THE DARK ENERGY SURVEY: PROSPECTS FOR RESOLVED STELLAR POPULATIONS
- Observatorio Nacional, Rua Gal. Jose Cristino 77, Rio de Janeiro, RJ-22460-040 (Brazil)
- Laboratorio Interinstitucional de e-Astronomia-LIneA, Rua Gal. Jose Cristino 77, Rio de Janeiro, RJ-20921-400 (Brazil)
- Fermi National Laboratory, P.O. Box 500, Batavia, IL 60510-5011 (United States)
- National Center for Supercomputing Applications, University of Illinois, 1205 West Clark Street, Urbanan, IL 61801 (United States)
- Institut d'Astrophysique de Paris, UMR 7095 CNRS, Universite Pierre et Marie Curie, 98 bis boulevard Arago, F-75014 Paris (France)
- Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510 (United States)
Wide angle and deep surveys, regardless of their primary purpose, always sample a large number of stars in the Galaxy and in its satellite system. Here we make a forecast of the expected stellar sample resulting from the Dark Energy Survey (DES) and the perspectives that it will open for studies of Galactic structure and resolved stellar populations in general. An estimated 1.2 x 10{sup 8} stars will be sampled in DES grizY filters in the southern equatorial hemisphere. This roughly corresponds to 20% of all DES sources. Most of these stars belong to the stellar thick disk and halo of the Galaxy. DES will probe low-mass stellar and sub-stellar objects at depths from three to eight times larger than those in the Sloan Digital Sky Survey (SDSS). The faint end of the main sequence (MS) will be densely sampled beyond 10 kpc. The slope of the low mass end of the stellar initial mass function (IMF) will be constrained to within a few hundredths of dex, even in the thick disk and halo. In the sub-stellar mass regime, the IMF slope will be potentially constrained to within dlog {phi}(m)/dlog m {approx_equal} 0.1. About 3 x 10{sup 4} brown dwarf candidates and at least 7.6 x 10{sup 5} white dwarf candidates will be selected, the latter embedded into the thick disk and halo, for future follow-up. The stellar halo flattening will also be constrained to within a few percent. DES will probe the MS of new Milky Way satellites and halo clusters for distances out to {approx_equal} 120 kpc, therefore yielding stellar surface density contrasts 1.6-1.7 times larger than those attainable with SDSS. It will also allow detection of these objects in the far reaches of the stellar halo, substantially increasing the number and quality of probes to the Galactic potential. Combined with northern samples, such as the SDSS, the DES stellar sample will yield constraints on the structure and stellar populations of Galactic components in unprecedented detail. In particular, the combined sample from both hemispheres will allow detailed studies of halo and thick disk asymmetries and triaxiality.
- OSTI ID:
- 21583109
- Journal Information:
- Astronomical Journal (New York, N.Y. Online), Vol. 141, Issue 6; Other Information: DOI: 10.1088/0004-6256/141/6/185; ISSN 1538-3881
- Country of Publication:
- United States
- Language:
- English
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