Realization of the Vilnius photometric system for CCD-observations of selected sky areas at the Andrushivka Astronomical Observatory
We describe a set of glass UPXYZVS filters of the Vilnius photometric system of the Andrushivka Astronomical Observatory in Zhytomyr Region (Ukraine) [7]. They are installed at the Zeiss-600 Cassegrain reflector together with the 15-bit 1024×1024 CCD-camera S1C-017. The response curves of instrument...
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| Published in: | Кинематика и физика небесных тел |
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| Date: | 2005 |
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Головна астрономічна обсерваторія НАН України
2005
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| Cite this: | Realization of the Vilnius photometric system for CCD-observations of selected sky areas at the Andrushivka Astronomical Observatory / V. Andruk, G. Butenko, O. Gerashchenko, Yu. Ivashchenko, G. Kovalchuk, V. Lokot', V. Samoylov // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 401-404. — Бібліогр.: 10 назв. — англ. |
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Digital Library of Periodicals of National Academy of Sciences of Ukraine| _version_ | 1859596665334267904 |
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| author | Andruk, V. Butenko, G. Gerashchenko, O. Ivashchenko, Yu. Kovalchuk, G. Lokot', V. Samoylov, V. |
| author_facet | Andruk, V. Butenko, G. Gerashchenko, O. Ivashchenko, Yu. Kovalchuk, G. Lokot', V. Samoylov, V. |
| citation_txt | Realization of the Vilnius photometric system for CCD-observations of selected sky areas at the Andrushivka Astronomical Observatory / V. Andruk, G. Butenko, O. Gerashchenko, Yu. Ivashchenko, G. Kovalchuk, V. Lokot', V. Samoylov // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 401-404. — Бібліогр.: 10 назв. — англ. |
| collection | DSpace DC |
| container_title | Кинематика и физика небесных тел |
| description | We describe a set of glass UPXYZVS filters of the Vilnius photometric system of the Andrushivka Astronomical Observatory in Zhytomyr Region (Ukraine) [7]. They are installed at the Zeiss-600 Cassegrain reflector together with the 15-bit 1024×1024 CCD-camera S1C-017. The response curves of instrumental photometric systems are presented and a comparison of them with a standard system are analysed. Test observations in the Vilnius system of the star cluster IC 4665 with the Andrushivka filters were carried out in May–June 2003. The MIDAS/ROMAFOT and ASTROIMAGE software is adapted for digital processing of CCD-images of stellar fields. Comprehensive ground-based observations are being planned to design a catalogue of primary UPXYZVS CCD-standards in selected areas of the sky where are with radio sources, globular and open clusters, etc.
|
| first_indexed | 2025-11-27T22:22:17Z |
| format | Article |
| fulltext |
REALIZATION OF THE VILNIUS PHOTOMETRIC SYSTEM
FOR CCD-OBSERVATIONS OF SELECTED SKY AREAS
AT THE ANDRUSHIVKA ASTRONOMICAL OBSERVATORY
V. Andruk1, G. Butenko2, O. Gerashchenko1, Yu. Ivashchenko3,
G. Kovalchuk1, V. Lokot’ 3, V. Samoylov1
1Main Astronomical Observatory, NAS of Ukraine
27 Akademika Zabolotnoho Str., 03680 Kyiv, Ukraine
e-mail: andruk@mao.kiev.ua, koval@mao.kiev.ua
2International Center for Astronomical, Medical and Ecological Research
27 Akademika Zabolotnoho Str., 03680 Kyiv, Ukraine
e-mail: butenko@mao.kiev.ua
3Andrushivka Astronomical Observatory
3–7b Observatorna Str., Galchyn, Zhytomyr Region, Ukraine
e-mail: aao@gluk.org
We describe a set of glass UPXYZVS filters of the Vilnius photometric system of the Andrushivka
Astronomical Observatory in Zhytomyr Region (Ukraine) [7]. They are installed at the Zeiss-600
Cassegrain reflector together with the 15-bit 1024×1024 CCD-camera S1C-017. The response
curves of instrumental photometric systems are presented and a comparison of them with a stan-
dard system are analysed. Test observations in the Vilnius system of the star cluster IC 4665
with the Andrushivka filters were carried out in May–June 2003. The MIDAS/ROMAFOT and
ASTROIMAGE software is adapted for digital processing of CCD-images of stellar fields. Compre-
hensive ground-based observations are being planned to design a catalogue of primary UPXYZVS
CCD-standards in selected areas of the sky where are with radio sources, globular and open clus-
ters, etc.
INTRODUCTION
Regular astronomical observations began in 2001 at the Andrushivka Astronomical Observatory (AAO) in Zhy-
tomyr Region (Ukraine). Its coordinates determined by GPS-methods are: φ= 50◦ 00′ 02.0′′, λ = 28◦ 59′ 50.3′′,
h =240 m. The Zeiss-600 Cassegrain reflector (D/F = 60/750 cm) with the digital television CCD-camera
S1C-017 made by “Electron Optronic” (St.-Petersburg, Russia) is installed at the Observatory. The S1C-017
device can operate over a wide spectral range with a high geometrical accuracy and low reading noise and is
destined for the detection of black–white images with low illumination. An image has 1024×1024 pixels, frame
size is 7.8′×7.8′ and a scale is 1 pixel = 1.34′′ (for the primary focus).
Table 1. Components and optical features of instrumental photometric system filters
Filter Components λmax (Å) Transmission
in maximum (%)
U S21(2.0) +UFS2(1.0) +Quartz(3.0) 3570 24.9
P SZS21(2.0) + UFS(2.7) +Quartz(10.3) 3760 34.1
X ZS4(3.2) +ZS7(6.2) +SZS21(1.8) + Quartz(1.8) 4060 20.0
Y ZS12(5.2) +SZS21(2.6) + SS15(2.0) +K8(5.2) 4630 25.7
Z ZS17(2.0) +ZS7(3.1) + SZS22(10.0) 5140 36.8
V OS11(1.5) +SZS22(5.0) + PS7(2.0) + K8(6.5) 5400 32.7
S KS13(2.0) + SZS23(2.0) + K8(11.0) 6400 31.9
The availability of the high quantum efficiency device for the detection of radiation over a wide spectral range
stimulated the realization of that photometric system measurements in which physical properties of celestial
c© V. Andruk, G. Butenko, O. Geraschenko, Yu. Ivashchenko, G. Kovalchuk, V. Lokot’, V. Samoylov, 2004
401
bodies can be reflected in an unique manner. Such a system is the seven-colour Vilnius UPXYZVS system
providing a possibility of a many-dimensional spectral classification of stars when the space reddening exceeds
the overall star temperature interval [1]. At AAO, in the first stage of the UPXYZVS system realization,
observations of a selected list of initial photoelectric standards of the Vilnius system in the north sky will be
carried out to form a network of initial CCD-standards. The second stage works will be performed in parallel,
namely the formation of a CCD-variant of photometric UPXYZVS-standards in selected sky areas, in areas
with open and globular clusters, with infrared objects and radio sources for the purpose to perform statistical
investigations of the Galaxy and Solar System bodies. The photometric investigations in the Vilnius system
in these sky areas will be supplemented with measurements in the Johnson UBVRI system. Some results of
this program will be as follows: a catalogue of a unified list of stars (objects) in two photometric systems,
investigation of interstellar extinction, search maps for sky areas in the form of adapted CCD-images, and
investigation of the seeing at Andrushivka settlement (extinction, night airglow brightness). An experience of
this kind of investigation was accumulated before [3–5].
A COMPARISON OF FILTERS OF INSTRUMENTAL
AND STANDARD UPXYZVS SYSTEMS
Three sets of glass filters for seven UPXYZVS bands were made for the Andrushivka Astronomical Observatory
in May 2002. The sizes of all the filters are 35 mm×35 mm and their thickness equals 15 mm (to level off
optical thickness, quartz or the glass K8 was added by forming the transmission curve of a combination of
glasses of different thickness). Industrially prepared standard glass filters were used similar to filters employed
by developers of the original UPXYZVS system [9, 10]. Spectral transmission coefficients for prototypes of
all the filters were measured in the Ukrainian State Research and Production Center for Standardization,
Metrology and, Certification (UkrCSM, Kyiv). Absolute errors are within 1.0 percent for transmission coefficient
measurements and 1.0 nm for wavelength measurements. For the “telescope+receiver” system, filters play
a crucial role in the formation of curves of reaction of the photometric system. Table 1 gives some information
on components (a sort of glass and glass thickness in mm in brackets) and optical features (the transmission
maximum wavelength λmax (Å), transmission bandwidth (Å), and the transmission maximum value (in percent))
for the filters made for AAO. Atmospheric transparency (the equivalent thickness of the layers O2 and H2O are
3 and 10 mm, respectively) and selectivity of mirror reflection [1] were taken into account by calculating final
curves of reaction of instrumental system bands.
Figure 1 illustrates the response curves for the instrumental system (the dotted line) and for the standard
system [10] (the solid line).
RESULTS OF FIRST OBSERVATIONS
An extensive observational information was accumulated during the spring and summer 2002 period of observa-
tions of various sky areas with the use of UBVR photometric standards. An analysis of the observations reduced
by means of the MIDAS/ROMAFOT software package [5, 6] showed that the limiting magnitude of objects
to be recorded (signal accumulation time is equal to 10 min) in integral light is close to 21m in the R band
(these are precisely the magnitudes which are used in ASTROMETRICA, the software package for reducing
CCD-observations, that we have applied [http://www.astrometrica.at]).
Photometric observations with UPXYZVS filters were carried out in June 2003 to check the identity of
the instrumental and standard systems. The IC 4665 cluster which is sufficiently compact and rich by stars
with UPXYZVS values determined reliably (Straizys V., Kazlauskas A., private communication) was selected
as an object for observations. The camera was installed in the primary focus (F =2400 mm, the scale is
1 pixel = 1.34′′). Such mode of the camera installation on at the classical Cassegrain telescope was used to
increase the penetrating power of the telescope in the case of observations of extremely faint objects, namely
asteroids and comets (a gain of magnitude is almost 1 m at a sacrifice of resolving power). But this mode
of the installation is tolerable and allows us to avoid many hazards in the case of photometric observations.
The observations were carried out practically in the meridian and the cluster zenith distance did not exceed
30◦ (plausible corrections for atmospheric extinction can not exceed 0.01m in this case). The exposure was
equal to 60 s for U, P, and X filters and to 120 s for the other filters. The ASTROMETRICA package
(version 4.1.2) was used for the initial traditional CCD-frames reducing which included the correction for dark
current (dark frame) and flat field (flat field frame). Two software packages, namely MIDAS/ROMAFOT and
ASTROIMAGE [http://www.phasespace.com.au] packages, were applied in the following stages of reducing,
in particular, by determining magnitudes of program stars, since ASTROMETRICA is primarily aimed to
calculate star coordinates. The USNO-SA 2.0 catalogue founded on magnitude measurements in B and R filters
is used as the basic one in the package, which is developed to solve photometric problems. Compilating and
402
Figure 1. The normalized response curves of the standard Vilnius system (thin line) and the Andrushivka instrumental
CCD-system (thick line)
Figure 2. Comparison of observed (axis Y) and standard (axis X) meanings of V -magnitude (panel a) and colour-index
Y –Z(panel b) for stars in cluster IC 4665
403
applying a user’s catalogue with magnitudes data in other photometric systems are not provided in the package.
Figure 2 illustrates a comparison of V-magnitude (panel a) and colour-index Y–Z (panel b) of the same stars in
the instrumental (the axis Y) and standard (the axis X) photometric system. It may be preliminary deduced
from these graphs that the instrumental UPXYZVS photometric system of the Andrushivka Astronomical
Observatory is in a reasonably good agreement with the standard system. The research work is planned to be
continued using the list of the cluster IC 4665 standards enlarged at the expense of fainter stars.
CONCLUSION
A set of filters for the UPXYZVS photometric system was manufactured and their metrological attestation
was performed. The response curves for the instrumental system were investigated and compared with ones
for the standard system. We carried out series of observations of the cluster IC 4665 stars with magnitudes
determined before by the photoelectric method. Our comparison of the instrumental and standard photomet-
ric system confirmed an inference which was derived from calculations that these two systems are in good
agreement. An extensive observational program is scheduled to be performed to form initial CCD-standards in
the UPXYZVS system for selected sky areas, in particular, in globular and open clusters, as well as in areas
with infrared and radio sources.
Acknowledgements. This research was performed using the SIMBAD database, operated at CDS, Strasbourg,
France.
[1] Allen K. Astrophysical quantities.–Moscow: Mir, 1993.–446 p. (in Russian).
[2] Andruk V. N. Photometric survey near main galactic meridian: Photoelectric observations and creation of the cata-
logue of stellar magnitudes and colour indexes in the UBVR system // Kinematics and Physics of Celestial Bodies.–
1996.–12, N 4.–P. 60–73.
[3] Andruk V. N., Bartasiute S., Kharchenko N. UBVR and UPXYZVS sequences of standard stars for the MEGA
program fields along the Main Meridian of the Galaxy // Baltic Astron.–1996.–5.–P. 197–206.
[4] Andruk V. N., Butenko G. Z., Kuznetsov V. I., et al. Investigations of seening for 2-m telescope at Terskol Peak //
Kinematics and Physics of Celestial Bodies. Suppl. Ser.–2003.–N 4.–P. 75–80.
[5] Andruk V. N., Parusimov V. G., Dudnik T. B. The experience of digital processing of stellar fields’ images in
the MIDAS–ROMAFOT software // Kinematics and Physics of Celestial Bodies. Suppl. Ser.–2001.–N 1.–P. 100–103.
[6] MIDAS Users Guide, European Southern Observatory – Image Processing Group 1994, Garching, ESO, 1994.–
Vol. A, B, C.
[7] Ivashchenko Yu. M., Andruk V. N. Andrushivka Astronomical Observatory in 2001. Extension and connection of
reference frames using ground-based CCD technique.–Mykolaiv: Atoll, 2001.–P. 224–230.
[8] Pugach A. F., Kovalchuk G. U. Identification Charts and Secondary UBVR-standards to Observe the Antiflare
Stars // Peremennie zvezdy.–1983.–22, N 1.–P. 9–23.
[9] Straizys V. Multicolor stellar phonometry.–Vilnius: Mosklas, 1977.
[10] Straizys V., Zdanavichius K. Response curves of the system UPXYZVS // Bull. Vilnius Obs.–1970.–29.–P. 15.
404
|
| id | nasplib_isofts_kiev_ua-123456789-79687 |
| institution | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| issn | 0233-7665 |
| language | English |
| last_indexed | 2025-11-27T22:22:17Z |
| publishDate | 2005 |
| publisher | Головна астрономічна обсерваторія НАН України |
| record_format | dspace |
| spelling | Andruk, V. Butenko, G. Gerashchenko, O. Ivashchenko, Yu. Kovalchuk, G. Lokot', V. Samoylov, V. 2015-04-03T19:17:25Z 2015-04-03T19:17:25Z 2005 Realization of the Vilnius photometric system for CCD-observations of selected sky areas at the Andrushivka Astronomical Observatory / V. Andruk, G. Butenko, O. Gerashchenko, Yu. Ivashchenko, G. Kovalchuk, V. Lokot', V. Samoylov // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 401-404. — Бібліогр.: 10 назв. — англ. 0233-7665 https://nasplib.isofts.kiev.ua/handle/123456789/79687 We describe a set of glass UPXYZVS filters of the Vilnius photometric system of the Andrushivka Astronomical Observatory in Zhytomyr Region (Ukraine) [7]. They are installed at the Zeiss-600 Cassegrain reflector together with the 15-bit 1024×1024 CCD-camera S1C-017. The response curves of instrumental photometric systems are presented and a comparison of them with a standard system are analysed. Test observations in the Vilnius system of the star cluster IC 4665 with the Andrushivka filters were carried out in May–June 2003. The MIDAS/ROMAFOT and ASTROIMAGE software is adapted for digital processing of CCD-images of stellar fields. Comprehensive ground-based observations are being planned to design a catalogue of primary UPXYZVS CCD-standards in selected areas of the sky where are with radio sources, globular and open clusters, etc. This research was performed using the SIMBAD database, operated at CDS, Strasbourg, France. en Головна астрономічна обсерваторія НАН України Кинематика и физика небесных тел MS4: Positional Astronomy and Global Geodynamics Realization of the Vilnius photometric system for CCD-observations of selected sky areas at the Andrushivka Astronomical Observatory Article published earlier |
| spellingShingle | Realization of the Vilnius photometric system for CCD-observations of selected sky areas at the Andrushivka Astronomical Observatory Andruk, V. Butenko, G. Gerashchenko, O. Ivashchenko, Yu. Kovalchuk, G. Lokot', V. Samoylov, V. MS4: Positional Astronomy and Global Geodynamics |
| title | Realization of the Vilnius photometric system for CCD-observations of selected sky areas at the Andrushivka Astronomical Observatory |
| title_full | Realization of the Vilnius photometric system for CCD-observations of selected sky areas at the Andrushivka Astronomical Observatory |
| title_fullStr | Realization of the Vilnius photometric system for CCD-observations of selected sky areas at the Andrushivka Astronomical Observatory |
| title_full_unstemmed | Realization of the Vilnius photometric system for CCD-observations of selected sky areas at the Andrushivka Astronomical Observatory |
| title_short | Realization of the Vilnius photometric system for CCD-observations of selected sky areas at the Andrushivka Astronomical Observatory |
| title_sort | realization of the vilnius photometric system for ccd-observations of selected sky areas at the andrushivka astronomical observatory |
| topic | MS4: Positional Astronomy and Global Geodynamics |
| topic_facet | MS4: Positional Astronomy and Global Geodynamics |
| url | https://nasplib.isofts.kiev.ua/handle/123456789/79687 |
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