The Substellar Domain in the ɛ Orionis Cluster

Details The Substellar Domain in the ɛ Orionis Cluster The Substellar Domain in the ɛ Orionis Cluster

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003csss...12..651b&link_type=abstract

The Future of Cool-Star Astrophysics: 12th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (2001 July 30 - August

Astronomy and Astrophysics

Astrophysics

1

Ɛ Ori, Brown Dwarfs & Extrasolar Planets, Very Low Mass Stars

Scientific paper

We present an IZ photometric survey covering a total area of about 1000 arcmin2 around the ɛ Orionis young massive star (˜10 Myr, d=412 pc) and reaching a limiting magnitude I=22. From the resulting I, I-Z color-magnitude diagram we have selected 123 red candidates in the interval I=15--22 mag, which according to evolutionary models corresponds to masses between 0.40 and 0.020 M&odot, i.e, approaching the deuterium burning mass limit. We have obtained follow-up J-band photometry for half of our photometric candidates. The I, I-J color-magnitude diagram and low-resolution optical spectroscopy of four of them suggest that we have identified a rather abundant population of young low-mass stars and brown dwarfs. We compare our findings with previous works in other young clusters.

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