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Stellar populations in three outer fields of the Large Magellanic Cloud

Geha, Marla C. and Holtzman, Jon A. and Mould, Jeremy R. and Gallagher, John S., III and Watson, Alan M. and Cole, Andrew A. and Grillmair, Carl J. and Stapelfeldt, Karl R. and Ballester, Gilda E. and Burrows, Christopher J. and Clarke, John T. and Crisp, David and Evans, Robin W. and Griffiths, Richard E. and Hester, J. Jeff and Hoessel, John G. and Scowen, Paul A. and Trauger, John T. and Westphal, James A. (1998) Stellar populations in three outer fields of the Large Magellanic Cloud. Astronomical Journal, 115 (3). pp. 1045-1056. ISSN 0004-6256. doi:10.1086/300252.

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We present Hubble Space Telescope photometry for three fields in the outer disk of the Large Magellanic Cloud (LMC) extending approximately 4 mag below the faintest main-sequence turnoff. We cannot detect any strongly significant differences in the stellar populations of the three fields based on the morphologies of the color-magnitude diagrams, the luminosity functions, and the relative numbers of stars in different evolutionary stages. Our observations therefore suggest similar star formation histories in these regions, although some variations are certainly allowed. The fields are located in two regions of the LMC: one is in the northeast and two are located in the northwest. Under the assumption of a common star formation history, we combine the three fields with ground-based data at the same location as one of the fields to improve statistics for the brightest stars. We compare this stellar population with those predicted from several simple star formation histories suggested in the literature, using a combination of the R-method of Bertelli et al. (1992) and comparisons with the observed luminosity function. The only model we consider that is not rejected by the observations is one in which the star formation rate is roughly constant for most of the LMC's history and then increases by a factor of 3 about 2 Gyr ago. Such a model has roughly equal numbers of stars older and younger than 4 Gyr, and thus is not dominated by young stars. This star formation history, combined with a closed-box chemical evolution model, is consistent with observations that the metallicity of the LMC has doubled in the past 2 Gyr.

Item Type:Article
Related URLs:
URLURL TypeDescription
Geha, Marla C.0000-0002-7007-9725
Mould, Jeremy R.0000-0003-3820-1740
Gallagher, John S., III0000-0001-8608-0408
Cole, Andrew A.0000-0003-0303-3855
Grillmair, Carl J.0000-0003-4072-169X
Stapelfeldt, Karl R.0000-0002-2805-7338
Crisp, David0000-0002-4573-9998
Additional Information:© 1998 American Astronomical Society. Received 1997 September 19; revised 1997 November 12. This work was supported in part by NASA under contract NAS 7-918 to JPL, and by a grant to M. C. G. from the New Mexico Space Grant Consortium. We thank B. Stappers for kindly providing the ground-based data used in this work.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
New Mexico Space Grant ConsortiumUNSPECIFIED
Subject Keywords:galaxies, stellar content; Magellanic Clouds; stars, evolution
Issue or Number:3
Record Number:CaltechAUTHORS:20150122-083945622
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Official Citation:Stellar Populations in Three Outer Fields of the Large Magellanic Cloud. Marla C. Geha et al. 1998 The Astronomical Journal 115 1045
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:53980
Deposited By: Ruth Sustaita
Deposited On:22 Jan 2015 19:19
Last Modified:10 Nov 2021 20:25

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