Probing Star and Planet Formation in a Young OB Assocation: Warm Mission Mapping of the Orion OB1 Association

Details Probing Star and Planet Formation in a Young OB Assocation: Warm Mission Mapping of the Orion OB1 Association Probing Star and Planet Formation in a Young OB Assocation: Warm Mission Mapping of the Orion OB1 Association

Jun 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010sptz.prop70044m&link_type=abstract

Spitzer Proposal ID #70044

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Scientific paper

We propose to extend the Spitzer Survey of Orion from the molecular clouds into the neighboring OB association. Together the clouds and association comprise a 75 pc diameter star forming complex where star formation has been sustained for 10 million years. To date, Spitzer surveys of Orion have concentrated on the molecular cloud to probe ongoing star formation. However, the clouds contain only a fraction of the total population of young stars in the complex. A growing number of observations show that the Orion OB1 association, which neighbors the molecular cloud, contains a large a population of young (2-10 Myr) pre-main sequence stars and sub-stellar objects, many of which still retain their dusty disks. Using Spitzer's unique capability to survey wide fields and detect mid-IR emision from dusty disks, we will map the distribution of young stars in two of the youngest sub-groups of the association, the OB1b and c subgroups with ages of 2-5 Myr. The association is likely to contain a few thousand stars, many hundreds of which will exhibit IR-excesses from disk. Based on small, existing fields within the OB1b association, and from examples in other regions such as W5, we expect to see fossil structures in the spatial distribution of young stars which trace the distribution of star formation sites. The distribution of stars both inside and outside the clouds is thus a powerful probe of the star forming history of the Orion complex, and when combined with ground based spectroscopy, can be used to study how star formation is initiated, regulated and terminated in massive complexes like Orion (where most stars of all masses are formed!). In addition, the data will be used to study disk evolution in one of the richest collections of 1-5 Myr old intermediate to solar mass stars and sub-stellar objects within 500 pc of the Sun.

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