arXiv 1107.43132011-07-21astro-ph.CO

在潮汐剥离的低金属量小麦哲伦云（SAGE-SMC）中调查星系演化的因素。I.概述

Surveying the Agents of Galaxy Evolution in the Tidally-Stripped, Low Metallicity Small Magellanic Cloud (SAGE-SMC). I. Overview

Karl D. Gordon, Margaret Meixner, Marilyn Meade, Barbara A. Whitney, Charles W. Engelbracht, Caroline Bot, Martha L Boyer, Brandon Lawton, Marta Sewilo, Mr. Bri… 展开作者

Karl D. Gordon, Margaret Meixner, Marilyn Meade, Barbara A. Whitney, Charles W. Engelbracht, Caroline Bot, Martha L Boyer, Brandon Lawton, Marta Sewilo, Mr. Brian L. Babler, Jean-Philippe Bernard, Steve Bracker, Miwa Block, Robert D. Blum, Alberto D. Bolatto, Alceste Zoe Bonanos, Jason Harris, Joseph L. Hora, Remy Indebetouw, Karl A. Misselt, William T. Reach, B. Shiao, Alexander Tielens, Lynn Redding Carlson, Edward B. Churchwell, Geoff C. Clayton, C-H Rosie Chen, Martin Cohen, J. Lewis Fukui, Varoujan Gorjian, Sacha Hony, Frank Israel, Akiko Kawamura, F. Kemper, Adam K. Leroy, Aigen Li, Suzanne C. Madden, Andrew R. Marble, Iain McDonald, Akira Mizuno, Norikazu Mizuno, EriK Muller, Joana M. Oliveira, Knut A. G. Olsen, T. Onishi, Roberta Paladini, Deborah Paradis, Sean Points, Thomas Robitaille, Douglas Rubin, Karin Sandstrom, S Sato, Hiroshi Shibai, Joshua D. Simon, Linda J Smith, Sundar Srinivasan, Uma P. Vijh, Schuyler D. Van Dyk, Jacobus Theodorus van Loon, Dennis F. Zaritsky

备注：: 16 pages, 11 figures, AJ, in press
DOI：: 10.1088/0004-6256/142/4/102

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摘要：

小麦哲伦云（SMC）提供了一个独特的实验室，研究尘埃的生命周期，因为它的金属含量低（~1/5太阳）和相对接近（~60千秒差距）。这激发了SAGE-SMC（在潮汐剥离的低金属量小麦哲伦云中调查星系演化的因素）斯皮策遗产计划，其具体目标是研究当前星际介质中的尘埃数量和类型，演化恒星风中的尘埃来源，以及恒星形成过程中消耗了多少尘埃。该程序映射了整个SMC（30 sq.（摄氏度）包括身体，翅膀和尾巴在7个波段从3.6到160微米使用IRAC和MIPS仪器斯皮策太空望远镜。数据被简化，镶嵌，点源测量使用定制的例程特定的大型调查。我们已经向社区提供了由此产生的马赛克和点源目录。SMC的红外颜色与其他邻近星系的红外颜色相比，8微米/24微米的比例略低，70微米/160微米的比例略高于平均值。全球红外光谱能量分布显示，SMC的芳烃发射/PAH（多环芳烃）丰度比大多数邻近星系低3倍。给出了不同渐近巨星分支星的红外色星等分布图和年轻恒星的位置。最后，HII/恒星形成区的平均光谱能量分布（SED）进行了比较，相当于大麦云平均HII/恒星形成区SED。这些初步结果在配套文件中详细扩展。

英文摘要：

The Small Magellanic Cloud (SMC) provides a unique laboratory for the study of the lifecycle of dust given its low metallicity (~1/5 solar) and relative proximity (~60 kpc). This motivated the SAGE-SMC (Surveying the Agents of Galaxy Evolution in the Tidally-Stripped, Low Metallicity Small Magellanic Cloud) Spitzer Legacy program with the specific goals of studying the amount and type of dust in the present interstellar medium, the sources of dust in the winds of evolved stars, and how much dust is consumed in star formation. This program mapped the full SMC (30 sq. deg.) including the Body, Wing, and Tail in 7 bands from 3.6 to 160 micron using the IRAC and MIPS instruments on the Spitzer Space Telescope. The data were reduced, mosaicked, and the point sources measured using customized routines specific for large surveys. We have made the resulting mosaics and point source catalogs available to the community. The infrared colors of the SMC are compared to those of other nearby galaxies and the 8 micron/24 micron ratio is somewhat lower and the 70 micron/160 micron ratio is somewhat higher than the average. The global infrared spectral energy distribution shows that the SMC has ~3X lower aromatic emission/PAH (polycyclic aromatic hydrocarbon) abundances compared to most nearby galaxies. Infrared color-magnitude diagrams are given illustrating the distribution of different asymptotic giant branch stars and the locations of young stellar objects. Finally, the average spectral energy distribution (SED) of HII/star formation regions is compared to the equivalent Large Magellanic Cloud average HII/star formation region SED. These preliminary results are expanded in detail in companion papers.

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