Other
Scientific paper
Jan 2012
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21942303k&link_type=abstract
American Astronomical Society, AAS Meeting #219, #423.03
Other
Scientific paper
Massive stars play a major role in our and other Galaxies despite their low numbers, but it is not understood how they form. Intensive modeling has allowed us to better understand how massive stars can accrete despite their high luminosities, but the discussion is on-going on how the mass of the star-forming cloud is assembled onto the star.
Two protostars of intermediate mass have been identified in the star-forming region around IRAS 05345+3157. Observations with Spitzer and CARMA, combined with literature data, allowed us to construct the complete spectral energy distribution (SED) for two dense molecular cores in that region. We fit the SED with a radiative transfer (RT) model using the on-line model grid by Robitaille et al.(2007). The SED fit allows us determine the protostar's and its envelope's properties. A detailed analysis is performed to determine which parameters are well constrained by the SED which and which are not. Adding near infrared (NIR) and interferometric observations, a comprehensive picture of the star-forming region is created. The synthesis of the information on the region around IRAS 05345+3157 allows us understand the star formation history of the region and its current status.
This study serves as a pilot study to extend the SED fitting and parameter analysis to 168 candidates for massive embedded protostars selected from millimeter surveys of massive star-forming regions. These clumps are selected to be in a very early stage of their evolution. This will provide the theoretical underpinning to understand the SEDs and their evolution. The goal is to track observable and physical quantities using SEDs through the early stages of massive star formation to classify the stages and understand their evolution.
Henning Th
Klein Randolf
Lee Kyung-Il
Looney Leslie W.
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