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<title>UTas ePrints - The star formation history of the large magellanic cloud</title>
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<meta content="Smecker-Hane, T.A." name="eprints.creators_name" />
<meta content="Cole, A.A." name="eprints.creators_name" />
<meta content="Gallagher, J.S." name="eprints.creators_name" />
<meta content="Stetson, P.B." name="eprints.creators_name" />
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<meta content="andrew.cole@utas.edu.au" name="eprints.creators_id" />
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<meta content="2007-11-29 00:23:37" name="eprints.datestamp" />
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<meta content="The star formation history of the large magellanic cloud" name="eprints.title" />
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<meta content="Using WFPC2 on board the Hubble Space Telescope, we have created deep color-magnitude diagrams in the V and I passbands for approximately 105 stars in a field at the center of the LMC bar and another in the disk. The main-sequence luminosity functions (LFs) from 19V23.5, the red clump and horizontal branch morphologies, and the differential Hess diagram of the two fields all strongly imply that the disk and bar have significantly different star formation histories (SFHs). The disk's SFH has been relatively smooth and continuous over the last 15 Gyr, while the bar's SFH was dominated by star formation episodes at intermediate ages. Comparison of the LF against predictions based on Padova theoretical stellar evolution models and an assumed age-metallicity relationship allows us to identify the dominant stellar populations in the bar with episodes of star formation that occurred from 4 to 6 and 1 to 2 Gyr ago. These events accounted for 25% and 15%, respectively, of its stellar mass. The disk field may share a mild enhancement in SF for the younger episode, and thus we identify the 4 to 6 Gyr episode with the formation of the LMC bar." name="eprints.abstract" />
<meta content="2002-02-10" name="eprints.date" />
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<meta content="The Astrophysical Journal" name="eprints.publication" />
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<meta content="Ardeberg, A., Gustafsson, B., Linde, P., & Nissen, P.-E. 1997, A&A, 322, L13 First citation in article | NASA ADS
Cole, A. A. 1998, ApJ, 500, L137 First citation in article | Full Text | NASA ADS
. 2000, Science, 289, 1149 First citation in article
Cole, A. A., Smecker-Hane, T. A., & Gallagher III, J. S. 2000, AJ, 120, 1808 (CSG00) First citation in article | Full Text | NASA ADS
Elson, R. A. W., Gilmore, G. F., & Santiago, B. X. 1997, MNRAS, 289, 157 First citation in article | NASA ADS
Gallagher III, J. S., Cole, A. A., Holtzman, J. A., & Smecker-Hane, T. A. 1999, in IAU Symp. 190, New Views of the Magellanic Clouds, ed. Y.-H. Chu, N. B. Suntzeff, J. E. Hesser, & D. A. Bohlender (San Francisco: ASP), 306 First citation in article
Gallagher III, J. S., Mould, J. R., de Feijter, E., Holtzman, J., Stappers, B., Watson, A., Trauger, J., & The WFPC2 Team. 1996, ApJ, 466, 732 First citation in article | NASA ADS
Gardiner, L. T., Sawa, M., & Fujimoto, M. 1994, MNRAS, 266, 567 First citation in article | NASA ADS
Girardi, L. 1999, MNRAS, 308, 818 First citation in article | NASA ADS
Girardi, L., Bressan, A., Bertelli, G., & Chiosi, C. 2000, A&AS, 141, 1 First citation in article
Girardi, L., & Salaris, M. 2001, MNRAS, 323, 109 First citation in article | NASA ADS
Hill, V., Andrievsky, S., & Spite, M. 1995, A&A, 293, 347 First citation in article | NASA ADS
Holtzman, J. A., Burrows, C. J., Casertano, S., Hester, J. J., Trauger, J. T., Watson, A. M., & Worthey, G. 1995, PASP, 107, 1065 First citation in article | NASA ADS
Holtzman, J. A., Gallagher III, J. S., Cole, A. A., Mould, J. R., Grillmair, C. J., & The WFPC2 Team. 1999, AJ, 118, 2262 (H99) First citation in article | Full Text | NASA ADS
Kroupa, P., Tout, C. A., & Gilmore, G. 1993, MNRAS, 262, 545 First citation in article | NASA ADS
Olsen, K. 1999, AJ, 117, 2244 First citation in article | Full Text | NASA ADS
Pagel, B. E. J., & Tautvaiien, G. 1998, MNRAS, 299, 535 First citation in article | NASA ADS
Smecker-Hane, T. A., Cole, A. A., Mandushev, G., & Gallagher III, J. S. 2001, in preparation First citation in article
Stetson, P. B. 1987, PASP, 99, 191 First citation in article | NASA ADS
. 1994, PASP, 106, 250 First citation in article | NASA ADS
Weinberg, M. D., & Nikolaev, S. 2001, ApJ, 548, 712 " name="eprints.referencetext" />
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<meta content="Cole, A.A." name="DC.creator" />
<meta content="Gallagher, J.S." name="DC.creator" />
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<meta content="Using WFPC2 on board the Hubble Space Telescope, we have created deep color-magnitude diagrams in the V and I passbands for approximately 105 stars in a field at the center of the LMC bar and another in the disk. The main-sequence luminosity functions (LFs) from 19V23.5, the red clump and horizontal branch morphologies, and the differential Hess diagram of the two fields all strongly imply that the disk and bar have significantly different star formation histories (SFHs). The disk's SFH has been relatively smooth and continuous over the last 15 Gyr, while the bar's SFH was dominated by star formation episodes at intermediate ages. Comparison of the LF against predictions based on Padova theoretical stellar evolution models and an assumed age-metallicity relationship allows us to identify the dominant stellar populations in the bar with episodes of star formation that occurred from 4 to 6 and 1 to 2 Gyr ago. These events accounted for 25% and 15%, respectively, of its stellar mass. The disk field may share a mild enhancement in SF for the younger episode, and thus we identify the 4 to 6 Gyr episode with the formation of the LMC bar." name="DC.description" />
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<h1 class="ep_tm_pagetitle">The star formation history of the large magellanic cloud</h1>
<p style="margin-bottom: 1em" class="not_ep_block"><span class="person_name">Smecker-Hane, T.A.</span> and <span class="person_name">Cole, A.A.</span> and <span class="person_name">Gallagher, J.S.</span> and <span class="person_name">Stetson, P.B.</span> (2002) <xhtml:em>The star formation history of the large magellanic cloud.</xhtml:em> The Astrophysical Journal, 566 (1). pp. 239-244. ISSN 0004-637X</p><p style="margin-bottom: 1em" class="not_ep_block"></p><table style="margin-bottom: 1em" class="not_ep_block"><tr><td valign="top" style="text-align:center"><a href="http://eprints.utas.edu.au/2514/1/15638.web.pdf"><img alt="[img]" src="http://eprints.utas.edu.au/style/images/fileicons/application_pdf.png" border="0" class="ep_doc_icon" /></a></td><td valign="top"><a href="http://eprints.utas.edu.au/2514/1/15638.web.pdf"><span class="ep_document_citation">PDF</span></a> - Full text restricted - Requires a PDF viewer<br />1194Kb</td><td><form method="get" accept-charset="utf-8" action="http://eprints.utas.edu.au/cgi/request_doc"><input value="3307" name="docid" accept-charset="utf-8" type="hidden" /><div class=""><input value="Request a copy" name="_action_null" class="ep_form_action_button" onclick="return EPJS_button_pushed( '_action_null' )" type="submit" /> </div></form></td></tr></table><p style="margin-bottom: 1em" class="not_ep_block">Official URL: <a href="http://dx.doi.org/10.1086/337985">http://dx.doi.org/10.1086/337985</a></p><div class="not_ep_block"><h2>Abstract</h2><p style="padding-bottom: 16px; text-align: left; margin: 1em auto 0em auto">Using WFPC2 on board the Hubble Space Telescope, we have created deep color-magnitude diagrams in the V and I passbands for approximately 105 stars in a field at the center of the LMC bar and another in the disk. The main-sequence luminosity functions (LFs) from 19V23.5, the red clump and horizontal branch morphologies, and the differential Hess diagram of the two fields all strongly imply that the disk and bar have significantly different star formation histories (SFHs). The disk's SFH has been relatively smooth and continuous over the last 15 Gyr, while the bar's SFH was dominated by star formation episodes at intermediate ages. Comparison of the LF against predictions based on Padova theoretical stellar evolution models and an assumed age-metallicity relationship allows us to identify the dominant stellar populations in the bar with episodes of star formation that occurred from 4 to 6 and 1 to 2 Gyr ago. These events accounted for 25% and 15%, respectively, of its stellar mass. The disk field may share a mild enhancement in SF for the younger episode, and thus we identify the 4 to 6 Gyr episode with the formation of the LMC bar.</p></div><table style="margin-bottom: 1em" border="0" cellpadding="3" class="not_ep_block"><tr><th valign="top" class="ep_row">Item Type:</th><td valign="top" class="ep_row">Article</td></tr><tr><th valign="top" class="ep_row">Additional Information:</th><td valign="top" class="ep_row">Copyright 2002. The American Astronomical Society</td></tr><tr><th valign="top" class="ep_row">Keywords:</th><td valign="top" class="ep_row">galaxies: stellar content, Hertzsprung-Russell diagram, Magellanic Clouds
</td></tr><tr><th valign="top" class="ep_row">Subjects:</th><td valign="top" class="ep_row"><a href="http://eprints.utas.edu.au/view/subjects/240101.html">240000 Physical Sciences > 240100 Astronomical Sciences > 240101 Astronomy and Astrophysics</a></td></tr><tr><th valign="top" class="ep_row">Collections:</th><td valign="top" class="ep_row">UNSPECIFIED</td></tr><tr><th valign="top" class="ep_row">ID Code:</th><td valign="top" class="ep_row">2514</td></tr><tr><th valign="top" class="ep_row">Deposited By:</th><td valign="top" class="ep_row"><span class="ep_name_citation"><span class="person_name">Dr. A.A. Cole</span></span></td></tr><tr><th valign="top" class="ep_row">Deposited On:</th><td valign="top" class="ep_row">29 Nov 2007 11:23</td></tr><tr><th valign="top" class="ep_row">Last Modified:</th><td valign="top" class="ep_row">07 Feb 2008 13:12</td></tr><tr><th valign="top" class="ep_row">ePrint Statistics:</th><td valign="top" class="ep_row"><a target="ePrintStats" href="/es/index.php?action=show_detail_eprint;id=2514;">View statistics for this ePrint</a></td></tr></table><p align="right">Repository Staff Only: <a href="http://eprints.utas.edu.au/cgi/users/home?screen=EPrint::View&eprintid=2514">item control page</a></p>
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