The Substellar Population in σ Orionis

Details The Substellar Population in σ Orionis The Substellar Population in σ Orionis

Jun 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003iaus..211..111z&link_type=abstract

Brown Dwarfs, Proceedings of IAU Symposium #211, held 20-24 May 2002 at University of Hawaii, Honolulu, Hawaii. Edited by Eduard

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The σ Orionis cluster (˜3 Myr, 350 pc) is an ideal site to investigate the early evolution of substellar (brown dwarf and planetary mass) objects. To date, the cluster photometric and spectroscopic sequence of free-floaters is known for a wide mass range from 1M&sun; down to roughly 3MJup. The substellar domain covers spectral types that go from mid-M classes to the recently defined ``methane'' T-types, i.e., surface temperatures between ˜3000 K and 800 K. We derive a rising initial substellar mass function in the mass interval of 150--5MJup (dN/dM ˜ M-α, with α = 0.9 ± 0.4). We also find evidence for a extension of this mass function toward lower masses down to 2--3MJup. This indicates that the population of isolated planetary mass objects with masses below the deuterium burning threshold is rather abundant in the cluster.

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