A survey of trigonometric parallaxes and proper motions with the UK Schmidt telescope. I - Methods and first results, for stars brighter than B = 14 in a field near the South Galactic Pole

Details A survey of trigonometric parallaxes and proper motions with the UK Schmidt telescope. I - Methods and first results, for stars brighter than B = 14 in a field near the South Galactic Pole A survey of trigonometric parallaxes and proper motions with the UK Schmidt telescope. I - Methods and first results, for stars brighter than B = 14 in a field near the South Galactic Pole

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979mnras.187..723m&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 187, June 1979, p. 723-751.

Computer Science

Numerical Analysis

22

Parallax, Schmidt Telescopes, Star Distribution, Statistical Analysis, Stellar Motions, Accuracy, Astronomical Catalogs, Astronomical Photometry, Atmospheric Refraction, Brightness, Numerical Analysis, Photographic Plates, Random Errors, Stellar Luminosity, Trigonometry

Scientific paper

In an attempt to investigate the statistics of stars in the solar neighbourhood, independent of the bias toward high-velocity stars introduced by selection of stars with large proper motion, a major astrometric investigation is being carried out at the RGO using UK Schmidt plates measured on the GALAXY machine.
So far more than 15 000 objects brighter than B = 18 in a field near the South Galactic Pole have been measured on more than 50 plates taken between 1974 and 1977.
This paper describes the methods of analysis and the results of a pilot investigation on nearly 900 stars with B < 14. The measurements show a very high degree of internal consistency, demonstrating the astrometric excellence of the UK Schmidt telescope and the GALAXY machine; random errors of measurement are found to be about ± 0.075 arcsec (= 1.1 μm) per coordinate over the whole area (4½° × 4½°) measured, using a simple linear plate constant model for all plates. The external error of a single component of proper motion is estimated to be ± 0.013 arcsec which is exactly consistent with the internal measurement error. The external error of a parallax in the present data is about ± 0.018 arcsec whereas that predicted from the errors of measurement, and the self-consistency of two subsets of the data, is ± 0.013 arcsec; it is shown that the discrepancy can be largely accounted for by the random errors (±O.11 mag) in the B-V colours used in computing the effect of atmospheric dispersion, and should be reduced when better photometry becomes available.
A correlation between parallax and large proper motion is found, as expected for stars with B-V ≥ 0.7, but is not evident for bluer stars. Significant parallaxes have been detected for the only two stars in the field which had been measured previously. Our parallax data for 33 stars with large proper motion are reasonably consistent with photometric parallaxes determined by Eggen.

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