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17 April 2024

» arxiv » astro-ph/0608189

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Spitzer SAGE survey of the Large Magellanic Cloud II: Evolved Stars and Infrared Color Magnitude Diagrams
R. D. Blum ; J. R. Mould ; K. A. Olsen ; J. A. Frogel ; M. Werner ; M. Meixner ; F. Markwick-Kemper ; R. Indebetouw ; B. Whitney ; M. Meade ; B. Babler ; E. B. Churchwell ; K. Gordon ; C. Engelbracht ; B. -Q. For ; K. Misselt ; U. Vijh ; C. Leitherer ; K. Volk ; S. Points ; W. Reach ; J. L. Hora ; J. -P. Bernard ; F. Boulanger ; S. Bracker ; M. Cohen ; Y. Fukui ; J. Gallagher ; V. Gorjian ; J. Harris ; D. Kelly ; A. Kawamura ; W. B. Latter ; S. Madden ; A. Mizuno ; N. Mizuno ; A. Nota ; M. S. Oey ; T. Onishi ; R. Paladini ; N. Panagia ; P. Perez-Gonzalez ; H. Shibai ; S. Sato ; L. Smith ; L. Staveley-Smith ; A. G. G. M. Tielens ; T. Ueta ; S. Van Dyk ; D. Zaritsky ;
Date:	9 Aug 2006
Abstract:	Color-magnitude diagrams (CMDs) are presented for the Spitzer SAGE (Surveying the Agents of a Galaxy’s Evolution) survey of the Large Magellanic Cloud (LMC). IRAC and MIPS 24 um epoch one data are presented. These data represent the deepest, widest mid-infrared CMDs of their kind ever produced in the LMC. Combined with the 2MASS survey, the diagrams are used to delineate the evolved stellar populations in the Large Magellanic Cloud as well as Galactic foreground and extragalactic background populations. Some 32000 evolved stars brighter than the tip of the red giant branch are identified. Of these, approximately 17500 are classified as oxygen-rich, 7000 carbon-rich, and another 1200 as ``extreme’’ asymptotic giant branch (AGB) stars. Brighter members of the latter group have been called ``obscured’’ AGB stars in the literature owing to their dusty circumstellar envelopes. A large number (1200) of luminous oxygen--rich AGB stars/M supergiants are also identified. Finally, there is strong evidence from the 24 um MIPS channel that previously unexplored, lower luminosity oxygen-rich AGB stars contribute significantly to the mass loss budget of the LMC (1200 such sources are identified).
Source:	arXiv, oai:arXiv.org:astro-ph/0608189
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