The calibration problem. I - Estimation of mean absolute magnitude using trigonometric parallaxes. II - Trigonometric parallaxes selected according to proper motion and the problem of statistical parallaxes

Details The calibration problem. I - Estimation of mean absolute magnitude using trigonometric parallaxes. II - Trigonometric parallaxes selected according to proper motion and the problem of statistical parallaxes The calibration problem. I - Estimation of mean absolute magnitude using trigonometric parallaxes. II - Trigonometric parallaxes selected according to proper motion and the problem of statistical parallaxes

Jan 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...171..336s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 171, no. 1-2, Jan. 1987, p. 336-347.

Astronomy and Astrophysics

Astrophysics

23

Astrometry, Calibrating, Stellar Luminosity, Stellar Magnitude, Stellar Parallax, Bayes Theorem, Bias, Trigonometry

Scientific paper

This paper is the first in a projected series considering various aspects of the problem of calibrating distance determination methods. In it we consider the application of Bayes estimation to determining the most probable true parallax of an individual star, both with and without the information provided by the star's apparent magnitude and the luminosity function. We then extend these results to the estimation of the mean absolute magnitude M0 and dispersion σM for a homogeneous stellar group. The well-known Lutz-Kelker correction is shown to be inappropriate for this problem when the apparent magnitude is specified. Selection effects other than that according to apparent magnitude are not considered here.

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