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On the Use of Statistical Parallaxes for the Proper Motion Reductions

Published online by Cambridge University Press:  19 July 2016

N.M. Bronnikova  and
N.A. Shakht
N.M. Bronnikova
Affiliation:
Central Astronomical Observatory, USSR Academy of Sciences Pulkovo 196140 Leningrad USSR
N.A. Shakht
Affiliation:
Central Astronomical Observatory, USSR Academy of Sciences Pulkovo 196140 Leningrad USSR

Extract

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The Pulkovo program of determination of proper motions with respect to galaxies approaches completion. It consists of 157 fields from +90° to −4° of declination. The proper motions and reductions with use of galaxies were derived for all areas. The errors of reductions are equal to ± 0.″006. In addition the statistical reductions Rx, Ry were computed for the control and for the zones of avoidance. The following formulae were used: where is the secular parallax according to Binnendijk [1]; P and P′ are parallactic factors; Q and Q′ are members dependent on the galactic rotation.

Type
Part 2: Pulkovo today
Information
Symposium - International Astronomical Union , Volume 141: Inertial Coordinate System on the Sky , 1990 , pp. 65 - 66
Copyright
Copyright © Kluwer 1990 

References

1. Binnendijk, L. (1943) “Mean parallaxes of faint stars, derived from a combination of the Pulkovo and Radcliffe Catalogue of proper motions”, Bull. of the Astr. Inst. of the Netherlands , 10, #362, 9–18.Google Scholar
2. Deits, A.N. (1947) “Secular parallaxes of faint stars as deduced from Pulkovo Catalogue data on proper motions in Kapteyn Areas”, Izv. GAO Pulkovo 17, #138, 2–59. (in Russian).Google Scholar
3. Klemola, A.R., Vasilevskis, S. (1971) “A study of solar motion and galactic rotation”, Publ. Lick Obs. 22, Part 3, 1–13.Google Scholar