Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21725828c&link_type=abstract
American Astronomical Society, AAS Meeting #217, #258.28; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
Recent Spitzer mid-IR observations have revealed a large number of individually resolved massive young stellar objects (YSOs) in the Magellanic clouds, providing an excellent opportunity to study massive star formation with metallicity and galactic environment different from the Milky Way. Using Spitzer IRAC/MIPS data from SAGE survey and complementary high-resolution ground-based optical/near-IR data, we have identified YSOs in HII complexes in the Large and Small Magellanic Cloud (LMC and SMC) and a large area in the Magellanic Bridge. These systems span a metallicity range of 1/3-1/8 Zo, and different galactic environments with star formation modes from mainly self-propagating in the LMC to tidally disrupted in the Bridge. We have modeled spectral energy distributions of the YSOs and found that they have masses ranging from 4 to 45 Mo in the LMC and SMC, while the most massive ones in the Bridge are < 10 Mo. YSOs in these three systems are found to span a wide range of evolutionary stages from highly embedded to surrounded by remnant material, though for the same mass range YSOs in the Bridge appear less embedded as almost all of them are visible at optical, opposed to only a small fraction in the LMC. The smaller extinction may be due to Bridge's lower dust content in either the CO clouds or circumstellar envelopes, or both. Using surveys in Hα, CO, and HI of these three systems, we further investigate the causal relationship between gas and stars. Examination of individual regions shows that massive YSOs tend to be found near ionized gas, i.e., where massive stars formed a few Myr ago, and the correlation is strongest for O-type YSOs. It appears that energy feedback plays a significant role in massive star formation. Star formation efficiencies in regions in these three systems are comparable, < 1/100-1/1000.
Chen Rosie Chang-Hui
Chu Yan-Yi
Fukui Yasuo
Gordon Karl
Gruendl Robert
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