On the use of trigonometric parallaxes for the calibration of luminosity systems. II

Details On the use of trigonometric parallaxes for the calibration of luminosity systems. II On the use of trigonometric parallaxes for the calibration of luminosity systems. II

Oct 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979mnras.189..273l&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 189, Oct. 1979, p. 273-278.

Astronomy and Astrophysics

Astronomy

19

Calibrating, Parallax, Stellar Luminosity, Astronomical Models, Stellar Magnitude, Trigonometry

Scientific paper

The work of Lutz and Kelker (1973) is extended to the case where the sample of stars is limited by apparent magnitude. In order to compute average-absolute-magnitude-difference corrections for a magnitude-limited sample, it is necessary, in general, to adopt a luminosity function. It is shown, however, that for some samples of stars the average-absolute-magnitude-difference corrections of the previous paper apply, independent of the luminosity function. An example is given to show how to determine if this is the case.

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