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The Milky Way Tomography with SDSS | | Mario Juric
; Zeljko Ivezic
; Alyson Brooks
; Robert H. Lupton
; David Schlegel
; Douglas Finkbeiner
; Nikhil Padmanabhan
; Nicholas Bond
; Constance M. Rockosi
; Gillian R. Knapp
; James E. Gunn
; Takahiro Sumi
; Donald Schneider
; J.C. Barentine
; Howard J. Brewington
; J. Brinkmann
; Masataka Fukugita
; Michael Harvanek
; S.J. Kleinman
; Jurek Krzesinski
; Dan Long
; Eric H. Neilsen
; Jr.
; Atsuko Nitta
; Stephanie A. Snedden
; Donald G. York
; | | Date: |
Tue, 18 Oct 2005 13:25:48 GMT (1824kb) | | Abstract: | Using the photometric parallax method, we estimate the distances to ~48 million stars detected by the Sloan Digital Sky Survey (SDSS), and map their three-dimensional number density distribution in the Galaxy. The data show strong evidence for a Galaxy consisting of an oblate halo, disk components, and a number of localized overdensities. The number density distribution of stars in the Solar neighborhood (D < 1.5kpc) favors a model having a ``thin’’ and a ``thick’’ exponential disk, with scale heights and lengths of H_1 ~ 280pc and L_1 ~ 2400pc, and H_2 ~ 1200pc and L_2 ~ 3500pc, respectively, and local thick-to-thin disk normalization
ho_{thick}(R_odot)/
ho_{thin}(R_odot) = 4%. The halo power law index is very poorly constrained, but we find an oblate halo with c/a ~ 0.5 to be strongly preferred. In addition to known features, a remarkable density enhancement covering over a thousand square degrees of sky is detected towards the constellation of Virgo, at distances of ~5-15 kpc, and is responsible for a factor of 2 number density excess. It may be a nearby tidal stream or a low-surface brightness dwarf galaxy merging with the Milky Way. The u-g color distribution of these stars implies metallicities lower than those of the thick disk, and consistent with the halo metallicity distribution. | | Source: | arXiv, astro-ph/0510520 | | Services: | Forum | Review | PDF | Favorites | |
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