Regions of Low Mass Star Formation in the LYNDS 1641 Giant Molecular Cloud

Details Regions of Low Mass Star Formation in the LYNDS 1641 Giant Molecular Cloud Regions of Low Mass Star Formation in the LYNDS 1641 Giant Molecular Cloud

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.9605a&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #96.05; Bulletin of the American Astronomical Society, Vol. 26, p.1477

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The nearest giant molecular cloud (d ~ 480 pc), Lynds 1641, contains several regions of low mass star formation, in addition to the rich Trapezium cluster. These young stars are grouped into loose aggregates of enhanced stellar surface density (>3sigma above the background) near regions of high molecular gas opacity, molecular outflows, embedded infrared sources, and HH objects. We present results of a multi-wavelength study of such regions, covering approximately 0.7 deg(2) of the cloud, and including the aggregate located near the L1641 North molecular outflow, the Cohen-Kuhi group, and the L1641 South cluster. Classification spectra in the in the lambda lambda 5500-9000{ Angstroms} range were obtained for ~ 400 stars, and are combined with photometry from infrared (J,H,K) and optical (R,I) images to place the stars in the HR diagram. Mass and age estimates follow from interpolation of theoretical pre-main sequence evolutionary tracks. We find that low and intermediate mass star formation (3.0Msun 50 %) of stars in the aggregates appear to have disks or envelopes. Finally, we investigate the spatial distributions of the young stars in relation to the morphology of the surrounding molecular gas. The local environments of young stars are found to vary, ranging from regions of high extinction (A_v > 20), to areas of low gas column density.

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