[show abstract][hide abstract] ABSTRACT: We present the results of determination of Pluto's positions derived from
photographic plates taken in 1930 - 1960. Observations were made with Normal
Astrograph at Pulkovo Observatory. Digitization of these plates was performed
with high precision scanner at Royal Observatory of Belgium (ROB Digitizer).
Mean values of standard errors of plate positions (x,y) lie between 12 and 18
mas. The UCAC4 catalogue was used as an astrometric calibrator. Standard errors
of equatorial coordinates obtained are within 85 to 100 mas. Final table
contains 63 positions of Pluto referred to the HCRF/UCAC4 frame.
[show abstract][hide abstract] ABSTRACT: The trigonometric parallaxes of 71 stars with large proper motion were
determined with the 26-inch refractor at Pulkovo Observatory. Relative
parallaxes of the targets were derived using three or four separate
series of observations (three or four pointings over 1.5 or 2 years for
each one). Observations were performed over the period 2007-2011. We
used from 5 to 20 reference stars per field. We applied a correction
from relative to absolute parallax based on the photometric parallaxes
of reference stars. The latter were estimated from infrared colours (J -
Ks) and the reduced proper motions of reference stars, and from
simulated colour-magnitude diagrams. The trigonometric parallaxes of 30
stars out of our 71 targets were previously unknown. In most cases,
typical standard errors were 2 to 6 mas. The General Catalogue of
Trigonometric Stellar Parallaxes contains data for 41 stars of our 71
targets. On the whole, Pulkovo parallaxes are in a good agreement with
Yale results. The values of parallax differences are within -5 mas to +5
mas in 25 of the 41 stars. Considerable discrepancies are revealed in
several cases. They may be explained by the presence of systematic
errors in the data of both projects or by possible orbital motions not
taken account for the case of double stars. The targets are mostly main
sequence M-dwarfs closer than 50 pc. Three stars are white dwarfs and
five stars are halo subdwarfs.
Monthly Notices of the Royal Astronomical Society 10/2013; 435(2):1083-1093. · 5.52 Impact Factor
[show abstract][hide abstract] ABSTRACT: Long series of astrometric observations of asteroids have been obtained
with Pulkovo Normal Astrograph (1949-2010). Observations of selected
asteroids were begun since 1949. Photographic observations were
performed before 2005. Only CCD observations are carried out with the
Normal Astrograph since 2005. At present the observational program
includes near 300 asteroids: 14 selected asteroids for analysis of
linking of reference systems, double asteroids, NEOs, asteroids of
families of Eos and Hygiea. All results are available via our database
(http://www.puldb.ru). Digitization and new reduction of old
photographic plates has been performing since 2010.
[show abstract][hide abstract] ABSTRACT: Astrometric CCD observations of 1123 stars with large proper motions (µ > 300 mas yr−1) from the LSPM (I/298) catalog in the declination zone +30°–+70° have been carried out with the Pulkovo normal astrograph
since 2006. The observational program includes mostly stars that previously have not entered into high-accuracy projects to
determine the proper motions. Our studies are aimed at determining new proper motions of fast stars in the HCRF/UCAC3 system
and searching for stars with invisible companions in the immediate Galactic neighborhoods of the Sun. Having analyzed about
10 000 CCD frames, we have obtained the equatorial coordinates of 414 program stars in the HCRF/UCAC3 system at an accuracy
level of 10–50 mas and determined their new proper motions. To derive the proper motions, we have used the data from several
star catalogs and surveys (M2000, CMC14, 2MASS, SDSS) as early epochs. The epoch differences range from 5 to 13 years (on
average, about 10 years); the mean accuracy of the derived proper motions is 4–5 mas yr−1. For 70 stars, we have revealed significant differences between the derived proper motions and those from the LSPM and I/306A
catalogs (these proper motions characterize the mean motion of the photocenter in 50 years or more). Apart from systematic
errors, these differences can result from the existence of invisible components of the program stars.
KeywordsGalactic solar neighborhoods–stars with large proper motions–astrometric binaries
[show abstract][hide abstract] ABSTRACT: While implementing the first stage of the Pulkovo program of research on stars with large proper motions, we determined the
trigonometric parallaxes of 29 stars (12
< V < 16
) based on CCD observations with a 26-inch refractor. The mean standard error was 3.7 mas. Comparison of the Pulkovo parallaxes
with those obtained at the Observatory of the Yale University and the US Naval Observatory (USNO) has shown that the parallax
differences (Pulkovo-Yale/USNO) lie within the limits of their measurement errors in an overwhelming majority of cases. On
average, they are −0.6 ± 1.0 mas. No systematic dependences on stellar distance, magnitude, and color in this set of differences
have been found. Our comparisons show that the observing and data reduction techniques used in the Pulkovo program of research
on fast stars allow highly accurate trigonometric parallaxes of these objects to be obtained. All program stars are within
50 pc of the Sun; most of them belong to the immediate solar neighborhood (D < 25 pc). For two stars (J0522+3814 and J1202+3636), the trigonometric parallaxes have been determined for the first time.
Key wordstrigonometric parallaxes-Galactic solar neighborhoods-stars with large proper motions
[show abstract][hide abstract] ABSTRACT: We present the results of 3489 astrometric observations for 361 visual double stars performed in 2003–2007 with the 26-inch
refractor of the Pulkovo Observatory. The angular separations between the components (ρ) and the position angles (θ) are given. The errors in these quantities are, on average, 0″.009 for ρ and 0°.40/ρ for θ, where ρ is the separation in arcseconds.
Key wordsvisual double stars-positional data
[show abstract][hide abstract] ABSTRACT: Context. In 2003, the Sun and the Earth passed through both the equatorial plane of Jupiter and therefore the orbital planes of its main satellites. Aims. During this period, mutual eclipses and occultations were observed and we present the data collected.Methods. Light curves of mutual eclipses and occultations were recorded by the observers of the international campaign PHEMU03 organized by the Institut de mécanique céleste, Paris, France. Results. We completed 377 observations of 118 mutual events from 42 sites and the corresponding data are presented in this paper. For each observation, information about the telescope, receptor, site, and observational conditions are provided.Conclusions. This paper gathers all data and indicates a first estimate of its precision. This catalogue of these rare events should constitute an improved basis for accurate astrometric data useful in the development of dynamical models.
[show abstract][hide abstract] ABSTRACT: Astrometric and photometric observations of major planets, their satellites and asteroids have been made with the 26-in. refractor of the Pulkovo observatory during the period from 1995 to 2006. The CCD (ST6) and photographic observations were carried out. Accurate relative position of satellites of Jupiter and Saturn have been derived. The positions of Saturn have been calculated using the theoretically predicted coordinates of satellites relative to the planet without measurements of the photographic images of the planet. Also the observations of Hale Bopp comet and Mercury transit have been made. The 26-in. refractor has been included into the international campaign PHEMU-2003: photometric CCD observations of mutual occultations and eclipses of Galilean satellites. The light curves of the events have been obtained and parameters of the events have been determined.
Planetary and Space Science 01/2008; 56:1908-1912. · 2.11 Impact Factor
[show abstract][hide abstract] ABSTRACT: We provide an overview of the main results obtained as part of the programs for astrometric observations of bodies in the
Solar system at the Pulkovo Observatory over the period 1898–2005. We summarize the results of photographic observations and
show new possibilities for astrometric observations in connection with the transition to CCD detectors on Pulkovo instruments.
Observing and data reduction techniques are considered. A database with Pulkovo observations of bodies in the Solar system
has been created and opened to users. The database is accessible at http://www.puldb.ru.
Solar System Research 01/2007; 41(1):72-80. · 0.56 Impact Factor
[show abstract][hide abstract] ABSTRACT: In 1995, a CCD camera (ST-6) was attached to the 26-inch Pulkovo
refractor, with which the systematic observations of binary stars and
satellites of major planets were continued simultaneously with their
photographic observations. We present the results of our
relative-position measurements for the components of 15 binaries and 36
pairs of Saturn's satellites. The required calibration and methodical
studies are conducted. We conclude that CCDs can be used to advantage in
long-focus astrometry. The measurement accuracy doubled in comparison
with the photographic method, the resolution limit decreased to 12, and
the limiting magnitude increased by 5 magnitudes.
[show abstract][hide abstract] ABSTRACT: A catalogue of positions and proper motions of 58483 stars (Pul-3) has been constructed at the Pulkovo observatory. The Pul-3 is based on the results of measurements of the photographic plates ((x,y)-data) with galaxies (Deutsch's plan). The observations were made with Pulkovo Normal Astrograph (F=3467mm, D=330mm) during the periods from 1935 till 1960 (the first epoch) and from 1969 till 1986 (the second epoch). The radius of working field was 50 arcmin for all plates. The exposure times were 1 hour. All plates were taken near the meridian. The measurements of the plates were made at the Pulkovo observatory in 1970-s and in 1980-s with ASCORECORD measuring machine. Photographic magnitudes of these stars have been determined at the Pulkovo observatory. The Pulkovo plates contain stars mainly 12-16.5 magnitudes in 146 field in declination zone from -5 to +85 degrees. The maximal density of stars in the Pulkovo plates is 500 stars per square degree. The Tycho-2 catalogue (Cat. ) has been used as a reference catalogue for astrometric reductions of the photographic plates. The great stars density of the Tycho-2 provides 40-65 reference stars in working field of the Pulkovo plates. Only approximate equatorial coordinates of the optical centers of all plates had been known in initial stage of construction of the Pul-3 catalogue and thus recalculation of ones has been done. A six-parameter plate model has been used for the astrometric reduction of the plates. The residuals of the tangential coordinates of reference stars have been analysed to investigate residual systematic errors. The coma parameters have been determined and coma-dependent systematic errors have been excluded. The magnitude-dependent systematic errors and color-dependent ones were investigated. The most significant corrections for magnitude equation have been obtained for stars brighter than 9 magnitude and fainter than 14 magnitude. The most significant color corrections have been obtained in equatorial zone for declinations of stars. The corrected coordinates of all stars have been determined. On the whole, recalculation of the plates optical centers and taking into account of all revealed systematic errors provide improvement of the accuracy of coordinates of stars on 64mas and 51mas for right ascension and declination correspondingly. The new proper motions have been determined for all stars. The mean position has been calculated at the mean epoch of observations of each star using it proper motion. The mean epoch of the Pul-3 is 1963.25. The internal positional accuracy of the Pul-3 catalogue at the mean epoch of observations is 80mas. The internal accuracy of the proper motions is 5mas/yr. Comparisons of the Pul-3 with Tycho-2 and ARIHIP have been done. The Pul-3 external positional accuracy relative to Tycho-2 is 150mas at the mean epoch of the Pulovo plates. The Pul-3 catalogue successfully represents the Tycho-2 system for more than 50000 stars which are fainter than 12 magnitude in 146 fields. The stars from the Pul-3 catalogue may be used as reference stars for reductions of the positional CCD-observations of the extragalactic radio sources and small bodies of the Solar system. The 40-years difference between Pul-3 observational epoch and modern epoch will allow to determine high precision proper motions of the faint stars of the Pul-3 catalogue (about 2mas/yr-3mas/yr). Proper motions of stars from Pul-3 catalogue may be used for stellar kinematics investigations. There are two data files for user's convenience: - the file pul3.dat represents the Pul-3 catalogue; - the file centers.dat contains the equatorial coordinates of centers of the Pulkovo fields (RA, DE). (2 data files).
[show abstract][hide abstract] ABSTRACT: The results of astrometric observations of Saturn’s satellites (S1–S8) obtained using a 26-inch refractor and a normal astrograph The results of astrometric observations of Saturn’s satellites (S1–S8) obtained using a 26-inch refractor and a normal astrograph
at Pulkovo Observatory in 2004–2007 are given. High-accuracy equatorial coordinates of Saturn’s satellites in the system of at Pulkovo Observatory in 2004–2007 are given. High-accuracy equatorial coordinates of Saturn’s satellites in the system of
the UCAC2 reference catalog and the relative “satellite-satellite” positions suitable for specifying their motion theories the UCAC2 reference catalog and the relative “satellite-satellite” positions suitable for specifying their motion theories
are obtained. The observations are compared with the DE405 + TASS1.7 and INPOP06 + TASS1.7 theories of motion. The root-mean-square are obtained. The observations are compared with the DE405 + TASS1.7 and INPOP06 + TASS1.7 theories of motion. The root-mean-square
errors of the obtained satellite positions lie within the range of 10–50 mas, as far as the intrinsic convergence is concerned, errors of the obtained satellite positions lie within the range of 10–50 mas, as far as the intrinsic convergence is concerned,
and 20–70 mas, as far as the extrinsic one is concerned. The observation results are included into the astrometrical database and 20–70 mas, as far as the extrinsic one is concerned. The observation results are included into the astrometrical database
of the Pulkovo Observatory (www.puldb.ru).
Solar System Research 43(4):285-290. · 0.56 Impact Factor
[show abstract][hide abstract] ABSTRACT: In 2009, in five Russian observatories photometric observations of Jupiter’s Galilean satellites during their mutual occultations
and eclipses were carried out. Based on these observations, an original method was used to ascertain astrometric results such
as the difference between the coordinates of pairs of satellites. Fifty-three phenomena were successfully observed. A total
of 94 light curves of satellites were measured. The error in the coordinates of satellites due to random errors in photometry,
calculated on all data obtained, was 0.041″ in right ascension and 0.046″ in declination. The discrepancies between the theory
and observations in these coordinates was found to be 0.060″ and 0.057″, respectively. The results were uploaded to the common
database for all observations of natural satellites of planets at the Natural Satellites Data Center (NSDC), which is available
online at http://www.sai.msu.ru/neb/nss/index.htm. For the first time in the practice of photometric observations of satellites in epochs of mutual occultations and eclipses
a new method of observation was tested, which eliminates from astrometric results the major systematic errors caused by an
inaccurate account of the background level. The tests were conducted in the Terskol Observatory and the observatory of the
Crimean laboratory of the Sternberg State Astronomical Institute of the Moscow State University. The application of the new
method showed that the elimination of the background level at these observatories was carried out correctly.
Solar System Research 45(3):264-277. · 0.56 Impact Factor