The Faint End of the Disk Luminosity Function

Details The Faint End of the Disk Luminosity Function The Faint End of the Disk Luminosity Function

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989jkas...22..101l&link_type=abstract

Journal of the Korean Astronomical Society, vol. 22, no. 2, p. 101-111

Astronomy and Astrophysics

Astronomy

2

Scientific paper

We have analysed the proper motion data of LHS catalog, to derive the faind end of the luminosity function more precise than ever before, by mean absolute method, and by making use of the reduced proper motion diagram. It is found that the relations between the mean absolute magnitude and the reduced proper motion for main sequence stars, subdwarfs, and the white dwarfs are so different that the proper application of an appropriate relation to each group is much more important. The derived luminosity function shows the broad maximum peak from M_B ~ 14 to M_B ~ 17 and declines after M_B ~ 17 up to M_B ~ 22.

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