Kyiv Meridian Axial Circle Catalogue (KMAC1) of stars in fields with extragalactic radio sources
The catalogue of astrometric (positions, proper motions) and photometric (B, V , R, r', J) data of stars in 192 fields with the ICRF objects has been compiled at the Main Astronomical Observatory of the National Academy of Sciences of Ukraine and the Astronomical Observatory of the Kyiv Nationa...
Gespeichert in:
| Veröffentlicht in: | Кинематика и физика небесных тел |
|---|---|
| Datum: | 2005 |
| Hauptverfasser: | , , , , , |
| Format: | Artikel |
| Sprache: | Englisch |
| Veröffentlicht: |
Головна астрономічна обсерваторія НАН України
2005
|
| Schlagworte: | |
| Online Zugang: | https://nasplib.isofts.kiev.ua/handle/123456789/79666 |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| Назва журналу: | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| Zitieren: | Kyiv Meridian Axial Circle Catalogue (KMAC1) of stars in fields with extragalactic radio sources / Yu. Babenko, P. Lazorenko, V. Karbovsky, M. Buromsky, S. Kasjan, O. Denysyuk // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 316-321. — Бібліогр.: 6 назв. — англ. |
Institution
Digital Library of Periodicals of National Academy of Sciences of Ukraine| _version_ | 1859555426608087040 |
|---|---|
| author | Babenko, Yu. Lazorenko, P. Karbovsky, V. Buromsky, M. Kasjan, S. Denysyuk, O. |
| author_facet | Babenko, Yu. Lazorenko, P. Karbovsky, V. Buromsky, M. Kasjan, S. Denysyuk, O. |
| citation_txt | Kyiv Meridian Axial Circle Catalogue (KMAC1) of stars in fields with extragalactic radio sources / Yu. Babenko, P. Lazorenko, V. Karbovsky, M. Buromsky, S. Kasjan, O. Denysyuk // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 316-321. — Бібліогр.: 6 назв. — англ. |
| collection | DSpace DC |
| container_title | Кинематика и физика небесных тел |
| description | The catalogue of astrometric (positions, proper motions) and photometric (B, V , R, r', J) data of stars in 192 fields with the ICRF objects has been compiled at the Main Astronomical Observatory of the National Academy of Sciences of Ukraine and the Astronomical Observatory of the Kyiv National University. All fields are located in declination zone from 0° up to +30° ; a nominal field size is 46' (right ascension)×24' (declination). The observational basis of this work is 1100 CCD scans deep to V =17 mag which were obtained with the Kyiv Meridian Axial Circle in 2001–2003 and which contain one million of images. Coordinates of star image centroids have been computed both as the weighted centers of gravity and as the linearized Gaussian profile fitting with unequal weights. Astrometric reductions have included corrections depending on image size fluctuations and position of a star on the CCD frame on the declination axis. A special approach was used for correction of magnitude-dependent errors since images of bright stars were oversaturated. The KMAC1 catalogue is presented in two versions. The KMAC1–T version contains 159 fields (104 796 stars) and was obtained with reduction to the Tycho-2 catalogue. For another 33 fields, the reduction was found to be unreliable due to a low sky density of the Tycho-2 stars. Therefore, transformation the second version of the KMAC1–CU to the ICRF was derived using the UCAC2 and CAMC13 catalogues as reference ones; it contains 115 032 stars in 192 fields and is of slightly better accuracy. As compared with the first version proper motions were derived using the USNOA2.0 catalogue as a first epoch catalogue. An external accuracy (based on comparison with UCAC2 and CMC13) of one catalogue position is about 60–70 mas for 14–15 mag stars. An average value of photometry error is better than 0.1 mag for stars to 16 mag.
|
| first_indexed | 2025-11-26T12:47:37Z |
| format | Article |
| fulltext |
KYIV MERIDIAN AXIAL CIRCLE CATALOGUE (KMAC1) OF STARS
IN FIELDS WITH EXTRAGALACTIC RADIO SOURCES
Yu. Babenko1, P. Lazorenko2, V. Karbovsky2,
M. Buromsky1, S. Kasjan1, O. Denysyuk2
1Astronomical Observatory, National Taras Shevchenko University of Kyiv
3 Observatorna Str., 04053 Kyiv, Ukraine
e-mail: babenko@observ.univ.kiev.ua
2Main Astronomical Observatory, NAS of Ukraine
27 Akademika Zabolotnoho Str., 03680 Kyiv, Ukraine
e-mail: laz@mao.kiev.ua
The catalogue of astrometric (positions, proper motions) and photometric (B, V , R, r ′, J) data of
stars in 192 fields with the ICRF objects has been compiled at the Main Astronomical Observatory
of the National Academy of Sciences of Ukraine and the Astronomical Observatory of the Kyiv Na-
tional University. All fields are located in declination zone from 0◦ up to +30◦; a nominal field size
is 46′ (right ascension)× 24′ (declination). The observational basis of this work is 1100 CCD scans
deep to V = 17 mag which were obtained with the Kyiv Meridian Axial Circle in 2001–2003 and
which contain one million of images. Coordinates of star image centroids have been computed
both as the weighted centers of gravity and as the linearized Gaussian profile fitting with unequal
weights. Astrometric reductions have included corrections depending on image size fluctuations and
position of a star on the CCD frame on the declination axis. A special approach was used for correc-
tion of magnitude-dependent errors since images of bright stars were oversaturated. The KMAC1
catalogue is presented in two versions. The KMAC1–T version contains 159 fields (104 796 stars)
and was obtained with reduction to the Tycho-2 catalogue. For another 33 fields, the reduction
was found to be unreliable due to a low sky density of the Tycho-2 stars. Therefore, transformation
the second version of the KMAC1–CU to the ICRF was derived using the UCAC2 and CAMC13
catalogues as reference ones; it contains 115 032 stars in 192 fields and is of slightly better accuracy.
As compared with the first version proper motions were derived using the USNOA2.0 catalogue as
a first epoch catalogue. An external accuracy (based on comparison with UCAC2 and CMC13) of
one catalogue position is about 60–70 mas for 14–15 mag stars. An average value of photometry
error is better than 0.1 mag for stars to 16 mag.
INTRODUCTION
The Meridian Axial Circle (MAC, D =0.18 m, F =2.3 m) in Kyiv was recently modernized by installing
a 1040×1160 CCD micrometer that can work in scan mode [6]. The micrometer designed at the Nikolaev
Observatory (Ukraine) incorporates a glass filter to enable observations in the V band. With effective exposure
of about 108 s for equatorial stars, the magnitude limit is Vlim =17, and an internal precision of one observation
in the optimal magnitude range of 12–14 mag is about 0.04′′–0.1′′.
The instrument is used in the two observational projects aimed at extending the Hipparcos–Tycho ref-
erence frame to fainter magnitudes. The first project, now completed, concerns star fields in directions of
192 extragalactic ISRF objects in the declination zone from 0◦ up to +30◦. The second, long-term project is
the astrometric survey of the sky in equatorial zone from 0◦ up to +5◦ to obtain astrometric and photometric
data for faint stars [6].
This report describes data reductions and compilation of the Kyiv Meridian Axial Circle Catalogue (KMAC1)
of stars in fields of extragalactic radio reference frame sources. The KMAC1 is a catalogue of astrometric (α, δ,
μα, μδ) and photometric (B, V , R, r ′, J) data for faint stars in 192 fields with ICRF objects. The catalogue was
obtained in the framework of international programs: maintenance of the Hipparcos frame and link of optical
frames to the ICRF. It was obtained in the framework of scientific cooperation between the Main Astronomical
Observatory of the National Academy of Sciences of Ukraine and the Astronomical Observatory of the Kyiv
National University. Besides of direct scientific aims the project allowed to develop infrastructure of the MAC
c© Yu. Babenko, P. Lazorenko, V. Karbovsky, M. Buromsky, S. Kasjan, O. Denysyuk, 2004
316
(experience in maintenance of electronics, optics adjusting, software for performing observations, database,
software for reductions, experience in managing CCD data, etc.)
IMAGE PROCESSING
The basis of the catalogue is formed by 1100 scans each of 24.2′×46.5′ size in the sky. Each of 192 fields was
scanned at least five times. The scanned data was archived and stored to the CD database in the original form.
The data was processed performing next steps of reductions: image processing, removing instrumental errors,
correction of the magnitude scale, reduction to the ICRF frame and, finally, compilation of the catalogue.
A scheme of astrometric reductions and source catalogues used for compilation of the KMAC1 are shown in
Fig. 1.
������� ��
��
���
�����
����
�����������
������ �� � �� ��� �����
������� ��������
�
��
�
���� �
� ����
�
�����
����
����
�������
��
� � ������
����� ����
� � ���
��
�������
� ������ � � ��� �� ����!� " �����
#� $�� � �� ��
�
��
��
��
�
�
�
�
%
�&
'( �( "
Figure 1. Compilation of the KMAC1: main steps of reductions and source catalogues
The first stage of the data reductions starts from a search and extraction of data files with a star field from
the database archive. Then CCD images of stellar fields are filtered from various instrumental and noisy features
which introduce inhomogeneity in a sky level. Inhomogeneity pattern inherent to a scan mode is dominated by
the 1D strip-like structure (Fig. 2) which changes only along declinations (the x-axis on a CCD) with a possible
weak trend over the y-axis (right ascensions). Besides a bias, read-out noise and sky background, the noisy
structure of images are strongly affected by noise from a few dozen of bad bright pixels, which produces vertical
one pixel width noisy strips. Images are also contaminated by a number of flares and treks from radioactive
particles of the cosmic or Chornobyl origin which have coma or star-like shapes (see right low end in Fig. 2).
It was found that noise sources contribute almost as additive factors (a similar conclusion was drawn in [2]).
Therefore, scans were filtered out by means of subtracting running average taken, first, over the x-axis, and then
in a perpendicular direction. Multiplicative noise component was found to be negligible. Filtration procedure
realized as a one-pass program very efficiently clears images and yields almost a perfect constant sky level that
does not show any variations across the image (Fig. 2).
Detection of objects in the noisy field was based on comparison of the pixel flux with a threshold defined
as Idet = [1.1 + (σn − 12)/45] σn, where σn is a local sky noise. For better reliability, candidate images were
preliminary convolved with a Point Spread Function (PSF) equal to a smoothed original star image [2]. It was
required that an object should contain at least two adjacent pixels.
Determination of the star position x, y and the flux V of each object was performed with the two methods:
1) the modified center of gravity [2] and 2) the full profile fitting procedure based on the Gaussian linearized
least squares method. The last method provided for both a circular and elliptical Gaussian model. The least
squares solution was found using original non-smoothed images and, due to a high noise typical for this CCD,
pixels were weighted depending on the pixel counts. The modified center of gravity positions were computed
with images smoothed with a local PSF. The best solution giving final x, y, V values was chosen taking into
account the image brightness and iteration convergence index.
All computations of x, y, V for the data array that contained more than one million of star images have
been performed with an effective original software for about 1.5 hours.
317
a) Original scan b) Scan after filtration
Figure 2. Example of a CCD sky scan filtration from a 1D strip structure; only a small part of a scan is shown
ASTROMETRIC REDUCTIONS
Astrometric reductions started from correcting measured x, y, V values for the instrumental errors of the MAC.
This type of errors is related to oversaturation of bright (V < 12 mag) images and to a slight asymmetry of
stellar profiles in a direction of the CCD x-axis. The amplitude of image distortions was found to depend
on a star position (x coordinate) and its brightness. Distortions lead to a correlation of differences MAC–
CMC13 in declinations with x and σx values, where σx is an image size parameter of the Gaussian model taken
along the x-axis (Fig. 3). A similar effect is also seen in V magnitudes. To remove the correlation, we applied
corrections to the measured x and V values in the form of a polinomial linear with respect to σx. Since the effect
discussed depends on the star magnitude, the coefficient at σx was defined to be dependent on V . The model
coefficient values were found as those which yielded the best intrinsic convergence of star declinations (or star
magnitudes) computed for each scan. Note that this approach of reductions is sensitive only to the variable
part of instrumental errors related to fluctuations of the computed σx values. The differences MAC–CMC13
in declinations computed after instrumental corrections do not show the presence of the correlation; besides,
the variance of residuals had been reduced. Another effect of instrumental nature resulted in a systematic
dependence of MAC–CMC13 differences (declinations and star magnitudes) on x. This error component was
eliminated using computed differences of MAC–CMC13.
It should be noted that above approach to correction of instrumental errors has become possible due to
the availability of the CMC13 catalogue which errors, of course, do not correlate with σx and x values measured
at the MAC.
�
�
�
��
�
�
�
�
�
�
��
�
�
�
δ �
�
��
��
�
������� �����
��
�
�
����
�
�
����
������ ��
��
�� ����
�� ���� �����
��
Figure 3. MAC–CMC13 differences in δ versus σx for the stars of 12–14 mag: before and after correction for instrumental
errors
318
Described procedure is not sensitive to systematic magnitude-dependent errors in x, y and V ; however,
direct inspection of the MAC–Tycho-2 residuals clearly showed on the presence of this error. The systematic
component of the MAC–Tycho-2 residuals was treated as errors in the MAC’s data. Adequate corrections
of x, y and V values were performed by subtracting the systematic effect, that was made, of course, only in
the Tycho-2 magnitude range V < 13 mag.
More explicit analysis however has revealed a presence of seasonal variations in the MAC–Tycho-2 differences
in δ as a function of V . Systematic part of these functions have been fitted with a model function and removed
based on use of the Tycho-2 catalogue, again for stars with V < 13 mag.
REDUCTION TO THE ICRF
The corrected CCD position of stars originally were supposed to be reduced to the ICRF with use of the Tycho-2
catalogue as reference. Prior to this conversion we performed a tentative study to find how well positions of
the Tycho-2 match with the CMC13 and UCAC2 [7]. For that purpose we compared the Tycho-2 star positions
with those given in the CMC13, UCAC2 and in the preliminary version of the KMAC1 catalogue. Figure 4
presents individual differences of right ascensions of Tycho-2–CMC13, Tycho-2–UCAC2 shown versus Tycho-2–
KMAC1 for 1843 Tycho-2 stars used as reference and with a restriction |μα|< 0.3′′/yr. One can notice a good
agreement between three ground-based catalogues which provide positions normally consistent to 0.1′′–0.2′′.
Large deviations, usually for faint V > 12 mag stars, originate from errors in the Tycho-2 catalogue. For
1.4 percent of stars these errors exceed ±0.5′′, and about 12% the errors are larger than ±0.2′′.
������ � ����
�
�
��
�
�
��
�
�
�
��
�
�
��
�
�
��
�
�
Figure 4. Tycho-2–CMC13 (+) and Tycho-2–UCAC2 (×) differences in right ascensions in comparison with the Tycho-2–
KMAC1 differences
Taking into consideration results of the above analysis, one can conclude that a reduction to the ICRF using
the Tycho-2 catalogue can be reliable providing that a number of reference stars is sufficiently large. In our case,
due to a rather short scan length, some fields with a low star density contained just 6–8 Tycho-2 stars, which,
of course, is insufficient for the purpose of a rigorous reduction. In addition, an accuracy of the reduction is
often affected by inhomogeneous sky distribution of reference stars. To obtain more robust results, we used only
those Tycho-2 stars whose positions, as found from a comparison with the CMC13 and UCAC2 catalogues, are
precise to better than ±0.2′′. In this case reliable results were obtained for 106 fields. For some other 53 fields,
a good transformation to the ICRF required rejection of some reference stars with differences Tycho-2–CMC13
and Tycho-2–UCAC2 in the range from ±0.2′′ to ±0.15′′. A reduction procedure for another 33 fields with
a low star density was found to give unstable results wildly reacting on the choice of a reference star set.
Thus, a reduction to the ICRF using the Tycho-2 catalogue was performed only for 159 sky fields with
a high star density. A reliable conversion to the ICRF for the holy data array (192 sky fields) required the use
of the CMC13 and UCAC2 catalogues which are also given in the ICRF system. Thus, the KMAC1 catalogue
had been derived into the two versions: with reduction to the Tycho-2 (KMAC1–T) and with reduction to
the CMC13 and UCAC2 catalogues (KMAC–CU).
319
CORRECTION OF THE V MAGNITUDE SCALE
Star magnitudes of the KMAC1 have been computed using measured V values which were corrected for the in-
strumental errors in a way described above. A zero point of the V magnitude scale was found using the Tycho-2
photometry of bright stars with V < 13 mag. The problem consisted in verification of the magnitude scale
linearity which can not be directly controlled due to the absence of faint all sky standards in the V photometric
band.
For this study we compared V values computed for stars of the open cluster NGC 2264 with those found in
some photometric catalogues. The comparison indicated a systematic shift of magnitude scales up to 0.6 mag.
Further analysis had shown that this error leads to a relative shift between positions of bright and faint stars
in the two colour diagram V – r ′ ∼V – J . The effect was modelled and a necessary corrections applied to
the V magnitudes for each star field.
CHARACTERISTICS OF THE KMAC1 CATALOGUE
Besides of positions and original V values, the catalogue contains: B, R values copied from the USNO–B1 [5];
r ′ values taken from the CMC13; J values copied from the 2MASS [1]; proper motions were derived using
positions in the USNO–A2.0 [4] as a first epoch, in doing this we used the USNO–B1 proper motions for
cross-identification of stars. Main features of the KMAC1 are given in Table 1.
Table 1. Characteristics of the Kyiv Meridian Axial Circle Catalogue of stars in fields with extragalactic radio sources:
versions KMAC1–T and KMAC1–CU
KMAC1–T KMAC1–CU
Reference catalogues Tycho-2 CMC13, UCAC2
The number of fields 159 192
Declination zone 0◦ ÷+30◦ 0◦ ÷+30◦
Nominal field size 46′×24′ 46′×24′
Number of stars 104 796 115 032
V limiting 17 mag 17 mag
Spectral band V (Johnson) V (Johnson)
Precision of positions∗ 30–50 mas, V < 14 mag 30–50 mas, V < 14 mag
160 mas, V = 16 mag; 160 mas, V =16 mag
Precision of photometry∗ 0.03–0.05 mag, V < 15 mag 0.03–0.05 mag, V < 15 mag
External catalogue error∗∗ 50–70 mas, V < 14 mag; 40–60 mas, V < 14 mag;
200 mas, V = 16 mag; 190 mas, V =16 mag;
Mean epoch 2002.3 2002.3
∗) Internal errors
∗∗) Found from residuals
KMAC1–CMC13 and KMAC1–UCAC2
Astronomical data included: α, δ, μα, μδ , B, V , R, r ′, J
0
50
100
150
200
250
300
350
400
450
500
8 10 12 14 16 18
V
0
50
100
150
200
250
300
350
400
450
500
8 10 12 14 16 18
V
a) External errors of the KMAC1–T b) External errors of the KMAC1–CU
Figure 5. External error of the KMAC1 (versions “T” and “CU”) positions estimated as a rms difference with the CMC13
and UCAC2 positions; solid lines – in right ascensions; dashes – in declinations; it is not specified which plot refer to
the CMC13 or UCAC2 since the results are very similar in both cases
320
External error of the KMAC1–T and KMAC1–CU positions estimated as a rms difference of this catalogue
positions with the CMC13 and UCAC2 are shown in Fig. 5. Systematic errors, with reference to the CMC13
and UCAC2, do not exceed ±20 mas.
Acknowledgements. This publication makes use of data products from the Two Micron All Sky Survey, which
is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California
Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science
Foundation.
[1] Cutri R. M., Skrutskie M. F., van Dyk S., et al. The 2MASS All-Sky Catalog of Point Sources.–University
of Massachusetts and Infrared Processing and Analysis Center (IPAC/California Institute of Technology), 2003.
[http://www.ipac.caltech.edu/2mass/].
[2] Evans D., Irwin M. J., Helmer L. The Carlsberg meridian telescope CCD drift scan survey // Astron. and
Astrophys.–2002.–395, N 11.–P. 347–356.
[3] Hoeg E., Fabricius C., Makarov V. V., et al. The Tycho-2 Catalogue of the 2.5 million brightest stars // Astron.
and Astrophys.–2000.–355, N 1.–P. L27–L30.
[4] Monet D., Bird A., Canzian B., et al. A Catalog of Astrometric Standards USNO–A V2.0 // CD-ROM distribution
(U.S. Naval Observatory Flagstaff Station and Universities Space Research Association).–1998.
[5] Monet D. G., Levine S. E., Casian B., et al. The USNO–B Catalog // Astron. J.–2003.–125, N 2.–P. 984–994.
[6] Telnyuk-Adamchuk V., Babenko Yu., Lazorenko P., et al. Observing programs of the Kyiv meridian axial circle
equipped with a CCD micrometer // Astron. and Astrophys.–2002.–386, N 2.–P. 1153–1156.
[7] Zacharias N., Urban S. E., Zacharias M., et al. The second US Naval Observatory CCD Astrograph Catalog
(UCAC2) // Astrophys. J.–2003.–127, N 5.–P. 3043–3059.
321
|
| id | nasplib_isofts_kiev_ua-123456789-79666 |
| institution | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| issn | 0233-7665 |
| language | English |
| last_indexed | 2025-11-26T12:47:37Z |
| publishDate | 2005 |
| publisher | Головна астрономічна обсерваторія НАН України |
| record_format | dspace |
| spelling | Babenko, Yu. Lazorenko, P. Karbovsky, V. Buromsky, M. Kasjan, S. Denysyuk, O. 2015-04-03T18:14:47Z 2015-04-03T18:14:47Z 2005 Kyiv Meridian Axial Circle Catalogue (KMAC1) of stars in fields with extragalactic radio sources / Yu. Babenko, P. Lazorenko, V. Karbovsky, M. Buromsky, S. Kasjan, O. Denysyuk // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 316-321. — Бібліогр.: 6 назв. — англ. 0233-7665 https://nasplib.isofts.kiev.ua/handle/123456789/79666 The catalogue of astrometric (positions, proper motions) and photometric (B, V , R, r', J) data of stars in 192 fields with the ICRF objects has been compiled at the Main Astronomical Observatory of the National Academy of Sciences of Ukraine and the Astronomical Observatory of the Kyiv National University. All fields are located in declination zone from 0° up to +30° ; a nominal field size is 46' (right ascension)×24' (declination). The observational basis of this work is 1100 CCD scans deep to V =17 mag which were obtained with the Kyiv Meridian Axial Circle in 2001–2003 and which contain one million of images. Coordinates of star image centroids have been computed both as the weighted centers of gravity and as the linearized Gaussian profile fitting with unequal weights. Astrometric reductions have included corrections depending on image size fluctuations and position of a star on the CCD frame on the declination axis. A special approach was used for correction of magnitude-dependent errors since images of bright stars were oversaturated. The KMAC1 catalogue is presented in two versions. The KMAC1–T version contains 159 fields (104 796 stars) and was obtained with reduction to the Tycho-2 catalogue. For another 33 fields, the reduction was found to be unreliable due to a low sky density of the Tycho-2 stars. Therefore, transformation the second version of the KMAC1–CU to the ICRF was derived using the UCAC2 and CAMC13 catalogues as reference ones; it contains 115 032 stars in 192 fields and is of slightly better accuracy. As compared with the first version proper motions were derived using the USNOA2.0 catalogue as a first epoch catalogue. An external accuracy (based on comparison with UCAC2 and CMC13) of one catalogue position is about 60–70 mas for 14–15 mag stars. An average value of photometry error is better than 0.1 mag for stars to 16 mag. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. en Головна астрономічна обсерваторія НАН України Кинематика и физика небесных тел MS4: Positional Astronomy and Global Geodynamics Kyiv Meridian Axial Circle Catalogue (KMAC1) of stars in fields with extragalactic radio sources Article published earlier |
| spellingShingle | Kyiv Meridian Axial Circle Catalogue (KMAC1) of stars in fields with extragalactic radio sources Babenko, Yu. Lazorenko, P. Karbovsky, V. Buromsky, M. Kasjan, S. Denysyuk, O. MS4: Positional Astronomy and Global Geodynamics |
| title | Kyiv Meridian Axial Circle Catalogue (KMAC1) of stars in fields with extragalactic radio sources |
| title_full | Kyiv Meridian Axial Circle Catalogue (KMAC1) of stars in fields with extragalactic radio sources |
| title_fullStr | Kyiv Meridian Axial Circle Catalogue (KMAC1) of stars in fields with extragalactic radio sources |
| title_full_unstemmed | Kyiv Meridian Axial Circle Catalogue (KMAC1) of stars in fields with extragalactic radio sources |
| title_short | Kyiv Meridian Axial Circle Catalogue (KMAC1) of stars in fields with extragalactic radio sources |
| title_sort | kyiv meridian axial circle catalogue (kmac1) of stars in fields with extragalactic radio sources |
| topic | MS4: Positional Astronomy and Global Geodynamics |
| topic_facet | MS4: Positional Astronomy and Global Geodynamics |
| url | https://nasplib.isofts.kiev.ua/handle/123456789/79666 |
| work_keys_str_mv | AT babenkoyu kyivmeridianaxialcirclecataloguekmac1ofstarsinfieldswithextragalacticradiosources AT lazorenkop kyivmeridianaxialcirclecataloguekmac1ofstarsinfieldswithextragalacticradiosources AT karbovskyv kyivmeridianaxialcirclecataloguekmac1ofstarsinfieldswithextragalacticradiosources AT buromskym kyivmeridianaxialcirclecataloguekmac1ofstarsinfieldswithextragalacticradiosources AT kasjans kyivmeridianaxialcirclecataloguekmac1ofstarsinfieldswithextragalacticradiosources AT denysyuko kyivmeridianaxialcirclecataloguekmac1ofstarsinfieldswithextragalacticradiosources |