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Star Counts

Published online by Cambridge University Press:  12 April 2016

Richard G. Kron
Richard G. Kron*
Affiliation:
Yerkes Observatory, The University of Chicago, Williams Bay, Wisconsin 53191 USA

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The number of stars counted along a particular line of sight depends on the spatial distribution of stars, the luminosity function, and the absorption. Thus star count programs are designed to constrain or determine one or more of these functions. Early efforts to understand the structure of our Galaxy, including the fundamentals of stellar statistics, were largely based on work that involved star counts. Since then a growing appreciation has developed for the variety of forms the density function D(r) and the luminosity function Φ(M) can take, especially the recognition of different stellar populations, each with different density and luminosity functions. In the simplest formulation two distinct populations are considered: disk and halo. This suggests two distinct formation histories, but uncertainty in the picture remains (Eggen, Lynden-Bell and Sandage 1962; Ostriker and Thuan 1975; Saio and Yoshii 1979; Jones and Wyse 1983).

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 78: Astronomy with Schmidt-type telescopes , 1984 , pp. 315 - 324
Copyright
Copyright © Reidel 1984

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