Confidence intervals for the Lutz-Kelker correction

Details Confidence intervals for the Lutz-Kelker correction Confidence intervals for the Lutz-Kelker correction

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.256...65k&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 256, no. 1, May 1, 1992, p. 65-68.

Statistics

Computation

39

Computational Astrophysics, Correction, Stellar Magnitude, Stellar Parallax, Confidence Limits, Distribution Functions, Spatial Distribution

Scientific paper

The distribution function of the bias in the absolute magnitude of a star, as determined from its trigonometric parallax, is calculated for the case where the error dispersion is imperfectly known. A general power law is assumed for the spatial distribution of stars. The distribution function is used to calculate most probable and mean bias corrections as well as confidence intervals for the correction, the latter providing an indication of the intrinsic accuracy of the Lutz-Kelker correction. The basic method may be used for bias correction in other situations also.

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