Identification maps for selected sky fields with IR/radio sources constructed at the base of CCD observations at the Andrushivka Astronomical Observatory
In July 2002 the CCD unfiltered images of eight sky areas with the IR/radio sources from ICRF 1732+389, 1803+784, 1807+698, 1845+797, 1943+228, 2023+335, 2223–052, and 2229+695 were obtained with the Zeiss-600 telescope of the Andrushivka Observatory. This telescope is equipped with a CCD S1C-017 de...
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| Cite this: | Identification maps for selected sky fields with IR/radio sources constructed at the base of CCD observations at the Andrushivka Astronomical Observatory / O.V. Perekhod, V.M. Andruk, L.K. Pakuliak, Yu.M. Ivashchenko // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 417-422. — Бібліогр.: 4 назв. — англ. |
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Perekhod, O.V. Andruk, V.M. Pakuliak, L.K. Ivashchenko, Yu.M. 2015-04-03T19:26:04Z 2015-04-03T19:26:04Z 2005 Identification maps for selected sky fields with IR/radio sources constructed at the base of CCD observations at the Andrushivka Astronomical Observatory / O.V. Perekhod, V.M. Andruk, L.K. Pakuliak, Yu.M. Ivashchenko // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 417-422. — Бібліогр.: 4 назв. — англ. 0233-7665 https://nasplib.isofts.kiev.ua/handle/123456789/79691 In July 2002 the CCD unfiltered images of eight sky areas with the IR/radio sources from ICRF 1732+389, 1803+784, 1807+698, 1845+797, 1943+228, 2023+335, 2223–052, and 2229+695 were obtained with the Zeiss-600 telescope of the Andrushivka Observatory. This telescope is equipped with a CCD S1C-017 detector; our observations were carried out in integral light only. The processing of images was implemented by the MIDAS/ROMAFOT software. Coordinates and magnitudes down to B = 21 mag in 3'×3' fields were obtained in the USNO A2.0 system. Identification maps in integral light obtained as the result of the CCD image processing are shown. This work has been partly supported by the Fundamental Research State Fund of the Ministry of Ukraine for Education and Science (Grant 02.07/00017) and the Scientific and Technological Center in Ukraine (Grant NN43). The authors wish to thank the amateurs of astronomy, the pupils of Andrushivka secondary school No. 1 O. Drobenko, D. Kyrylenko, P. Kyrylenko, O. Pastovens’kii, B. Studyns’kii, and A. Solom’ianiuk for a help in observations. en Головна астрономічна обсерваторія НАН України Кинематика и физика небесных тел MS4: Positional Astronomy and Global Geodynamics Identification maps for selected sky fields with IR/radio sources constructed at the base of CCD observations at the Andrushivka Astronomical Observatory Article published earlier |
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Identification maps for selected sky fields with IR/radio sources constructed at the base of CCD observations at the Andrushivka Astronomical Observatory |
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Identification maps for selected sky fields with IR/radio sources constructed at the base of CCD observations at the Andrushivka Astronomical Observatory Perekhod, O.V. Andruk, V.M. Pakuliak, L.K. Ivashchenko, Yu.M. MS4: Positional Astronomy and Global Geodynamics |
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Identification maps for selected sky fields with IR/radio sources constructed at the base of CCD observations at the Andrushivka Astronomical Observatory |
| title_full |
Identification maps for selected sky fields with IR/radio sources constructed at the base of CCD observations at the Andrushivka Astronomical Observatory |
| title_fullStr |
Identification maps for selected sky fields with IR/radio sources constructed at the base of CCD observations at the Andrushivka Astronomical Observatory |
| title_full_unstemmed |
Identification maps for selected sky fields with IR/radio sources constructed at the base of CCD observations at the Andrushivka Astronomical Observatory |
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identification maps for selected sky fields with ir/radio sources constructed at the base of ccd observations at the andrushivka astronomical observatory |
| author |
Perekhod, O.V. Andruk, V.M. Pakuliak, L.K. Ivashchenko, Yu.M. |
| author_facet |
Perekhod, O.V. Andruk, V.M. Pakuliak, L.K. Ivashchenko, Yu.M. |
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MS4: Positional Astronomy and Global Geodynamics |
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MS4: Positional Astronomy and Global Geodynamics |
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2005 |
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English |
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Кинематика и физика небесных тел |
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Головна астрономічна обсерваторія НАН України |
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In July 2002 the CCD unfiltered images of eight sky areas with the IR/radio sources from ICRF 1732+389, 1803+784, 1807+698, 1845+797, 1943+228, 2023+335, 2223–052, and 2229+695 were obtained with the Zeiss-600 telescope of the Andrushivka Observatory. This telescope is equipped with a CCD S1C-017 detector; our observations were carried out in integral light only. The processing of images was implemented by the MIDAS/ROMAFOT software. Coordinates and magnitudes down to B = 21 mag in 3'×3' fields were obtained in the USNO A2.0 system. Identification maps in integral light obtained as the result of the CCD image processing are shown.
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0233-7665 |
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https://nasplib.isofts.kiev.ua/handle/123456789/79691 |
| citation_txt |
Identification maps for selected sky fields with IR/radio sources constructed at the base of CCD observations at the Andrushivka Astronomical Observatory / O.V. Perekhod, V.M. Andruk, L.K. Pakuliak, Yu.M. Ivashchenko // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 417-422. — Бібліогр.: 4 назв. — англ. |
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2025-11-25T21:07:14Z |
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| fulltext |
IDENTIFICATION MAPS FOR SELECTED SKY FIELDS WITH IR/RADIO
SOURCES CONSTRUCTED AT THE BASE OF CCD OBSERVATIONS
AT THE ANDRUSHIVKA ASTRONOMICAL OBSERVATORY
O. V. Perekhod1, V. M. Andruk1, L. K. Pakuliak1, Yu. M. Ivashchenko2
1Main Astronomical Observatory, NAS of Ukraine
27 Akademika Zabolotnoho Str., 03680 Kyiv, Ukraine
e-mail: andruk@mao.kiev.ua
2Adrushivka Astronomical Observatory
3–7b Observatorna Str., Galchyn, Zhytomyr Region, Ukraine
In July 2002 the CCD unfiltered images of eight sky areas with the IR/radio sources from ICRF
1732+389, 1803+784, 1807+698, 1845+797, 1943+228, 2023+335, 2223–052, and 2229+695 were
obtained with the Zeiss-600 telescope of the Andrushivka Observatory. This telescope is equipped
with a CCD S1C-017 detector; our observations were carried out in integral light only. The proces-
sing of images was implemented by the MIDAS/ROMAFOT software. Coordinates and magnitudes
down to B = 21 mag in 3′× 3′ fields were obtained in the USNO A2.0 system. Identification maps
in integral light obtained as the result of the CCD image processing are shown.
INTRODUCTION
First we observed eight sky regions in the optical spectral range with a CCD device. These fields have common
extragalactic sources identified in the radio and IR ranges. The sources are a part of the list from [4] –
total list includes 31 sources which were observed by IRAS (see the IRAS PSC catalog [2]). The purpose
of our observations was to check the identifications made both to exclude the possible errors and to answer
the question: are there some objects with sufficiently high level of radiation in the optical diapason in that
points of sky?
OBSERVATIONS
We made our observations at the Adrushivka Astronomical Observatory in Zhytomyr Region in July 2002.
The S1C-017 television digital camera of “Electron Optronic” company (St.-Petersburg, Russia) was mounted
in Cassegrain focus of the Zeiss-600 telescope. The S1C device has a wide spectral range and is intended for
registering the black-and-white images at low illumination level. The format of images was 1024×1024 pixels or
7.65′×7.65′. Table 1 lists the numerical parameters of the quantum efficiency of the CCD with thermoelectronic
microrefregerator as the maker claims. Our investigation showed that it was possible to register the stars down
to V = 20m in the integral light at 10 min exposure, i.e., to observe all objects of our list both in visual and
close IR ranges.
First of all, we checked the existence of some objects at the sky points which have coordinates from [4].
In future, to carry out the final verification of identity of ICRF radio sources with their IR counterparts we
shall assume to accomplish the UBVRI and UPXYZVS photometry of IR/radio sources which verification was
successful at the first stage. The accuracy of one determination of position and photometry for bright source
(R < 16m) is not less than 0.05′′ and 0.03m, respectively, when the MIDAS/ROMAFOT software is used for
processing the CCD star field images.
CCD OBSERVATION PROCESSING
The CCD star field image processing was carried out by the MIDAS/ROMAFOT software (LINUX shell) [1].
The ROMAFOT software is intended for high-precision determination of astrometric (rectangular coordinates
X , Y ) and photometric (magnitudes, FWHM values, etc.) characteristics for all objects to be registered on
CCD frame digitized images. The use of the MIDAS software gives possibility to automatize the CCD frame
processing by organizing the cyclic MIDAS procedures for files in FITS format.
c© O. V. Perekhod, V. M. Andruk, L. K. Pakuliak, Yu. M. Ivashchenko, 2004
417
Table 1. Quantum effectiveness of S1C-017 CCD camera as a function of wavelength (nm) according to producer
announcement
λ % λ % λ % λ % λ %
230 17.5 380 37.3 530 47.5 680 46.5 830 28.2
250 21.6 400 37.5 550 47.9 700 45.2 850 25.0
270 20.9 420 37.5 570 48.3 720 41.5 870 20.0
290 25.5 440 38.1 590 49.3 740 37.5 890 15.0
310 31.7 460 41.1 610 49.0 760 34.6 910 11.4
330 35.3 480 43.7 630 47.4 780 33.4 930 9.0
350 34.0 500 45.6 650 46.0 800 32.3 950 7.0
370 36.5 520 46.9 670 46.5 820 30.1 970 5.2
The original stage of processing the CCD frames consists of standard subtraction reduction of dark current
and reading noise, and then the result division on the flat field. Commonly, when the standard reduction is
used, they obtain the frames with a flat field by short exposures of the early morning sky or twilight one, i.e.,
the flat field frames and star field image frames are exposed separately and at different conditions. In this paper
the flat field frames were obtained directly from the star field image frames because the flat field frame was
exposed at the same conditions as the star field image frame. To do this, all objects registered were removed
from the frame under processing after the subtraction the “dark current” frame from the “raw” frame. By such
a way, we obtained the spatial envelope curve from the frame with flat field image. As a result, the frame of true
flat field have been created. This frame was undergone to the normalizing procedure, i.e., the division procedure
of the flat field on the mean value over whole frame. The frame with normalized own flat field was used for
photometric reduction (the correction for optical vignetting and large-scale homogeneity of matrix sensitivity) of
the CCD frame of star field image. To obtain the value of residual photometric field error, the above-mentioned
new photometric reduction technique of the “raw” CCD frames of star field images was used (the reduction
to the flat field). Investigations of observations in a wide exposure range (10–840 s), and comparison with
photometric standards over the whole field of matrix of CCD frames did not show the existence of the field
photometric error and distortion of magnitude scale. Independent comparison of photometric data obtained by
the above technique with results of processing of the CCD frames under standard reduction for the flat field
have shown that the procession of both techniques was the same one.
By using the MIDAS software, the bright overexposed objects (when the photometric section in the central
part of star has a gap) with B < 14–15 mag were marked out and transformed to process by the ROMAFOT
software.
REDUCTION OF INSTRUMENTAL VALUES INTO THE USNO A2.0 SYSTEM
Main aim of this work is the determination of equatorial coordinates and magnitudes of objects registered
on the CCD frames. The USNO A2.0 catalog was used as a reference one. The reference star rectangular
coordinates ξi and ηi were determined by rms solution of the equation system
ξi = a1Xi + b1Yi + c1 + d1X
2
i + e1XiYi + f1Y
2
i ,
ηi = a2Xi + b2Yi + c2 + d2X
2
i + e2XiYi + f2Y
2
i ,
(1)
where i = 1, 2, ..., N is the number of reference stars from the USNO A2.0 catalog for the field of 7.65×7.65 arc-
min, N varies from 40 to 400. The solution rms errors of reduction Equations (1) are 0.2–0.5 arcsec and they
depend on N value. As an example, we consider the determination errors of coordinates and magnitudes of
ICRS 1943+228 region because this one has the greatest number of stars. First and second panels in Fig. 1
show the differences of rectangular coordinates ΔX and ΔY for all objects on two plates. The CCD frames were
obtained consequently at 840 s exposure; the shift between optical centers of stars is approximately 10 pixels.
The differences of equatorial coordinates ΔRA and ΔDEC between calculated and reference values are shown
on forth and fifth panels of Fig. 1. There were no reference stars with B < 20m in the USNO A2.0 catalog
for this sky region. The origin of magnitude scale was determined according to faint stars (B = 16–19m).
The comparison of magnitudes calculated for two frames are shown on third panel of Fig. 1, and at the bottom
of the figure such a comparison with B values of reference catalog is shown. The large dispersion of magnitude
differences is explained by absence of filters during CCD observations because that were made in integral
418
Figure 1. Determination of coordinates and magnitudes errors. Three upper panels demonstrates the differences of
rectangular coordinates ΔX, ΔY and magnitudes ΔMag which have been obtained by data comparison for two frames.
Three lower panels have the differences of equatorial coordinates ΔRA, ΔDEC and magnitudes ΔMag which have been
obtained by comparison of our observations with the data of the USNO A2.0 reference catalog
light. As a whole, the errors of coordinates and magnitudes of objects for eight sky regions investigated were
determined of the USNO A2.0 reference catalog accuracy. The determination of the measuring coordinates
differences and the equatorial coordinates ones for all stars in eight sky regions gives the possibility to calculate
a pixel size in angular units: 1 pixel = 0.4483± 0.0006 arcsec.
The sky region maps with IR/radio sources are shown in Figs. 2 and 3. Field size is 3×3 arcmin. The maps
are obtained by the MIDAS/ROMAFOT software procession of the CCD frames. The geometrical center of
maps to be identified corresponds to the equatorial coordinates (equinox 2000.0) of IR/radio sources’ list [4].
The list of objects which have been registered on the CCD frames is quoted in Table 2 (for every region of
60 arcsec size – such a region is marked out on a map).
Table 2. Equatorial coordinates and magnitudes of objects which are candidates to be the extragalactic IR sources (from
[4]) according to CCD observations (without filters) made at the Andrushivka Astronomical Observatory in July 2002
RA2000 DEC2000 Mag B R
ICRS 1732+389 (17h34m20.5s, 38◦57′51′′); UT = 23h49m46s, July 4, Tex = 840 s
17h34m21.696s 38◦58′06.04′′ 20.1m 19.9m 18.5m
17 34 19.442 38 57 56.30 20.3 – –
17 34 18.709 38 57 51.55 20.9 – –
17 34 20.611 38 57 51.34 19.3 19.5 19.2
17 34 19.979 38 57 50.54 21.1 – –
17 34 20.058 38 57 41.17 19.6 18.5 18.7
17 34 19.201 38 57 39.70 20.3 – –
17 34 22.680 38 57 32.16 20.7 – –
17 34 19.269 38 57 30.78 19.9 – –
419
RA2000 DEC2000 Mag B R
ICRS 1803+784 (18h00m45.6s, 78◦28′04′′); UT = 0h15m30s, July 1, Tex = 360 s
18 00 41.720 78 28 17.01 17.8 17.6 16.6
18 00 46.547 78 28 16.20 20.4 – –
18 00 45.713 78 28 10.00 18.8 – –
18 00 52.326 78 28 06.79 20.7 – –
18 00 45.780 78 28 04.03 16.0 15.5 14.9
18 00 39.747 78 27 46.84 20.4 – –
18 00 42.302 78 27 46.54 20.7 – –
18 00 36.753 78 27 44.35 19.8 – –
ICRS 1807+698 (18h06m50.6s, 69◦49′28′′); UT = 0h59m18s, July 1, Tex = 300 s
18 06 48.652 69 49 51.97 19.6 – –
18 06 50.178 69 49 51.59 19.6 – –
18 06 44.884 69 49 41.66 19.4 – –
18 06 46.589 69 49 33.97 19.5 – –
18 06 50.683 69 49 27.96 14.5 14.3 11.2
18 06 48.552 69 49 24.94 18.7 – –
ICRS 1845+797 (18h42m08.9s, 79◦46′17′′); UT = 22h35m59s, July 9, Tex = 840 s
18 42 09.235 79 46 17.26 15.5 15.0 13.0
18 42 13.372 79 46 11.56 19.8 – –
ICRS 1943+228 (19h46m06.2s, 23◦00′04′′); UT = 0h35m30s, July 6, Tex = 840 s
19 46 05.375 23 00 23.97 20.6 – –
19 46 07.923 23 00 17.57 19.9 – –
19 46 04.747 23 00 13.92 20.9 – –
19 46 08.268 23 00 02.85 18.9 19.4 17.4
19 46 05.811 23 00 00.60 20.7 – –
19 46 05.040 23 00 00.61 21.6 – –
19 46 05.957 23 00 00.44 20.4 – –
19 46 04.115 22 59 58.88 20.6 – –
19 46 04.375 22 59 52.78 21.6 – –
19 46 06.889 22 59 51.66 18.3 19.7 15.9
19 46 06.492 22 59 34.69 21.9 – –
19 46 07.803 22 59 34.33 19.6 – –
19 46 06.818 22 59 31.77 20.2 – –
ICRS 2023+335 (20h25m10.8s, 33◦43′00′′); UT = 0h43m34s, July 4, Tex = 420 s
20 25 09.858 33 43 29.51 17.2 17.0 15.8
20 25 09.909 33 43 24.66 18.8 – –
20 25 10.219 33 43 10.40 20.6 – –
20 25 11.642 33 43 05.68 17.0 17.7 15.8
20 25 10.044 33 43 05.09 21.0 – –
20 25 08.497 33 42 59.55 16.1 15.7 14.9
20 25 09.392 33 42 56.40 18.2 18.7 17.0
20 25 12.454 33 42 52.87 17.5 17.3 16.2
20 25 10.008 33 42 52.39 18.4 19.0 17.3
20 25 11.172 33 42 46.75 19.4 19.2 17.4
20 25 11.327 33 42 36.41 18.2 18.1 17.0
ICRS 2223–052 (22h25m47.2s, –4◦57′01′′); UT = 0h04m54s, July 10, Tex = 900 s
22 25 46.480 -4 56 40.22 20.4 – –
22 25 45.641 -4 56 41.30 20.9 – –
22 25 49.045 -4 56 41.76 19.9 19.7 18.5
22 25 45.234 -4 56 59.11 21.0 – –
22 25 47.234 -4 57 01.02 18.7 17.7 16.7
ICRS 2229+695 (22h30m36.4s, 69◦46′28′′); UT = 23h54m42s, July 9, Tex = 840 s
22 30 33.116 69 46 47.47 21.0 – –
22 30 30.654 69 46 46.49 21.8 – –
22 30 32.456 69 46 39.24 21.1 – –
22 30 37.960 69 46 34.20 21.8 – –
22 30 35.638 69 46 29.20 20.6 – –
22 30 33.254 69 46 28.73 19.8 19.1 18.1
22 30 40.649 69 46 21.80 20.8 – –
22 30 35.294 69 46 10.08 18.5 18.4 17.1
22 30 34.973 69 46 01.39 19.1 18.9 17.6
420
Figure 2. Maps for sky regions which contain IR/radio sources in accordance with optical CCD observations made at
the Andrushivka Astronomical Observatory (ICRS 1732+389, ICRS 1803+784, ICRS 1807+698, ICRS 1845+797)
Figure 3. The same as in Fig. 2 for ICRS 1943+228, ICRS 2023+335, ICRS 2223–052, ICRS 2229+695
421
The list includes equatorial coordinates RA2000, DEC2000, and magnitudes Mag (zero is connected with
the B values’ scale of the USNO A2.0 catalog) of the objects registered. The B and R values from the USNO
A2.0 are also listed (a selection up to B < 20m).
CONCLUSION
The list of optical objects which are candidates to be the IR/radio sources is obtained at the base of CCD
observations’ processing of eight sky regions.
Acknowledgements. This work has been partly supported by the Fundamental Research State Fund of
the Ministry of Ukraine for Education and Science (Grant 02.07/00017) and the Scientific and Technological
Center in Ukraine (Grant NN43).
The authors wish to thank the amateurs of astronomy, the pupils of Andrushivka secondary school No. 1
O. Drobenko, D. Kyrylenko, P. Kyrylenko, O. Pastovens’kii, B. Studyns’kii, and A. Solom’ianiuk for a help in
observations.
[1] MIDAS Users Guide, European Southern Observatory – Image Processing Group 1994, Garching, ESO, 1994.–
Vol. A, B, C.
[2] IRAS Catalogues and Atlases: The Explanatory Supplement // NASA RP-1190 / Eds C. A. Beichman, G. Neuge-
bauer, H. J. Habing, and T. J. Chester, 1987.–Vol. 1–6.
[3] Ivashchenko Yu. M., Andruk V. M. Andrushivka Astronomical Observatory in 2001 // Intern. Astron. Conf.: Ex-
tension and connection of Reference frames using group based CCD technique.–Mykolaiv: Atoll, 2001.–P. 224–230.
[4] Kharin A. C., Kumkova I. I., Vedenicheva I. P. Program of astrometric observations in IR range to improve
the correlation of optical (HIPPARCOS) and radio (ICRF) reference systems // Proc. of First Ukrainian Conference
of Advanced Space Investigations, 8–10 June 2001.–Kyiv, 2001.–P. 78–82.
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