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Spitzer Sage Survey of the Large Magellanic Cloud. III. Star Formation and ~1000 New Candidate Young Stellar Objects

Whitney, B. A. and Sewilo, M. and Indebetouw, R. and Robitaille, T. P. and Meixner, M. and Gordon, K. and Meade, M. R. and Babler, B. L. and Harris, J. and Hora, J. L. and Bracker, S. and Povich, M. S. and Churchwell, E. B. and Engelbracht, C. W. and For, B.-Q. and Block, M. and Misselt, K. and Vijh, U. and Leitherer, C. and Kawamura, A. and Blum, R. D. and Cohen, M. and Fukui, Y. and Mizuno, A. and Mizuno, N. and Srinivasan, S. and Tielens, A. G. G. M. and Volk, K. and Bernard, J. P. and Boulanger, F. and Frogel, J. A. and Gallagher, J. and Gorjian, V. and Kelly, D. and Latter, W. B. and Madden, S. and Kemper, F. and Mould, J. R. and Nota, A. and Oey, M. S. and Olsen, K. A. and Onishi, T. and Paladini, R. and Panagia, N. and Perez-Gonzalez, P. and Reach, W. and Shibai, H. and Sato, S. and Smith, L. J. and Staveley-Smith, L. and Ueta, T. and van Dyk, S. D. and Werner, M. and Wolff, M. and Zaritsky, D. (2008) Spitzer Sage Survey of the Large Magellanic Cloud. III. Star Formation and ~1000 New Candidate Young Stellar Objects. Astronomical Journal, 136 (1). pp. 18-43. ISSN 0004-6256.

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We present ~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 ~2900 M_☉ and the total luminosity is ~2.1 × 10^6 L_☉ . By extrapolating the mass function with a standard initial mass function and integrating, we calculate a current star-formation rate of ~0.06 M_☉ yr^(–1), which is at the low end of estimates based on total ultraviolet and IR flux from the galaxy (~0.05 – 0.25 M_☉ 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.

Item Type:Article
Related URLs:
URLURL TypeDescription
Sewilo, M.0000-0003-2248-6032
Robitaille, T. P.0000-0002-8642-1329
Hora, J. L.0000-0002-5599-4650
Povich, M. S.0000-0001-9062-3583
Leitherer, C.0000-0003-2685-4488
Mould, J. R.0000-0003-3820-1740
Olsen, K. A.0000-0002-7134-8296
Paladini, R.0000-0002-5158-243X
Reach, W.0000-0001-8362-4094
Smith, L. J.0000-0002-0806-168X
van Dyk, S. D.0000-0001-9038-9950
Wolff, M.0000-0002-4013-5650
Zaritsky, D.0000-0002-5177-727X
Additional Information:© 2008. The American Astronomical Society. Received 2007 June 20; accepted 2008 April 1; published 2008 May 27. We thank the anonymous referee whose comments helped improve this paper. We thank Eva Villaver for providing helpful information about PNe. This work was supported by NASA grants to the Spitzer SAGE Legacy project (1275598, 1275588, 1282646, 1275421, 397380, 1275471, and 1282688), the Spitzer Theoretical Research Program (1290701; B. W., T. R.), the Spitzer Fellowship Program (R. I.), the NASA Theory Program (NNG05GH35G; B.W.), NASA grant NAG5-12595 (M. M., U. V.). This research is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA; has made use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the IR Processing and Analysis Center/California Institute of Technology, funded by NASA and the National Science Foundation; and has used the SIMBAD database, operated at CDS, Strasbourg, France.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Subject Keywords:circumstellar matter galaxies: dwarf infrared: stars Magellanic Clouds stars: formation stars: pre-main sequence
Issue or Number:1
Record Number:CaltechAUTHORS:20090731-090808353
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Official Citation:Spitzer Sage Survey of the Large Magellanic Cloud. III. Star Formation and ~1000 New Candidate Young Stellar Objects B. A. Whitney, M. Sewilo, R. Indebetouw, T. P. Robitaille, M. Meixner, K. Gordon, M. R. Meade, B. L. Babler, J. Harris, J. L. Hora, S. Bracker, M. S. Povich, E. B. Churchwell, C. W. Engelbracht, B-Q For, M. Block, K. Misselt, U. Vijh, C. Leitherer, A. Kawamura, R. D. Blum, M. Cohen, Y. Fukui, A. Mizuno, N. Mizuno, S. Srinivasan, A. G. G. M. Tielens, K. Volk, J-P. Bernard, F. Boulanger, J. A. Frogel, J. Gallagher, V. Gorjian, D. Kelly, W. B. Latter, S. Madden, F. Kemper, J. R. Mould, A. Nota, M. S. Oey, K. A. Olsen, T. Onishi, R. Paladini, N. Panagia, P. Perez-Gonzalez, W. Reach, H. Shibai, S. Sato, L. J. Smith, L. Staveley-Smith, T. Ueta, S. Van Dyk, M. Werner, M. Wolff, and D. Zaritsky 2008 The Astronomical Journal 136 18-43 doi: 10.1088/0004-6256/136/1/18
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:14751
Deposited By: Ruth Sustaita
Deposited On:01 Sep 2009 21:28
Last Modified:09 Mar 2020 13:19

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