On the use of trigonometric parallaxes for the calibration of luminosity systems - II.
Abstract
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.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- October 1979
- DOI:
- 10.1093/mnras/189.2.273
- Bibcode:
- 1979MNRAS.189..273L
- Keywords:
-
- Calibrating;
- Parallax;
- Stellar Luminosity;
- Astronomical Models;
- Stellar Magnitude;
- Trigonometry;
- Astronomy;
- Luminosities:Calibrations;
- Stars:Trigonometric Parallaxes