Computer Science
Scientific paper
Aug 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999noao.prop...36w&link_type=abstract
NOAO Proposal ID #1999B-0036
Computer Science
Scientific paper
The Orion OB1a and b associations are nearby fossil star formation regions. Fossil star formation regions have the optimum conditions for studying global aspects of the star formation process: the star formation is complete, the regions are unobscured, and the stars have not yet had time to disperse. Our UBVRI photometry of selected regions in the Orion OB1a and b associations shows that the association is full of young low mass stars, and suggests that these stars tend to cluster around the massive stars of the belt. The photometry shows a distinct pre-main sequence locus at an age comparable to that estimated for the OB stars, extending down into the brown dwarf regime. Low resolution spectra of the brighter stars near σ Ori, obtained with WIYN/HYDRA, confirm youth (from the Lithium line) and association with Orion's belt (from radial velocities). We have obtained and reduced CCD photometry of about 4 square degrees in the belt of Orion and within Ori OB1a. We propose follow-up spectroscopy on a sample of photometrically-identified PMS stars in these regions. Spectroscopy, combined with the photometry, will give the statistically complete stellar population of this association, and the initial mass function, down to substellar masses. In addition, high- dispersion spectra of the brighter stars will reveal the kinematics of the association, the binary frequency, and the stellar characteristics. Low dispersion spectra of the fainter stars will be used to study the very low mass stars and the brown dwarf population.
Sherry William
Walter Frederick M.
Wolk Scott
No associations
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