The FONAC catalogue as a result of the FON project
The technique for constructing the first version of the astrographic catalogue FONAC 1.0 based on the measurements of the FON project plates (the Golosiiv overlapping the northern sky) and the Astrographic Catalogue (Carte du Ciel) data is described briefly. The procedure of plate measurements with...
Збережено в:
| Дата: | 2005 |
|---|---|
| Автори: | , |
| Формат: | Стаття |
| Мова: | English |
| Опубліковано: |
Головна астрономічна обсерваторія НАН України
2005
|
| Назва видання: | Кинематика и физика небесных тел |
| Теми: | |
| Онлайн доступ: | http://dspace.nbuv.gov.ua/handle/123456789/79406 |
| Теги: |
Додати тег
Немає тегів, Будьте першим, хто поставить тег для цього запису!
|
| Назва журналу: | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| Цитувати: | The FONAC catalogue as a result of the FON project / V.S. Kislyuk, A.I. Yatsenko // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 33-39. — Бібліогр.: 11 назв. — англ. |
Репозитарії
Digital Library of Periodicals of National Academy of Sciences of Ukraine| id |
irk-123456789-79406 |
|---|---|
| record_format |
dspace |
| spelling |
irk-123456789-794062015-04-01T03:02:46Z The FONAC catalogue as a result of the FON project Kislyuk, V.S. Yatsenko, A.I. Plenary Sessions The technique for constructing the first version of the astrographic catalogue FONAC 1.0 based on the measurements of the FON project plates (the Golosiiv overlapping the northern sky) and the Astrographic Catalogue (Carte du Ciel) data is described briefly. The procedure of plate measurements with the PARSEC measuring machine as well as the methods of their reduction are considered. The results of comparing the FONAC 1.0 with other astrometric catalogues as well as description of the second version of the catalogue FONAC 2.0 are given. Value of the FONAC catalogue series on a background of the Post-Hipparcos astrometry is discussed. 2005 Article The FONAC catalogue as a result of the FON project / V.S. Kislyuk, A.I. Yatsenko // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 33-39. — Бібліогр.: 11 назв. — англ. 0233-7665 http://dspace.nbuv.gov.ua/handle/123456789/79406 en Кинематика и физика небесных тел Головна астрономічна обсерваторія НАН України |
| institution |
Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| collection |
DSpace DC |
| language |
English |
| topic |
Plenary Sessions Plenary Sessions |
| spellingShingle |
Plenary Sessions Plenary Sessions Kislyuk, V.S. Yatsenko, A.I. The FONAC catalogue as a result of the FON project Кинематика и физика небесных тел |
| description |
The technique for constructing the first version of the astrographic catalogue FONAC 1.0 based on the measurements of the FON project plates (the Golosiiv overlapping the northern sky) and the Astrographic Catalogue (Carte du Ciel) data is described briefly. The procedure of plate measurements with the PARSEC measuring machine as well as the methods of their reduction are considered. The results of comparing the FONAC 1.0 with other astrometric catalogues as well as description of the second version of the catalogue FONAC 2.0 are given. Value of the FONAC catalogue series on a background of the Post-Hipparcos astrometry is discussed. |
| format |
Article |
| author |
Kislyuk, V.S. Yatsenko, A.I. |
| author_facet |
Kislyuk, V.S. Yatsenko, A.I. |
| author_sort |
Kislyuk, V.S. |
| title |
The FONAC catalogue as a result of the FON project |
| title_short |
The FONAC catalogue as a result of the FON project |
| title_full |
The FONAC catalogue as a result of the FON project |
| title_fullStr |
The FONAC catalogue as a result of the FON project |
| title_full_unstemmed |
The FONAC catalogue as a result of the FON project |
| title_sort |
fonac catalogue as a result of the fon project |
| publisher |
Головна астрономічна обсерваторія НАН України |
| publishDate |
2005 |
| topic_facet |
Plenary Sessions |
| url |
http://dspace.nbuv.gov.ua/handle/123456789/79406 |
| citation_txt |
The FONAC catalogue as a result of the FON project / V.S. Kislyuk, A.I. Yatsenko // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 33-39. — Бібліогр.: 11 назв. — англ. |
| series |
Кинематика и физика небесных тел |
| work_keys_str_mv |
AT kislyukvs thefonaccatalogueasaresultofthefonproject AT yatsenkoai thefonaccatalogueasaresultofthefonproject AT kislyukvs fonaccatalogueasaresultofthefonproject AT yatsenkoai fonaccatalogueasaresultofthefonproject |
| first_indexed |
2025-07-06T03:27:58Z |
| last_indexed |
2025-07-06T03:27:58Z |
| _version_ |
1836866578839240704 |
| fulltext |
THE FONAC CATALOGUE AS A RESULT OF THE FON PROJECT
V. S. Kislyuk, A. I. Yatsenko
Main Astronomical Observatory, NAS of Ukraine
27 Akademika Zabolotnoho Str., 03680 Kyiv, Ukraine
e-mail: kislyuk@mao.kiev.ua, yatsenko@mao.kiev.ua
The technique for constructing the first version of the astrographic catalogue FONAC 1.0 based
on the measurements of the FON project plates (the Golosiiv overlapping the northern sky) and
the Astrographic Catalogue (Carte du Ciel) data is described briefly. The procedure of plate
measurements with the PARSEC measuring machine as well as the methods of their reduction are
considered. The results of comparing the FONAC 1.0 with other astrometric catalogues as well
as description of the second version of the catalogue FONAC 2.0 are given. Value of the FONAC
catalogue series on a background of the Post-Hipparcos astrometry is discussed.
INTRODUCTION
Astrometry deals with the construction of spatial and temporal reference systems. During the 20th century
the photographic astrometry technique was widely used for this purpose. Photographic observations were very
fruitful at the middle of the last century. That is why photographic astrometry became one of main scientific
directions of the new-born Golosiiv Observatory. For the space of five decades photographic observations were
carried out systematically at this Observatory and some photographic catalogues were compiled.
In the middle of the 1970s the Main Astronomical Observatory (non-official name is the Golosiiv Observatory)
initiated a project of photographic overlapping the sky by means of wide-angle astrographs available in the USSR.
Necessity of new sky surveys has been widely discussed at that time. First of all it was necessary to obtain
new epoch of observations. Besides that available reference frame needed in densification and extension to more
faint objects. One can note some preconditions to these efforts:
– some soviet observatories were supplied with the same type wide-angle astrographs;
– well-known astronomer H. Eichhorn developed the method of overlapping plates;
– new AGK3 reference catalogue has appeared in 1975;
– there were rather reliable first epoch observations given with the Astrographic Catalogue (Carte du Ciel
project);
– at last we had wide experience in the field of photographic astrometry at that time.
FON PROJECT. PHOTOGRAPHIC OBSERVATIONS
The project of fourfold overlapping the northern hemisphere of sky known as FON (Fotografichny Ohlyad Neba –
Photographic survey of the sky) was initiated by I. Kolchinsky and A. Onegina at the Golosiiv Observatory
in 1977 [4]. It was supposed to carry out fourfold overlapping the northern sky by means of the same type
C. Zeiss wide–angle astrographs. In 1982 six observatories of the former USSR started regular observations under
the FON program. Here are these observatories: Abastumani (Georgia), Dushambe (Tajikistan), the Golosiiv
Observatory (Ukraine), Kitab (Uzbekistan), the Kazan Station at Zelenchuk (Russia), Zvenigorod (Russia).
All the astrographs have the same aperture (D =0.4 m) and different focal lengths, namely F =2 m (Dushambe,
Golosiiv, Zelenchuk, Zvenigorod) and F = 3 m (Abastumani, Kitab). The working fields of the astrographs for
all observatories were accepted identical and equal to 4◦×4◦.
All observations were carried out according to uniform coordinated format. Six observatories were combined
into four groups in order to ensure the fourfold overlapping the northern sky. Some characteristics of the FON
project are shown in Table 1.
Between the groups the centres of plates were displaced for 2◦ in right ascension and/or declination. To con-
sider magnitude equation there were two exposures of different duration (on the average 18 min and 40 s)
on each plate, shifted in RA and DEC by about half a millimeter. The astrometric limiting magnitudes of
star images for two exposures on the plates with ORWO ZU-21 emulsion were equal to B = (15 − 16)m and
B = (12 − 13)m, respectively.
c© V. S. Kislyuk, A. I. Yatsenko, 2004
33
Table 1. Some characteristics of the FON project
Overlap Station Latitude Dec Dec Plates Plates
from to required obtained
1 Golosiiv (Ukraine) 50◦ 27′ +32◦ +90◦ 952 ∼ 2300
Kitab (Uzbekistan) 41◦ 45′ −4◦ +32◦ 900 ∼ 500
2 Zelenchuk (Russia) 43◦ 47′ −6◦ +90◦ 1783 1783
3 Abastumani (Georgia) 41◦ 35′ −6◦ +30◦ 900 ∼ 900
Zvenigorod (Russia) 55◦ 45′ +30◦ +90◦ 973 973
4 Dushambe (Tajikistan) 38◦ 33′ −4◦ +90◦ 1762 ∼ 1370
The coordination of observations under the FON program was broken as a result of the USSR disintegration.
As one can see from Table 1, Dushambe and especially Kitab could not carry out observations completely.
That is why at the Golosiiv Observatory were obtained negatives for the whole northern sky including Kitab
overlapping zone. More than 2300 plates were taken.
In parallel with observations the methodical researches were carried out in order to increase accuracy of
determination of coordinates and proper motions of stars. In particular, special series of measurements by
means of semi-automatic measuring machine “Ascorecord” were carried out for investigation of random and
systematic errors (like a coma, magnitude equation and distortion) in determination of star positions from
observations at the Golosiiv Observatory wide-angle astrograph. In 1995 observations were finished and we
began measuring the plates.
MEASUREMENTS
It was decided to apply the FON photographic collection to the determination of positions and proper motions
of all stars in the Astrographic Catalogue (AC) which is the product of well–known international photographic
enterprise “Carte du Ciel”. Photographic observations started in 1891 within the project were finished only
in the early 1950s. At present, some versions of the AC are available. The most generally used of them are
the AC2000 and AC2000.2 [7] which consist of positions of 4 millions of stars up to 14m on the whole sky based
on the new reduction of measured coordinates to the Hipparcos catalogue system. We used the AC2000 in two
ways: (i) as the input catalogue for automatic measuring machine, and (ii) as the first epoch of observations
for determination of stars’ proper motions.
About 1600 the best Golosiiv plates were selected for measurements. In addition, 90 Kitab plates for
equatorial zone were used as well. Measurements of such plenty of negatives were made by means of automatic
measuring machine PARSEC (Programming Automatic Radial-Scanning Coordinatometer). The device consist
of an optical-mechanical part KOMESS, electronic-recording block and microcomputer. Four such complexes
were installed at the Golosiiv, Nikolaev and Pulkovo observatories as well as at the Sternberg Astronomical
Institute in Moscow. The complex can work in a mode of automatic measurement of the images on astronegatives
under the given list of stars. Operator can also choose objects of measurement independently with the further
automatic registration of coordinates. Depending on accuracy of input coordinates of stars PARSEC measures
automatically from 400 up to 900 images per hour.
The carried out researches have shown that PARSEC provides more accurate and homogeneous (depend-
ing on diameters of star images) measurements than executed manually on measuring device “Ascorecord”.
The random errors of coordinate measurements by means of PARSEC are on average ±2.8 microns for a long
exposures and ±2.1 microns for a short ones.
All the plates were measured by means of Kyiv PARSEC. About 80 astronegatives were repeatedly measured
on the same device at the Nikolaev Observatory for estimation of measurement quality.
PLATE ADJUSTMENT
All the plate measurements were reduced twice. Firstly the PPM catalogue was used as the reference system
which gave us about 100 reference stars on the working field 4◦×4◦. Plate parameters were obtained from joint
solutions of connection equations for both exposures to eliminate of coma and magnitude equation effects. These
solutions were carried out using the Gramm–Schmidt orthogonalization method. The statistical F -criterion was
used for estimation of significant terms number in the reduction models. Later on, after appearance of two catalo-
gues: (i) AC2000 (positions of star of all AC zones in the Hipparcos system) and (ii) ACT (combined data of both
AC2000 and Tycho catalogues), new reduction of the FON project plates was carried out. The ACT catalogue
34
was used as the reference one and the AC2000 data were used as the first observation epochs. By the way
average epoch of the ACT catalogue (1991.25) is closer to average epoch of the Golosiiv part of the FON program
(1989.19) rather than of the catalogue PPM, which average epoch is close to 1931.0. Therefore, new reduction
of the measured coordinates using the catalogue ACT as reference one was carried out [9]. The reduction
was individually made for each exposures. The average random errors of weight unit are equal to ±2.5, ±3.0
microns (for long and short exposures, respectively). Proper motions of stars were obtained from comparison
of their reduced coordinates with the same ones taken from the AC2000 catalogue. For correction of a residual
aberrations the method of masks was used. The masks were constructed from analysis of differences of star
positions given in the Guide Star Catalogue (GSC) and FON data in individual intervals of star magnitudes
(see Fig. 1).
Figure 1. The plate masks of the Golosiiv wide-angle astrograph (working field is equal to 4◦×4◦, width of cross is equal
to 2′′)
The aberration masks for the Golosiiv wide-angle astrograph (GWA) were used for taking into account
the errors of measured coordinates depending on positions and magnitudes (mainly, like coma and magnitude
equation). Besides that the aberration masks for the Palomar Schmidt Telescope were constructed as well from
comparison of the FON and GSC data (see Fig. 2).
These masks are in a good coincidence with those constructed by other independent investigators. One can
see that aberration pattern is more complicated for the Palomar Schmidt Telescope than in the case of GWA.
PHOTOMETRY
Determination of photometric characteristics of stars was the next step. Using the automatic measuring ma-
chine PARSEC the diameters (D) of star images on each plate were measured. Photometric data taken from
the catalogue ACT were used for the final calibration of the measured machine magnitudes of stars and deter-
mination of BJ -magnitudes of stars in the Johnson photometric system. Colour indexes (B −V ) were obtained
using the V -magnitudes from the GSC1.1 catalogue reduced to the Johnson system (V ). In the same way
R-magnitudes, given in the USNO-A2.0 catalogue, were applied to obtain the colour indexes (B − R) of stars.
COMPILING THE FONAC 1.0 CATALOGUE
As a result of processing the measured data we obtained about 1700 separate files with calculated positions,
proper motions and photometric characteristics of stars for each FON project plate. Taking into account that
35
there were two exposures on plates, and some plates contained overlapping working fields, the part of stars had
several coordinates and photometry determinations on different epoch of observations. Therefore, all the star
data were reduced to general epoch J2000.0 and the final catalogue was obtained as mean-weighted of all
determinations. The final catalogue was called FONAC (FON+AC) [3]. That is a combination of the FON and
AC data. The first version of the FONAC catalogue consists of positions, proper motions and BJ -magnitudes
for 2 004 701 stars of the Astrographic Catalogue list, including the (B−V )J -magnitudes for 1 712 420 stars and
(B −R)J -values for 1 779 442 stars in 93 one-grade zones of declinations (from −2◦ to +90◦). The mean epoch
of catalogue is 1988.19. Mean precision of the catalogue for stars brighter than 10m is ±0.2′′, ±0.003′′/yr and
±0.18m in positions, proper motions and magnitudes of stars, respectively. The errors are increasing for more
bright and more faint stars.
The FONAC 1.0 catalogue [3] is available on the Main Astronomical Observatory of the NAS of Ukraine
home page [ftp://ftp.mao.kiev.ua/pub/astro/fonac]. It was transferred to the Strasbourg Centre of Stars
Data [http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=I/261] and was distributed on CD-discs.
Figure 2. The plate masks of the Palomar Schmidt Telescope (working field is equal to 6.5◦ × 6.5◦, width of cross is
equal to 2′′)
CATALOGUE COMPARISON
The FONAC catalogue having been compiled, the appropriate control of accuracy of the obtained results was
carried out at each stage of processing the measurements. However, all derived estimates of errors basically
characterized only internal accuracy of the catalogue. For investigation of real accuracy there was necessary
a comparison with other independent sources which would have high accuracy of the data on epoch close to
average epoch of our catalogue and for all range of star magnitudes [10].
Positions and proper motions of stars given in the FONAC catalogue were compared to the high-precision
catalogues: space-born Hipparcos (error of positions and proper motions are ±0.001′′ and ±0.001′′/yr, respec-
tively) and ground-based CMC11 (±0.06′′ and ±0.004′′/yr). 41 759 stars were selected from the Hipparcos
catalogue and 66783 stars – from the catalogue CMC11 after their identification. Systematic differences Δi
between these catalogues were represented by a series development using product of Hermite Hp(y(m)) and
Legendre Ln(x(δ)) polynomials as well as the Fourier Fkl(α) terms depending on equatorial coordinates (αi, δi)
and brightness (mi) as [6]:
36
Δi =
g∑
j=1
Yj(αi, δi, mi)bj , (1)
Yj = Rpnk Hp(y(m))Ln(x(δ))Fkl(α) , (2)
where bj are unknown coefficients of the development series. At comparison we were limited to the terms of
the first order of developments which depend on magnitude and terms of the second order – from coordinates.
Thus, the maximum quantity of the terms of developments was accepted equal to 30. Significant (at 1% level
of significance) coefficients bj of developments for differences (FONAC–Hipparcos) are given in Table 2.
Table 2. Some terms of development of differences (FONAC−Hipparcos)
For For For For
j p n k l Δα cos δ Δδ Δμα cos δ Δμδ
(0.001′′) (0.001′′) (0.001′′/yr) (0.001′′/yr)
1 0 0 0 0 −3.9 ± 0.9 −4.0 ± 1.0 – 0.01 ± 0.002
3 0 0 1 1 – – −0.07 ± 0.02 –
16 1 0 0 0 −2.5 ± 0.9 – −0.06 ± 0.02 –
17 1 0 1 –1 – – 0.10 ± 0.02 –
18 1 0 1 1 – – 0.06 ± 0.02 0.06 ± 0.02
20 1 0 2 1 – – – −0.05 ± 0.02
23 1 1 1 1 – −3.0 ± 1.0 – –
30 0 0 1 1 – – −0.06 ± 0.02 –
The mean square differences of coordinates for all stars in FONAC–Hipparcos comparison are approximately
±0.004′′ in both coordinates, and ±0.0001′′/yr for proper motions of stars. Taking into account these systematic
differences we practically do not change the square differences of coordinates and proper motions of stars which
are ±0.18′′ and ±0.19′′ for coordinates α and δ, respectively, and equal ±0.0037′′/yr on average for the proper
motions of stars.
The mean square differences of coordinates and proper motions in (FONAC–CMC11) after considering
the significant coefficients of developments are on average ±0.24′′ for positions and ±0.005′′/yr for proper
motions in both coordinates. The same estimates for the differences (Hipparcos–CMC11) are equal to ±0.1′′
and ±0.0037′′/yr, respectively. If considering the errors of CMC11 catalogues in the mean square differences
(FONAC–CMC11), we obtain the same values for the accuracy of FONAC catalogue that in the case of compa-
rison to the Hipparcos catalogue (namely: ±0.2′′ and ±0.004′′/yr for positions and proper motions, respectively).
Dependencies of random errors of the FONAC catalogue from star magnitudes were obtained from compa-
rison between the specified catalogues in individual intervals of star magnitudes (see Fig. 3). One can see that
for stars brighter 6m and fainter 14m these errors increase up to ±0.3′′ and ±0.006′′/yr for positions and proper
motions, respectively.
GALAXY KINEMATICS
The FONAC data were used to determine some kinematic parameters of the Milky Way, in particular the Oort
constants, direction of solar apex, secular parallaxes as well as galactic rotation. The most general Ogorodnikov–
Milne model [5] was chosen for this purpose. This model, which considers the solar motion, differential rotation
and space deformation of the Galaxy, was applied to the FONAC catalogue stars in three bands with different
colour indexes (B−V ) and proper motions (μα cos δ, μδ) ≤ 0.05′′/yr, namely: (B−V ) < 0.5m, 0.5m < (B−V ) <
1.0m, (B − V ) > 1.0m. The following parameters have been estimated: P = M12, Q = W21 are the Oort’s
constants; C = 0.5(M11−M22), K = 0.5(M11 +M22)−M33, N = M13 +W13, D = W32 −M23, L = W13 −M13,
R = W32 + M32 are the parameters, describing rotation and space deformation of the Galaxy (here Mij are
elements of the rotation matrix in the Ogorodnikov–Milne theory). The most significant kinematic parameters
are given in Table 3 (in 0.0001′′/yr). These values are obtained rather reliable. The rest of parameters, which
describe rotation and deformation in the planes XZ and Y Z, are very small and not always reliable, besides
the parameter W13 = −6 ± 1 (describing rotation in the XZ plane), which is reliably obtained.
Our results are in a good coincidence with the data obtained by V. Vityazev [8] and V. Bobylev [1] from analy-
sis of stars’ proper motions in the Hipparcos catalogue. The direction of solar apex obtained from the FONAC
and Hipparcos data are in a good coincidence as well.
37
Figure 3. Dependences of random errors of the FONAC catalogue from star FONAC 1.0 found from comparison to
the Hipparcos catalogue
NEW VERSION OF THE CATALOGUE (FONAC 2.0)
At the beginning of 2000 new version of the Tycho catalogue (Tycho-2) [2] had appeared which consists of nearly
in 2.5 times more stars and has considerably more precise positions and proper motions than its predecessor
Tycho-1. A little later there was accessible a catalogue AC2000.2 [7], made on the basis of a new reduction of
the AC plates and with star magnitudes specified from the Tycho-2 catalogue. Therefore, there was an oppor-
tunity to use the new reference catalogue to improving an accuracy of reduction of the measured coordinates
in particular to exclude magnitude equation errors.
Indeed, the accuracy of determination of plate constants was considerably improved. The corresponding
root-mean-square errors had been decreased almost twice. However, an accuracy of new equatorial coordinates
and proper motions of stars did not differ from those found in the first FONAC catalogue version. That is why
Table 3. Kinematic parameters obtained from analysis of the FONAC and Hipparcos catalogue data (in 0.0001′′/yr)
Parameters FONAC [11] Hipparcos Hipparcos
Vityazev [8] Bobylev [1]
Q −25 ± 1 −25 ± 3 −27.0 ± 0.8
P +26 ± 1 +29 ± 4 +24.3 ± 1.1
C −14 ± 1 − −
K −11 ± 2 − −
W13 −6 ± 1 −5 ± 3 −3.6 ± 1.5
W23 +2 ± 1 −1 ± 3 −
M13 − +2 ± 4 −
M23 −2 ± 1 −2 ± 3 −
SOLAR APEX
l +64.0◦ ± 0.5◦ +61.0◦ ± 0.3◦ –
b +19.0◦ ± 0.5◦ +11.0◦ ± 0.3◦ –
The number of stars 910 395 113 710 –
38
we conclude that the version FONAC 2.0 is the limit of increasing the catalogue accuracy owing to use both
new reduction models and new reference catalogue.
FUTURE PROSPECTS
Is there a future for the FON project? And what kind is this future? As one could understand we extracted
astrometrical information only concerning to stars of 12th or 13th magnitudes from one photographic overlap-
ping the sky. The FONAC catalogue we consider as a pilot product of the FON project. Theoretically we have
possibility to improve and extend of the FONAC data up to stars of 15–16 magnitudes in two ways: (i) by
re-measuring the Golosiiv FON plates and (ii) by measuring the plates obtained within other three overlapping
the northern sky (Abastumani+Zvenigorod, Dushambe and Zelenchuk) in order to use completely the advan-
tages of a method of fourfold overlapping the sky. It would enable us to increase accuracy of star positions
approximately twice.
However, there are some difficulties with measurements of such plenty of material, because measuring ma-
chines like PARSEC are obsolete both morally and physically. Thus, we study now a possibility of plate measure-
ments by means of scanners. In particular, five FON plates were tested using scanner Microtek ScanMaker which
resolution is equal to 900× 900 pixels on inch. The rectangular coordinates and photometric characteristics of
stars were obtained using a program complex MIDAS/ROMAFOT. The reductions of rectangular coordinates
were carried out with the Tycho-2 catalogue as the reference one. After corrections of rectangular coordinates
of stars for systematic errors of the scanner (±3 mkm on x and ±21 mkm on y) and averaging the results of
several scans the final errors of determination of positions and photometry consist of about ±(2–3) mkm (0.2′′)
and ±0.2m, respectively.
Hence, it is possible to achieve accuracy of a measuring device like PARSEC scanning the plates by means
of qualitative enough scanners. It gives us a hope to increase an accuracy of star positions approximately twice
after full realization of the FON project possibilities. It is also supposed that in some time the FON data will
be used as the first epoch of observations for CCD-surveys of the sky.
Acknowledgements. We express our deep thanks to Drs. G. A. Ivanov, L. K. Pakulyak, A. V. Sergeev,
and T. P. Sergeeva for collaboration in constructing the FONAC catalogue and to Drs. V. M. Andruk and
M. T. Pogoreltsev for scanning the FON plates and processing the scans.
[1] Bobylev V. V. How inertial is the Hipparcos catalogue? // Motion of Celestial Bodies, Astrometry and Astronomical
Reference Frames: JOURNEES 1999 and IX Lohrmann–Colloquium.–Dresden, Germany, September 13–15, 1999.–
P. 11–13.
[2] Høg E., Fabricius C., Makarov V. V., et al. The Tycho-2 catalogue of the 2.5 million brightest stars // Astron.
and Astrophys.–2000.–355.–P. L27–L30.
[3] Kislyuk V. S., Yatsenko A. I., Pakuliak L. K., et al. FONAC: The astrographic catalogue of the FON project //
Kinematics and Physics of Celestial Bodies.–2000.–16, N 6.–P. 483–496.
[4] Kolchinsky I. G., Onegina A. B. Plan of celestial photography with wide–angle astrographs // Asrometriya i
Astrofizika.–1977.–33, N 1.–P. 11–16.
[5] Ogorodnikov K. F. Dynamics of stellar systems.–Moscow: Fizmatgiz, 1958.–627 p. (in Russian).
[6] Schwan H. A computer program for evaluating the analytic representation of the systematic differences between
FK4 and FK5 or other catalogues of positions and proper motion // Astron. and Astrophys.–1988.–198, N 1/2.–
P. 363–364.
[7] Urban S. E., Corbin T. E., Wycoff G. L., et al. The AC 2000.2 Catalogue // American Astronomical Society,
199th AAS Meeting.–Bull. Amer. Astron. Soc.–2001.–33.–P. 1494.
[8] Vityazev V. V. Physical completeness of the classical models of the galactic rotation // Kinematics and Physics of
Celestial Bodies.–1990.–6, N 4.–P. 74–82.
[9] Yatsenko A. I. Reduction of the measurements of the FON program plates with the use of USNO ACT data //
Kinematics and Physics of Celestial Bodies.–2000.–16, N 1.–P. 67–71.
[10] Yatsenko A. I. Comparison of coordinates and proper motion of FONAC stars with Hipparcos and CMC11 data //
Kinematics and Physics of Celestial Bodies.–2000.–16, N 3.–P. 261–265.
[11] Yatsenko A. I. Determination of the kinematic parameters of the Galaxy from the FONAC catalogue data //
Kinematics and Physics of Celestial Bodies.–2000.–17, N 2.–P. 166–171.
39
|