MAPPING THE STELLAR STRUCTURE OF THE MILKY WAY THICK DISK AND HALO USING SEGUE PHOTOMETRY

We map the stellar structure of the Galactic thick disk and halo by applying color-magnitude diagram (CMD) fitting to photometric data from the Sloan Extension for Galactic Understanding and Exploration (SEGUE) survey. The SEGUE imaging scans allow, for the first time, a comprehensive analysis of Milky Way structure at both high and low latitudes using uniform Sloan Digital Sky Survey photometry. Incorporating photometry of all relevant stars simultaneously, CMD fitting bypasses the need to choose single tracer populations. Using old stellar populations of differing metallicities as templates, we obtain a sparse three-dimensional map of the stellar mass distribution at vertical bar Z vertical bar > 1 kpc. Fitting a smooth Milky Way model comprising exponential thin and thick disks and an axisymmetric power-law halo allows us to constrain the structural parameters of the thick disk and halo. The thick-disk scale height and length are well constrained at 0.75 +/- 0.07 kpc and 4.1 +/- 0.4 kpc, respectively. We find a stellar halo flattening within similar to 25 kpc of c/a = 0.88 +/- 0.03 and a power-law index of 2.75 +/- 0.07 (for 7 kpc less than or similar to R-GC less than or similar to 30 kpc). The model fits yield thick-disk and stellar halo densities at the solar location of rho(thick,) (circle dot) = 10(-2.3+/-0.1) M-circle dot pc(-3) and rho(halo, circle dot) = 10(-4.20+/-0.05) M-circle dot pc(-3), averaging over any substructures. Our analysis provides the first clear in situ evidence for a radial metallicity gradient in the Milky Way's stellar halo: within R less than or similar to 15 kpc the stellar halo has a mean metallicity of [Fe/H] similar or equal to -1.6, which shifts to [Fe/H] similar or equal to -2.2 at larger radii, in line with the two-component halo deduced by Carollo et al. from a local kinematic analysis. Subtraction of the best-fit smooth and symmetric model from the overall density maps reveals a wealth of substructures at all latitudes, some attributable to known streams and overdensities, and some new. A simple warp cannot account for the low latitude substructure, as overdensities occur simultaneously above and below the Galactic plane.