No CrossRef data available.
Article contents
On the Use of Statistical Parallaxes for the Proper Motion Reductions
Published online by Cambridge University Press: 19 July 2016
Extract
Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.
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
You have
Access