wfpdb development: restoring characteristic curve from digitized images of scanned photographic...
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WFPDB DEVELOPMENT: RESTORING CHARACTERISTIC CURVE FROM DIGITIZED
IMAGES OF SCANNED PHOTOGRAPHIC PLATES
VII-th Bulgarian-Serbian Astronomical Conference
1 - 4 June, 2010, Chepelare, Bulgaria
H. Markov, M. Tsvetkov, A. Borisava, N. Petrov
Institut of Astronomy and National Astronomical Observatory - BAS
saving astronomical photographs
Today astronomical photography is rarely applied, but
for the sake of this a huge amount of photographic
plates and films with valuable and still only partially
utilized information for the astronomical objects and
phenomena have been accumulated in the archives of
the astronomical observatories. The preservation and
utilization of this treasure is of great importance for
contemporary astronomy. To retrieve the information
stamped there we need to refine not only the digitisation
process but also some approaches wich ensure us the
posiible highest photometric quality.
digitization of the photographic material gives the opportunity
these astronomical observations to be processed and analyzed in
the manner of the CCD observation
one serious disadvantage of the photographic emulsion is its
nonlinearity. In order to overcome this problem one have to
build-up the so called characteristic curve – the relation between
photographic density and the relative intensity.
one particular task
The profesional astronomy practice requires on every
astronomical plate a photometric wedge to be
stamped additionally. Most oftenly when the object
of scientific interest is a globular cluster such wedge
is missing. In these cases the recovering of the
emulsion characteristic curve is tricky in some sense.
the wedge used in the NAO
the approach
our main goal was to develope a method for building-up the
emulsion characteristic curve only by means of apropriate tasks
available in IRAF packages. Here we demonstrate the principles of
the method we developed and would like to emphasize that no
additional software or routines were used.
our presentation is not a review of the available methods to recover
characteristic curves but will demonstrate one of them – a method
offered by de Vacouleuers in 1982
The principle of bulding characteristic curve using radial profiles of
two stars with known magnitudes. The step between every two points
is Δm – the difference in the magnitudes of the couple.
To apply the method of de Vaucouleurs one needs to identify in the field of the
investigated plate some stars with known magnitudes. Here we demonstrate a
scaned plate with a wedge. The stars identified by means af GSC are marked
Radial stellar profile – the base for recovering the characteristic curve.
The requirement for two stellar profiles to be used in a couple is to merge in
the same background. This could be influenced not only from the variable
sky illumination but also from the non-equal chemical fog caused by un-
proper treatment of the plate during the development process.
Concerning here demonstrated method every couples of stellar
profiles contains information for the characteristic curve of the
emulsion. Following the method the more close in transparency
profiles will produce more points on the curve.
On the right, the char. curve derived by means of stellar profiles is marked by point. The continuous curve shows the char. curve derived by the wedge stamped on the plate. A good coincidence between two relations is achieved if the magnitude difference of the stars in a couple is accepted to be 0.21 mag instead 0.29 mag adopted from GSC.
stellar profiles of the coupleGSC Δm = 0.29 mag
These couple demonstrates the ability of the method to reveal inconsistency of stellar magnitudes. In our opinion the magnitude difference of 1.67 mag is not realistic
stellar profiles of the coupleGSC Δm = 1.67 mag (???)Δm = 0.5 mag is more realistic
One particular case of the outlined method to recover the characteristic curve of the emulsion uses rich sample of stars with known magnitudes. This approach relies on the fact that the top pixels of the stellar image(or the max values in the profile) are well proportional to the brightness of the star. So if we have rich sample of stars with known magnitudes which cover the whole dynamic range in transparency(density) we can construct the char. curve. The most appropriate fields filling such requirements are the regions of globular clusters. where we can find many stars with well established brightness(Stetson 2001, Catalog of CCD standards).
another approach
Part of the field near the center of the globular cluster M3 where about
400 CCD standard stars from the Stetson catalog were identified and
used to buld-up the characteristic curve for this plate
characteristic curve derived by means of the CCD standard of
Stetson in the field of globular cluster М3. The points' scatter in
the middle is caused by stars on the horisontal branch of the
cluster which are more blue than others cluster members.
some basic IRAF packages and routins
DAOPHOT(DAOFIND, PHOT)
APPHOT(RADPROF)
MATH(CURFIT)
IMAGES(DISPLAY, IMEXAM)
TABLES
So feel free to use the photographic archive of the National Astronomical Observatory. We can help you to retrieve the maximum
quality information from the astronomical photographic plates
THANK YOU FOR YOUR ATTENTION
Това изследване е извършено с помощта на договори с ФНИ ДО 02-273, ДО 02-85, НИК-05