Is the Slope of the Hyades IMF Rising Below M ~ 0.1 M_&sun;?

Details Is the Slope of the Hyades IMF Rising Below M ~ 0.1 M_&sun;? Is the Slope of the Hyades IMF Rising Below M ~ 0.1 M_&sun;?

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...18510303b&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #103.03; Bulletin of the American Astronomical Society, Vol. 26, p.1486

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We have used the Minnesota Automated Plate Scanner to compare Palomar Schmidt plates of the Hyades region from three different epochs--- generating a list of candidate members of the Hyades cluster selected by color and proper motion which includes stars complete to more than a magnitude fainter than previous work. Adopting the most conservative possible value for the number of true Hyads found, and combining our results with the survey of Reid (1992, MNRAS, 257, 257), we derive the form of the cluster luminosity function (LF) down to luminosities corresponding to masses of M ~ 0.1 M_&sun;. We find that the LF matches best to a moderately increasing mass function with a power law index of alpha < 1.0 in the mass range 0.3 ~> M/Msun ~> 0.2 increasing to alpha ~ 1.5 below M ~ 0.2 Msun. Within the statistical uncertainties, this increase may be even more dramatic below M ~ 0.15 Msun. We note that if lower mass stars were preferentially evaporated from the cluster, our observed mass function would have a lesser slope than the original IMF. If alpha > 2 for the IMF below the hydrogen burning limit (M ~ 0.08 Msun), then brown dwarfs would have initially been (and may still be) a significant contributer to the Hyades' total mass.

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