A New Method for Determining the Shape of the Faint End of the Luminosity Function

Details A New Method for Determining the Shape of the Faint End of the Luminosity Function A New Method for Determining the Shape of the Faint End of the Luminosity Function

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983nssl.conf..187h&link_type=abstract

The Nearby Stars and the Stellar Luminosity Function, Proceedings of IAU Colloquium No. 76 held 13-16 June 1983 at Wesleyan Univ

Physics

2

Scientific paper

A new observational method for determining the space density of very low luminosity stars is outlined. The essence of the method is to use a dark cloud of known distance to cut off the light of stars beyond that distance, providing a well defined volume of space in which all stars with MB ≤ Bl - DM will be detected. Bl is the limiting magnitude of the plate and DM is the distance modulus of the cloud.

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