Distributed vs. Clustered Star Formation in Cam OB-1

Details Distributed vs. Clustered Star Formation in Cam OB-1 Distributed vs. Clustered Star Formation in Cam OB-1

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop50533f&link_type=abstract

Spitzer Proposal ID #50533

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Scientific paper

The accepted paradigm in OB associations is that both high and low mass stars form predominantly in clusters containing 100s to 1000s of members. We have been re-examining that paradigm by identifying forming stars (protostars and stars with circumstellar disks) in GMCs via their infrared excesses at mid-IR and near-IR wavelengths, and studying the projected spatial distribution of those stars and their relative frequency as a function of physical parameters of the cloud such as luminosity, local gas and dust density, age, dynamical effects, among others. We are also comparing star formation in GMCs preferentially harboring low mass stars with these higher mass analogues, in order to identify differing evolutionary behaviors. The question of whether the distributed stellar population formed in situ, or was expelled from clusters, is the main driver for this proposal. Cam OB-1 is a lower luminosity (by factors of 10 or greater) example than most other associations in GMCs studied by us to date, including NGC 2264, Cep OB3, Mon R2, and Orion. A sufficiently large sample of high mass star forming GMCs is necessary to disentangle influence of various effects. Here we request MIPS observations to study the protostellar population in Cam OB1. Near IR Ks-band excess objects (mainly stars with disks) are more uniformly distributed in Cam OB1 than in other clouds in our sample. We are interested here to assess whether the protostars are also a larger percentage of the distributed population. We will propose to obtain 3.6 and 4.5 micron maps of Cam OB1 in a post-cryo mission, thus completing a sensitive, Spitzer enabled analysis of the YSO spatial distribution as an input to answering the driving question mentioned above.

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