MIPS SED Observations of Massive Quiescent Cores in Orion

Details MIPS SED Observations of Massive Quiescent Cores in Orion MIPS SED Observations of Massive Quiescent Cores in Orion

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sptz.prop30645l&link_type=abstract

Spitzer Proposal ID #30645

Computer Science

Scientific paper

We propose to obtain MIPS SED data for a sample of 39 massive quiescent cores in Orion. Orion is the closest known massive star forming region and an ideal place for studying massive prestellar and protostellar cores. We have compiled a sample of Orion cores based on surveys at 350 and 450 microns and 1.2 mm. We have excluded cores within 4 pc of OB association and/or with IRAS point sources to avoid the destruction of prestellar cores by massive young stars. We have also obtained molecular spectroscopy data toward half of the sources. Our preliminary analysis shows that our core sample consists of structures more massive(mean mass ~ 10 solar mass) and generally warmer (~ 20 K) than low mass cores in Taurus. The density and temperature structure of the gas and dust envelopes of these quiescent cores provides important constraints for distinguishing between star formation models and determining the initial conditions of star formation. The Wien (shorter wavelength) side of dust continuum SED is more sensitive to temperature. Our existing data, however, are all on the Rayleigh-Jeans (longer wavelength) side.MIPS SED, from 50 to 100 microns, would provide both the intensity and the slope of the dust emission on the Wien side. Such information is crucial for deriving an accurate thermal structure, especially if a warm dust layer exists, which is likely for the cores in Orion. We are developing a 3d modeling algorithm (COREFIT) for modeling multiple wavelength dust continuum data with different beam sizes and PSFs. The proposed MIPS SED observations will be combined with existing data and analyzed using the COREFIT program. MIPS observations will enable us to achieve a good understanding of the dense core structure in massive star forming regions and derive an accurate mass for these cores.

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