Spitzer Observations of High-Mass Quiescent Cores in Orion

Details Spitzer Observations of High-Mass Quiescent Cores in Orion Spitzer Observations of High-Mass Quiescent Cores in Orion

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21332704c&link_type=abstract

American Astronomical Society, AAS Meeting #213, #327.04; Bulletin of the American Astronomical Society, Vol. 41, p.383

Astronomy and Astrophysics

Astronomy

Scientific paper

The mechanisms for high-mass star formation are believed to be different from those for low-mass stars. By studying the density and temperature structure of quiescent cores, we can place constraints on these processes. Therefore, we have an ongoing program to study massive quiescent cores in Orion (Li et al. 2003; Li et al. 2007; Velusamy et al. 2008). Here we present Spitzer MIPS SED observations of seven of these cores. The long slit of the MIPS SED, where most of the pixels are not on the core, has allowed us to separate the emission from the diffuse warm interstellar dust from the colder dust of the core. We used a modeling program, COREFIT, to combine our spectra with existing infrared, sub-millimeter, and millimeter data to derive better constraints on the temperature and density model for each core. The 50-100 micron MIPS SED band is particularly sensitive to changes in
temperature, making these data important for accurate modeling. With better mass estimates for all the cores, we can examine whether these cores are gravitationally unstable (supercritical). This research was supported by the Jet Propulsion Laboratory, California Institute of Technology.

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