Other
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aj....109..280h&link_type=abstract
The Astronomical Journal (ISSN 0004-6256), vol. 109, no. 1669, p. 280-297
Other
55
A Stars, B Stars, Emission Spectra, Molecular Clouds, Pre-Main Sequence Stars, Star Formation, Early Stars, Infrared Photometry, Mass Distribution, Mass Spectra, Monte Carlo Method, Shock Wave Interaction, Visual Photometry
Scientific paper
We use optical and infrared photometry in combination with red optical spectra to study the star-forming region associated with the two Herbig Ae/Be stars BD + 40 deg 4124 and V1686 Cyg. We identify a partially embedded, dense, isolated cluster of pre-main sequence stars concentrated within 0.15 pc of the two young high-mass stars. The cluster is isolated in that it is separated by approximately 0.7 pc from a surrounding H alpha-bright rim and lies at the center of a molecular core with peak column density corresponding to 45 mag of visual extinction. The fraction of the stellar population with evidence for circumsteller activity is 100% amongst the optically visible cluster members and at least 50% amongst the embedded sources. This small region is characterized by an apparent age spread of approximately 3 Myr with evidence for both high-and low-mass stars forming relatively simultaneously (within several hundred thousand years). Comparison of the derived stellar mass distribution to that expected from Monte-Carlo sampling of the solar neighborhood mass spectrum reveals that this region is producing an unusually large number of intermediate-and high-mass stars. Our result suggests that not all star formation sites yield identical mass spectra, and that universal mass functions may be produced only when integrating over large spatial areas and/or over many star formation epochs. Futhermore, our data appear to exclude for the BD +40 deg 4124 region, the popular senario that low-mass star formation proceeds quietly and stochastically for several to ten Myr until the birth of an early type star, and its subsequent dynamical interaction with the cloud, ends all starformation processes in the core. Instead, we consider the hypothesis that star formation was induced in this region by the propagation of an external shock wave into the cloud core. This picture is similar to that invoked for other star-forming sites displaying a bright-rim morphology on optical images and cometary molecular structure, as we see in the vicinity of BD +40 deg 4124.
Hillenbrand Lynne A.
Meyer Michael R.
Skrutskie Michael F.
Strom Stephen E.
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