SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). I. OVERVIEW

被引：192

作者：

Gordon, K. D. ^{[1
]}

Meixner, M. ^{[1
]}

Meade, M. R. ^{[2
]}

Whitney, B. ^{[2
,3
]}

Engelbracht, C. ^{[4
]}

Bot, C. ^{[5
]}

Boyer, M. L. ^{[1
]}

Lawton, B. ^{[1
]}

Sewilo, M. ^{[6
]}

Babler, B. ^{[2
]}

Bernard, J. -P. ^{[7
]}

Bracker, S. ^{[2
]}

Block, M. ^{[4
]}

Blum, R. ^{[8
]}

Bolatto, A. ^{[9
]}

Bonanos, A. ^{[10
]}

Harris, J. ^{[8
]}

Hora, J. L. ^{[11
]}

Indebetouw, R. ^{[12
,13
]}

Misselt, K. ^{[4
]}

Reach, W. ^{[12
]}

Shiao, B. ^{[1
]}

Tielens, X. ^{[14
]}

Carlson, L. ^{[6
]}

Churchwell, E. ^{[2
]}

Clayton, G. C. ^{[15
]}

Chen, C. -H. R. ^{[16
]}

Cohen, M. ^{[17
]}

Fukui, Y. ^{[18
]}

Gorjian, V. ^{[19
]}

Hony, S. ^{[20
]}

Israel, F. P. ^{[14
]}

Kawamura, A. ^{[18
,21
]}

Kemper, F. ^{[22
,23
]}

Leroy, A. ^{[13
]}

Li, A. ^{[24
]}

Madden, S. ^{[20
]}

Marble, A. R. ^{[4
,25
]}

McDonald, I. ^{[26
]}

Mizuno, A. ^{[18
]}

Mizuno, N. ^{[18
]}

Muller, E. ^{[18
,21
]}

Oliveira, J. M. ^{[26
]}

Olsen, K. ^{[8
]}

Onishi, T. ^{[18
]}

Paladini, R. ^{[12
]}

Paradis, D. ^{[12
]}

Points, S. ^{[27
]}

Robitaille, T. ^{[11
]}

Rubin, D. ^{[20
]}

机构：

[1] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[2] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA

[3] Space Sci Inst, Boulder, CO 80301 USA

[4] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA

[5] Univ Strasbourg, Ctr Donnees Astron Strasbourg CDS, UMR 7550, F-67000 Strasbourg, France

[6] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[7] Univ Toulouse, UPS, CESR, F-31028 Toulouse 4, France

[8] Natl Opt Astron Observ, Tucson, AZ 85719 USA

[9] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[10] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece

[11] Harvard Smithsonian, CfA, Cambridge, MA 02138 USA

[12] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA

[13] Natl Radio Astron Observ, Charlottesville, VA 22903 USA

[14] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands

[15] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA

[16] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA

[17] Monterey Inst Res Astron, Marina, CA 93933 USA

[18] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan

[19] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[20] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France

[21] Natl Astron Observ Japan, ALMA J Project Off, Tokyo 1818588, Japan

[22] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan

[23] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England

[24] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA

[25] Natl Solar Observ, Tucson, AZ 85719 USA

[26] Univ Keele, Astrophys Grp, Lennard Jones Labs, Keele ST5 5BG, Staffs, England

[27] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, La Serena, Chile

[28] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[29] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA

[30] European Space Agcy, Res & Sci Support Dept, Baltimore, MD 21218 USA

[31] Inst Astrophys, F-75014 Paris, France

[32] Univ Toledo, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA

来源：

ASTRONOMICAL JOURNAL | 2011年 / 142卷 / 04期

关键词：

galaxies:; individual; (SMC); SPITZER-SPACE-TELESCOPE; MULTIBAND IMAGING PHOTOMETER; INFRARED ARRAY CAMERA; MASS-LOSS RETURN; SPECTRAL IRRADIANCE CALIBRATION; YOUNG STELLAR OBJECTS; GIANT BRANCH STARS; 24; MU-M; ABSOLUTE CALIBRATION; EVOLVED STARS;

D O I：

10.1088/0004-6256/142/4/102

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Small Magellanic Cloud (SMC) provides a unique laboratory for the study of the lifecycle of dust given its low metallicity (similar to 1/5 solar) and relative proximity (similar to 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 deg(2)) including the body, wing, and tail in seven bands from 3.6 to 160 mu m using IRAC and MIPS on the Spitzer Space Telescope. The data were reduced and mosaicked, and the point sources were 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 mu m/24 mu m ratio is somewhat lower than the average and the 70 mu m/160 mu m ratio is somewhat higher than the average. The global infrared spectral energy distribution (SED) shows that the SMC has approximately 1/3 the aromatic emission/polycyclic aromatic hydrocarbon abundance of 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 SED of H II/star formation regions is compared to the equivalent Large Magellanic Cloud average H II/star formation region SED. These preliminary results will be expanded in detail in subsequent papers.

引用

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