An Improved Grid of YSO Radiative Transfer Models, and Further Analysis of SEDs and Images from Spitzer

Details An Improved Grid of YSO Radiative Transfer Models, and Further Analysis of SEDs and Images from Spitzer An Improved Grid of YSO Radiative Transfer Models, and Further Analysis of SEDs and Images from Spitzer

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007sptz.prop40794w&link_type=abstract

Spitzer Proposal ID #40794

Computer Science

Scientific paper

Thanks to support from a previously funded Spitzer Theory proposal, we have made our grid of 200,000 Young Stellar Object Spectral Energy Distributions (YSO SEDs) and its companion data fitter publicly available. As part of that proposal, we promised to run a second generation grid of models that will be completed by Fall 2007. We have since identified additional models to run, as well as additional code development that will produce a significant advance over what was originally planned. In particular, the new radiation transfer code modifications will allow us to produce high signal-to-noise (S/N) images in addition to the SEDs at each of ten viewing angles in the 2-D models (and 200 in the 3-D models), as well as polarization maps and spectra. The SEDs will have much higher S/N, important for modeling IRS spectra, very embedded sources at IRAC wavelengths, and all sources at long wavelengths. The SEDs will be more accurate for edge-on disks, since they will not be averaged over a range of angles. As new models are computed, they will replace the ones in the 2007 grid, and the new grid will be designed to support expansion beyond the 2007 grid. The models run with the new code will take ~8 times longer. In addition, we plan to expand the number of models in the grid by at least a factor of two, based on requests from the community and our own work. We therefore request funds for a small but dedicated computer cluster to run models continuously over a period of a few years. We will use these tools to analyze star formation regions in the Galaxy and the LMC. We will also investigate the effects of source confusion on properties derived from the SED fitter.

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