The Palomar/MSU Nearby Star Spectroscopic Survey. IV. The Luminosity Function in the Solar Neighborhood and M Dwarf Kinematics

Astronomy and Astrophysics – Astronomy

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Galaxy: Solar Neighborhood, Stars: Kinematics, Stars: Luminosity Function, Mass Function

Scientific paper

We have used new astrometric and spectroscopic observations to refine the volume-complete sample of M dwarfs defined in previous papers in this series. With the addition of Hipparcos astrometry, our revised VC2 sample includes 558 main-sequence stars in 448 systems. Analysis of that data set shows no evidence of any systematic kinematic bias. Combining those data with a Hipparcos-based sample of AFGK dwarfs within 25 pc of the Sun, we have derived the solar neighborhood luminosity function, Φ(MV), for stars with absolute magnitudes between -1 and +17. Using empirical and semiempirical mass-MV relations, we transform Φ(MV) to the present-day mass function, ψ(M) (=dN/dM). Depending on the mass-luminosity calibration adopted, ψ(M) can be represented by either a two-component or a three-component power law. In either case, the power-law index α has a value of ~1.3 at low masses (0.1 Msolar4) stars in the Hipparcos 25 pc sample are well represented by two-component Gaussian distributions, with ~10% of the stars in the higher velocity dispersion component. We suggest that the latter component is the thick disk, and we offer a possible explanation for the relatively low velocity dispersions shown by ultracool dwarfs.
Based partly on observations made at the 60 inch (1.5 m) telescope at Palomar Mountain, which is jointly owned by the California Institute of Technology and the Carnegie Institution of Washington.

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