Short-interval estimations of trigonometric parallaxes

Details Short-interval estimations of trigonometric parallaxes Short-interval estimations of trigonometric parallaxes

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985pasp...97..345g&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 97, April 1985, p. 345-347. Research supported by the A

Astronomy and Astrophysics

Astronomy

3

Astrometry, Stellar Luminosity, Stellar Motions, Stellar Parallax, Astronomical Coordinates, Dwarf Stars

Scientific paper

A technique for estimating trigonometric parallaxes in a matter of days or weeks is presented. The technique relies on the discrepancy between the instantaneous proper motion and the proper motion of a star. The main sources of error in the method are the standard error of the individual observations (0.004 arcsec) and the arbitrary limit placed on the observation interval. The parallactic motion of an MO dwarf of known parallax and a blue magnitude of 11.2 is determined. The slope inferred is within 10 percent of the value (0.555 arcsec) derived from a 1.5-year study of Barnard's star. It is concluded that the technique, if used on the same time scale as conventional techniques, would yield results of much higher accuracy.

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