Clusters of Low-Mass Pre-Main Sequence Stars, Mass Functions, and Candidate Brown Dwarfs in Orion's Belt

Details Clusters of Low-Mass Pre-Main Sequence Stars, Mass Functions, and Candidate Brown Dwarfs in Orion's Belt Clusters of Low-Mass Pre-Main Sequence Stars, Mass Functions, and Candidate Brown Dwarfs in Orion's Belt

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...197.1003s&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #10.03; Bulletin of the American Astronomical Society, Vol. 32, p.1412

Astronomy and Astrophysics

Astronomy

Scientific paper

At least 3 of the 4 O stars of the Orion OB1b sub-association, ζ , δ , and σ Orionis, are associated with clusters of low-mass PMS stars. These clusters appear similar to the Orion nebular cluster (ONC); each consists of several hundred to a few thousand low-mass PMS stars centered on an O star system. These clusters are roughly 4 pc in radius. These PMS clusters in seem to be evolved analogs of the ONC. Like the ONC they should be excellent places to search for very low-mass stars and brown dwarfs because such low mass objects are at their brightest when they are very young. Recent observational work has shown that the σ Orionis cluster is a rich hunting ground for young brown dwarfs. We have used our moderately deep VRI photomery combined with 2MASS JHK photometry to derive mass functions for the ζ and δ Orionis clusters and for PMS stars around ɛ Orionis by fitting our data to the tracks of Baraffe et al. (1998). Our mass function reaches the base of the main sequence where we find several candidate brown dwarf in the δ Orionis and ζ Orionis clusters, and around ɛ Orionis. We expect that these regions, like the σ Orionis cluster, will also be fertile hunting grounds for very-low mass stars and brown dwarfs.

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