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N.R. Adams, S.J. Wolk (CfA), F.M. Walter, W.H. Sherry (SUNY Stony Brook)
On 2002 November 21-22, the Chandra X-ray Observatory observed the young star forming region around Sigma Orionis with the goal of studying the X-ray luminosity of a well understood sample of pre-main sequence stars and detecting X-ray emission from known young brown dwarfs(BDs). The Sigma Ori cluster is uniquely suited to this study; it spans different stellar interior conditions, almost 3 orders of magnitude in mass, it is relatively close, almost dust free (5 of stars with and without disks and we have measured its mass function well below the DB limit. We present X-ray characteristics of the Sigma Orionis region, the comparisions with the optical and IR data in this region and discuss the possibility of this being a star formation cluster.
This research is supported by NASA and the CXC through grant #GO2-3019A.
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Bulletin of the American Astronomical Society, 36 5
© 2004. The American Astronomical Society.