The Mass Loss Return from Evolved Stars to the Large Magellanic Cloud: Oxygen-Rich Asymptotic Giant Branch Stars

Details The Mass Loss Return from Evolved Stars to the Large Magellanic Cloud: Oxygen-Rich Asymptotic Giant Branch Stars The Mass Loss Return from Evolved Stars to the Large Magellanic Cloud: Oxygen-Rich Asymptotic Giant Branch Stars

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21545906s&link_type=abstract

American Astronomical Society, AAS Meeting #215, #459.06; Bulletin of the American Astronomical Society, Vol. 42, p.486

Astronomy and Astrophysics

Astronomy

Scientific paper

The Spitzer Space Telescope Legacy program Surveying the Agents of a Galaxy's Evolution (SAGE; PI: M. Meixner) has observed over 6 million stars in the Large Magellanic Cloud with both the Infrared Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS) instruments to explore the life-cycle of matter in a galaxy. Over 17000 of these stars were found to be candidate Oxygen-rich Asymptotic Giant Branch (O-rich AGB) stars. We combine photometry from Spitzer and elsewhere in constructing Spectral Energy Distributions (SEDs) for the SAGE candidate O-rich AGB stars. These SEDs are then modeled using the radiative transfer program 2Dust, with the goal of determining the O-rich AGB star candidates' mass-loss rates. Spitzer Infrared Spectrograph (IRS) spectra are available as part of the Spitzer Legacy program SAGE-Spectroscopy (PI: F. Kemper) for a number of SAGE O-rich AGB star candidates; for two of these, IRS spectra in addition to the photometry are modeled with 2Dust to determine reasonable dust grain parameters to use for the candidate O-rich AGB stars in the rest of the SAGE sample. Using these dust grain properties, a grid of radiative transfer models was computed using 2Dust, varying stellar effective temperature and luminosity, dust shell inner radius, and dust shell optical depth at 10 microns wavelength. Synthetic photometry from models and observed photometry are plotted on color-color and color-magnitude diagrams, and model SEDs are directly compared to observed SEDs. The mass-loss rates from all O-rich AGB stars, especially those with the highest mass-loss rates, in the LMC are estimated and compared to its mass budget. Dust composition is also discussed in light of the results of the model grids.

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