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The Dark Energy Survey: perspectives for resolved stellar population studies

Published online by Cambridge University Press:  13 April 2010

Basílio Santiago  and
Brian Yanny
Basílio Santiago
Affiliation:
Departamento de Astronomia, Universidade Federal do Rio Grande do Sul, CEP: 91501-970, Porto Alegre, Brazil email: santiago@if.ufrgs.br
Brian Yanny
Affiliation:
Fermi National Accelerator Laboratory, Chicago, Illinois, USA email: yanny@fnal.gov
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Abstract

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The Dark Energy Survey (DES) will cover 5000 sq. deg. in grizY filters. Although its main goals are related to cosmology, it will yield photometric measurements of over 108 stars, most of them belonging to the Galaxy. DES will increase the sampling depth of very low-luminosity stellar and sub-stellar species, such as white, red, and brown dwarfs, by a factor of several as compared to SDSS. The structure of the Galactic halo, including its complex sub-structures caused by accretion remnants and globular cluster tidal tails, will also be probed and analyzed. DES will also allow comparison of star counts between Northern and Southern Galactic hemispheres to unprecedented detail. Finally, a significant sample of stars in the outskirts of the Large Magellanic Cloud (LMC) will be studied, providing new light into the debate about the existence of an LMC spheroidal component. These, among other important research goals attainable with the DES stellar data, are discussed in this contribution.

Keywords

Surveysstars: statisticsGalaxy: stellar contentGalaxy: structureLocal Group
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 265 - 269
Copyright
Copyright © International Astronomical Union 2010

References

An, D., Johnson, J., Clem, J., et al. 2008, ApJS, 179, 326.CrossRefGoogle Scholar
Belokurov, V, Zucker, D., Evans, N., et al. ApJ, 654, 897CrossRefGoogle Scholar
Grillmair, C & Johnson, R. 2006 ApJ Letters, 639, L17CrossRefGoogle Scholar
Grillmair, C 2009 ApJ, 693, 1118CrossRefGoogle Scholar
Harris, H., Munn, J., Kilic, M., et al. 2006 AJ, 131, 571CrossRefGoogle Scholar
Hawley, S., Covey, K., & Knapp, G. 2002 AJ, 123, 3409CrossRefGoogle Scholar
Javiel, S., Santiago, B., & Kerber, L. 2005 A&A, 431, 73Google Scholar
Koch, A., Odenkirchen, M., Grebel, E., Martínez-Delgado, E., & Caldwell, J. 2004 ASPC, 327, 333Google Scholar
Koposov, S., de Jong, J., Belokurov, V., et al. 2007, ApJ, 669, 337CrossRefGoogle Scholar
Lee, K., Lee, H., Fahlman, G., & Sung, H. 2004 AJ, 128, 2838CrossRefGoogle Scholar
Santiago, B., Elson, R., & Gilmore, G. 1996, MNRAS, 281, 871CrossRefGoogle Scholar
Xu, Y., Deng, L., & Hu, J. 2007 MNRAS, 379, 1373CrossRefGoogle Scholar
Willman, B., Dalcanton, J., Martinez-Delgado, D., et al. 2005 ApJ, 626, L85CrossRefGoogle Scholar
Yanny, B., Newberg, H., Johnson, J., et al. 2009 ApJ, 700, 1282CrossRefGoogle Scholar