which proved recently some new and interesting identification of INTEGRAL gamma-ray sources such as newly detected symbiotic and cataclysmic variables (e.g. Masetti et al., 2005a, 2005, Wheatley et al., 2005).

Limitations of Recent Method Although successful, this method has some limitations.

it can be hardly applied for particular types of transients and recurrent transients.

it requires access to dedicated large aperture telescopes and spectrographs.

it can be laborious in the case of large error box and crowded field.

in some specific cases, only the spectral information alone is not enough for reliable classification of the objects.

The alternative method

We propose an alternative method how to identify the still non-classified INTEGRAL gamma ray sources and newly detected INTEGRAL sources in the future (and of other high energy satellites).

This method is based on the fact that (1) many of gamma-ray sources identified and classified so far do have optical counterparts, in many cases brighter than mag 18, (2) a significant fraction of these sources is variable both in gamma-rays as well as in optical wavelengths, and (3) they are in the fields densely covered by archival optical observations covering typically years to tens of years.

The results can be used also to confirm the classification proposed by spectroscopy and to provide additional details for better physical understanding of the sources.

B magnitudy

1% 13%

40%38%

8% 1

2

3

4

5

V magnitudy

1% 17%

43%

34%

5% 1

2

3

4

5

Legend - B1 = 2,29 - 52 = 5 -103 = 10 - 154 = 15 - 205 = 20 - 23

Legend - V1 = 2,39 - 52 = 5 -103 = 10 - 154 = 15 - 205 = 20 - 21

Optical B and V magnitudes of optically identified INTEGRAL Optical B and V magnitudes of optically identified INTEGRAL gamma-ray sources … most are brighter than mag 20, and gamma-ray sources … most are brighter than mag 20, and more than halfmore than half are brighter are brighter than mag 15 than mag 15

It is not very clear at the moment whether the fact that It is not very clear at the moment whether the fact that most of the identified sources are brighter than mag 15-20 most of the identified sources are brighter than mag 15-20 is due to the fact thatis due to the fact that::

•The non-identified sources are The non-identified sources are optically optically fainter than mag 20fainter than mag 20

oror

•They are brighter than mag 20 but remain non-identified because of They are brighter than mag 20 but remain non-identified because of lack of observational datalack of observational data/identification efforts. The recent /identification efforts. The recent identifications of CVs and SSs by Masetti et al., 2005, 2006, indicate identifications of CVs and SSs by Masetti et al., 2005, 2006, indicate that at least for some fraction of the sources this is may be true.that at least for some fraction of the sources this is may be true.

Surely, the selection effect plays a role since so far, the mean-class Surely, the selection effect plays a role since so far, the mean-class telescopes have been used to identify the sourcestelescopes have been used to identify the sources

Archival sky patrol platesArchival sky patrol platesThere are more than 3 millions archival plates in the world, lim mag up to 23, > 5 x 5 deg in most cases

Suitable for dense long-term photometry (up to 100 years, up to 2000 points, up to 23 mag)

Suitable to detect rare events - years od CONTINUOUS monitoring easily possible

Use of scanners, powerful computers and innovative software allows the effective data extraction and evaluation for the first time

Various types of astronomical plates (digitised)

automated analyses with novel algorithms - task mainly for informatics students

Spectral image Direct ImageMultiple exposure

Suitable DatabasesSuitable Databases for for INTEGRALINTEGRAL

The Sonneberg Field Patrol and Leiden/Johannesburg Franklin Adams Plates represent suitable database for identification and analysis of INTEGRAL sources

They both provide numerous data for regions along the Galactic Plane and in the Galactic center

Sonneberg Field patrolSonneberg Field patrol

Northern regions along the Galactic Plane (but also other fields) covered by numerous (typically 50…500) astrograph plates. Typical Field of View (FOV) is 10 x 10 deg and the typical limiting magnitude is B 17.

In exceptional cases, also low-dispersion spectral plates are available

Leiden/Johannesburg Franklin Leiden/Johannesburg Franklin Adams PlatesAdams Plates

These plates were taken in Johannesburg by the high quality Franklin Adams refractor (Taylor, 1904) in years 1923-1952 within the project originated by Prof. E. Hertzsprung and are located in Leiden.

The plates cover selected fields along the southern Galactic plane as well as the Galactic centre.

The typical number of plates per field is 300…400, FOV is 10 x 10 deg and limiting magnitude 17.

UKSTU PlatesUKSTU Plates (ROE, UK) (ROE, UK) faint limits, mag 19 - 23 FOV 40 sq. degrees various colors/filters spectral plates down to

mag 18 18 000 plates over 30

years Unfortunately end of

operation in 2001

The deepest astronomical The deepest astronomical plates in the worldplates in the world

Obloha.jpg

Digitized Schmidt plate, TLS Tautenburg, lim mag 20, field M92. Newly detected variable objects with light amplitude > 2 mag are indicated. Example of the use of the powerful computer and novel dedicated software on digitised plates.

Analogous study can be also performed by CCD Analogous study can be also performed by CCD imaging & monitoring.imaging & monitoring.

On CCD images separated in time by weeks to years, the variable On CCD images separated in time by weeks to years, the variable objects can be easily found. This is suitable for searches for objects objects can be easily found. This is suitable for searches for objects with variability scales less than one yearwith variability scales less than one year

We have started to monitor the IGR positions by robotic telescopes We have started to monitor the IGR positions by robotic telescopes and, more recently, by a 60 cm CCD telescope at the Brno and, more recently, by a 60 cm CCD telescope at the Brno ObservatoryObservatory

Monitoring of IGR sources by Monitoring of IGR sources by robotic CCD telescopes BART and robotic CCD telescopes BART and WATCHERWATCHER

The proposed analysisThe proposed analysisUsing the data mentioned here, the optically

identified INTEGRAL sources with objects brighter than ~ mag 17 can be investigated for long-term changes covering 10 … 50 years.

In addition, these data can be used to search for new optical identifications of non-classified INTEGRAL sources on hand of their optical variability. This has been used already succesfully for ROSAT (Greiner and Richter,2006)

Distribution of Sonneberg Field Patrol Fields and Franklin Adams Fields (blue) in Galactic

coordinates.The densely covered fields are darker.

The coverage of INTEGRAL IBIS for revolutions 1 - 430.

Additional prospects

analyzing the light curves for flares and flaring activity like these seen in V1223 Sgr and TV Col

trying to fit the flare profiles trying to look for possible periodicities and recurrence study of colors and color changes with time, with

consequent physical discussions and interpretations. correlations with other objects, with related conclusions

toward physical processes and physical models.

Optical analyses of INTEGRAL Optical analyses of INTEGRAL gamma ray sourcesgamma ray sources

Promising task for our group, taking into account our facilities and our experience

Also for other HE satellites and observing campaigns

Examples: LSI 61 303 mag 10, optical counterparts of fast X-ray transients-massive stars, INTEGRAL CVs and symbiotics, etc.

TV Col is an intermediate polar (IP) and the optical counterpart of the X-ray source 2A0526-328 (Cooke et al. 1978, Charles et al. 1979). This is the first cataclysmic variable (CV) discovered through its X-ray emission.

TV Col displays three types of variation in the optical:

(a) basic 0.2163 d photometric variation with an amplitude of ~0.27 mag (Motch 1981).(b) spectroscopic period of 0.22868 d (Hutchings et al. 1981).(c) beat period of 4.024 d between the photometric and spectroscopic period (Motch 1981).(d) flickering (~0.1 mag) on the time scale of minutes or dozens of minutes (Motch 1981).(e) brief outbursts lasting for ~hours with an amplitude of ~2 mag (Szkody and Mateo 1984).

Photographic light curve Photographic light curve of TV Col including of TV Col including segments densely segments densely covered by the covered by the observations. The observations. The detected outbursts are detected outbursts are marked by the vertical marked by the vertical lines. The data are lines. The data are connected by the line in connected by the line in the densely covered the densely covered intervals for convenience. intervals for convenience. The photographic The photographic magnitudes were magnitudes were calibrated to the calibrated to the BB magnitudes. The empty magnitudes. The empty triangles denote the upper triangles denote the upper limits of brightness.limits of brightness.

Outbursts of TV Col:

Date JD Max. (mag) Duration Source

2434420.348 B=12.60 <1 day Hudec et al. 20052434475.265 B=13.29? < 1 day Hudec et al. 20052439031.625 B=13.38 < 1 day Hudec et al. 20052439059.510 B=12.33 < 1day Hudec et al. 20052440572.398 B=12.25 <1 day Hudec et al. 20052444295.819 V~12.3 ~3 hr, ~1 d* Szkody and Mateo (1984)2446125.73 V~11.9 ~4.5 hr Schwarz and Heemskerk (1987)

2446133.50 V~12 ~6 hr Schwarz and Heemskerk (1987)2447122.6 B~1.2 ~6 hr Augustein et al. (1994)2447125.7 B~1.8 ~6 hr Augustein et al. (1994)2447133.6 B~1.8 ~8 hr Augustein et al. (1994)2448600.375 V~12.4 ~6 hr, ~3d* Hellier and Buckley (1993)

Note: * corresponds to the full decline of outburst.

Decay time scale of dwarf nova (DN) outbursts tD (in days/mag) versus the orbital Decay time scale of dwarf nova (DN) outbursts tD (in days/mag) versus the orbital period period PPorb. The solid line marks the fit to non-magnetic DN (empty circles) (Warner orb. The solid line marks the fit to non-magnetic DN (empty circles) (Warner 1995). Intermediate polars are denoted by the solid circles. The upper and lower 1995). Intermediate polars are denoted by the solid circles. The upper and lower symbols for HT Cam mark the initial and final tD, respectively. The outburst data for IPs symbols for HT Cam mark the initial and final tD, respectively. The outburst data for IPs come from Hellier et al., (1997), Ishioka et al. (2002), Schwarz et al. (1988), Šimon (2000, come from Hellier et al., (1997), Ishioka et al. (2002), Schwarz et al. (1988), Šimon (2000, 2002), van Amerongen and van Paradijs (1989), Warner (1995).2002), van Amerongen and van Paradijs (1989), Warner (1995).

ConclusionsConclusions•Alternative identification method based on high quality Alternative identification method based on high quality

astronomical archival plates has been proposedastronomical archival plates has been proposed

•In addition, already identifies sources can be effectively In addition, already identifies sources can be effectively monitored in optical lightmonitored in optical light

•Important also for searches for brightenings in IBIS dataImportant also for searches for brightenings in IBIS data

The EndThe End