Spitzer SAGE survey of the Large Magellanic Cloud.: III.: Star formation and ∼1000 new candidate Young Stellar Objects

被引：191

作者：

Whitney, B. A. ^{[1
]}

Sewilo, M. ^{[2
]}

Indebetouw, R. ^{[3
]}

Robitaille, T. P. ^{[4
]}

Meixner, M. ^{[2
]}

Gordon, K. ^{[5
]}

Meade, M. R. ^{[6
]}

Babler, B. L. ^{[6
]}

Harris, J. ^{[5
]}

Hora, J. L. ^{[7
]}

Bracker, S. ^{[6
]}

Povich, M. S. ^{[6
]}

Churchwell, E. B. ^{[6
]}

Engelbracht, C. W. ^{[5
]}

For, B-Q ^{[5
,8
]}

Block, M. ^{[5
]}

Misselt, K. ^{[5
]}

Vijh, U. ^{[2
]}

Leitherer, C. ^{[2
]}

Kawamura, A. ^{[9
]}

Blum, R. D. ^{[10
]}

Cohen, M. ^{[11
]}

Fukui, Y. ^{[9
]}

Mizuno, A. ^{[9
]}

Mizuno, N. ^{[9
]}

Srinivasan, S. ^{[12
]}

Tielens, A. G. G. M. ^{[13
]}

Volk, K. ^{[14
]}

Bernard, J-P. ^{[15
]}

Boulanger, F. ^{[16
]}

Frogel, J. A. ^{[17
]}

Gallagher, J. ^{[6
]}

Gorjian, V. ^{[18
]}

Kelly, D. ^{[5
]}

Latter, W. B. ^{[19
]}

Madden, S. ^{[20
]}

Kemper, F. ^{[21
]}

Mould, J. R. ^{[10
]}

Nota, A. ^{[2
]}

Oey, M. S. ^{[22
]}

Olsen, K. A. ^{[23
]}

Onishi, T. ^{[9
]}

Paladini, R. ^{[24
]}

Panagia, N. ^{[2
]}

Perez-Gonzalez, P. ^{[5
]}

Reach, W. ^{[24
]}

Shibai, H. ^{[9
]}

Sato, S. ^{[9
]}

Smith, L. J. ^{[2
,25
]}

Staveley-Smith, L. ^{[26
]}

机构：

[1] Space Sci Inst, 4750 Walnut St Suite 205, Boulder, CO 80301 USA

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

[3] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA

[4] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland

[5] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA

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

[7] Harvard Univ, Ctr Astrophys, Cambridge, MA 02138 USA

[8] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA

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

[10] Natl Opt Astron Observ, Tucson, AZ 85726 USA

[11] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA

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

[13] SOFIA Off, NASA Ames Res Ctr, Moffett Field, CA 94035 USA

[14] Gemini Observ, Hilo, HI 96720 USA

[15] CNRS, Ctr Etude Spatiale Rayonnements, F-31028 Toulouse, France

[16] CNRS, UPR 341, IAP, F-31028 Toulouse, France

[17] AURA Inc, Washington, DC 20005 USA

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

[19] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA

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

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

[22] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[23] Cerro Tololo Interamer Observ, La Serena, Chile

[24] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA

[25] UCL, Dept Phys & Astron, London WC1E 6BT, England

[26] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia

[27] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA

来源：

ASTRONOMICAL JOURNAL | 2008年 / 136卷 / 01期

基金：

英国科学技术设施理事会;

关键词：

circumstellar matter; galaxies : dwarf; infrared : stars; Magellanic Clouds; stars : formation; stars : pre-main sequence;

D O I：

10.1088/0004-6256/136/1/18

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present similar to 1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations. The YSOs are biased toward intermediate-to high-mass and young evolutionary stages, because these overlap less with galaxies and evolved stars in color-magnitude space. The YSOs are highly correlated spatially with atomic and molecular gas, and are preferentially located in the shells and bubbles created by massive stars inside. They are more clustered than generic point sources, as expected if star formation occurs in filamentary clouds or shells. We applied a more stringent color-magnitude selection to produce a subset of " high-probability" YSO candidates. We fitted the spectral-energy distributions (SEDs) of this subset and derived physical properties for those that were well fitted. The total mass of these well-fitted YSOs is similar to 2900 M-circle dot and the total luminosity is similar to 2.1 x 10(6)L(circle dot). By extrapolating the mass function with a standard initial mass function and integrating, we calculate a current star-formation rate of similar to 0.06M(circle dot) yr(-1), which is at the low end of estimates based on total ultraviolet and IR flux from the galaxy (similar to 0.05-0.25M(circle dot) yr(-1)), consistent with the expectation that our current YSO list is incomplete. Follow-up spectroscopy and further data mining will better separate the different IR-bright populations and likely increase the estimated number of YSOs. The full YSO list is available as electronic tables, and the SEDs are available as an electronic figure for further use by the scientific community.

引用

页码：18 / 43

页数：26

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