The calibration problem. III - First-order solution for mean absolute magnitude and dispersion

Details The calibration problem. III - First-order solution for mean absolute magnitude and dispersion The calibration problem. III - First-order solution for mean absolute magnitude and dispersion

Jul 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...181..391s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 181, no. 2, July 1987, p. 391-393.

Mathematics

Probability

7

Astrometry, Calibrating, Stellar Magnitude, Distance, Parallax, Probability Theory, Stellar Luminosity

Scientific paper

Trigonometric parallaxes are presently used to derive an approximate first-order method capable of estimating the mean and intrinsic dispersion of absolute magnitudes for a homogeneous stellar group. Attention is given to this method's relation to the probabilistic constraints considered by Eichhorn (1978). The method is approximate, being based on the expansion of an exponential to first order.

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