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1993•Journal of The Korean Astronomical SocietyRequires access

A STUDY ON THE INITIAL MASS FUNCTION OF HALO STARS

Lee, Sang-Gak

Open publisher page 4 citations

Abstract

The sample of sub dwarfs are selected from LHS catalogue on the bases of the reduced proper motion diagram utilizing Chui criteria, and confirmed with the available photometric and/or kinematic data. Among them, 20 sub dwarfs have trigonometric parallaxes with accuracy better than . The color­absolute magnitude relation is derived with them. By adopting this color-magnitude relation and method, we have derived the sub dwarf luminosity function over the absolute magnitude range of = 4.5 and 9.5. This halo luminosity function is consistent with that of Eggen(1987). By adopting the available mass-luminosity relations for halo stars, we have found that the halo IMF is steeper than disk IMFs of Scalo(1986) and Salpter(1955) in this small mass region.

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What this paper is about

The sample of sub dwarfs are selected from LHS catalogue on the bases of the reduced proper motion diagram utilizing Chui criteria, and confirmed with the available photometric and/or kinematic data. Among them, 20 sub dwarfs have trigonometric parallaxes with accuracy better than . The color­absolute magnitude relation is derived with them. By adopting this color-magnitude relation and method, we have derived the sub dwarf luminosity function over the absolute magnitude range of = 4.5 and 9.5. This halo luminosity function is consistent with that of Eggen(1987). By adopting the available mass-luminosity relations for halo stars, we have found that the halo IMF is steeper than disk IMFs of Scalo(1986) and Salpter(1955) in this small mass region.

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Available abstract

The sample of sub dwarfs are selected from LHS catalogue on the bases of the reduced proper motion diagram utilizing Chui criteria, and confirmed with the available photometric and/or kinematic data. Among them, 20 sub dwarfs have trigonometric parallaxes with accuracy better than . The color­absolute magnitude relation is derived with them. By adopting this color-magnitude relation and method, we have derived the sub dwarf luminosity function over the absolute magnitude range of = 4.5 and 9.5. This halo luminosity function is consistent with that of Eggen(1987). By adopting the available mass-luminosity relations for halo stars, we have found that the halo IMF is steeper than disk IMFs of Scalo(1986) and Salpter(1955) in this small mass region.

Key concepts: Physics, Halo, Astrophysics, Absolute magnitude, Stars, Magnitude (astronomy), Luminosity function, Luminosity

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