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Title:
The Milky Way Tomography with SDSS. II. Stellar Metallicity
Authors:
Ivezić, Željko; Sesar, Branimir; Jurić, Mario; Bond, Nicholas; Dalcanton, Julianne; Rockosi, Constance M.; Yanny, Brian; Newberg, Heidi J.; Beers, Timothy C.; Allende Prieto, Carlos; Wilhelm, Ron; Lee, Young Sun; Sivarani, Thirupathi; Norris, John E.; Bailer-Jones, Coryn A. L.; Re Fiorentin, Paola; Schlegel, David; Uomoto, Alan; Lupton, Robert H.; Knapp, Gillian R.; Gunn, James E.; Covey, Kevin R.; Smith, J. Allyn; Miknaitis, Gajus; Doi, Mamoru; Tanaka, Masayuki; Fukugita, Masataka; Kent, Steve; Finkbeiner, Douglas; Munn, Jeffrey A.; Pier, Jeffrey R.; Quinn, Tom; Hawley, Suzanne; Anderson, Scott; Kiuchi, Furea; Chen, Alex; Bushong, James; Sohi, Harkirat; Haggard, Daryl; Kimball, Amy; Barentine, John; Brewington, Howard; Harvanek, Mike; Kleinman, Scott; Krzesinski, Jurek; Long, Dan; Nitta, Atsuko; Snedden, Stephanie; Lee, Brian; Harris, Hugh; Brinkmann, Jonathan; Schneider, Donald P.; York, Donald G.
Affiliation:
AA(Department of Astronomy, University of Washington, Seattle, WA 98195.), AB(Department of Astronomy, University of Washington, Seattle, WA 98195.), AC(Institute for Advanced Study, Princeton, NJ 08540.), AD(Princeton University Observatory, Princeton, NJ 08544.), AE(Department of Astronomy, University of Washington, Seattle, WA 98195.), AF(University of California, Santa Cruz, CA 95060.), AG(Fermi National Accelerator Laboratory, Batavia, IL 60510.), AH(Department of Physics, Applied Physics, and Astronomy, Rensselaer Polytechnic Institute, Troy, NY 12180.), AI(Department of Physics and Astronomy, Center for the Study of Cosmic Evolution (CSCE) and Joint Institute for Nuclear Astrophysics (JINA), Michigan State University, East Lansing, MI 48824.), AJ(McDonald Observatory and Department of Astronomy, University of Texas, Austin, TX 78712.), AK(Department of Physics, Texas Tech University, Lubbock, TX 79409.), AL(Department of Physics and Astronomy, Center for the Study of Cosmic Evolution (CSCE) and Joint Institute for Nuclear Astrophysics (JINA), Michigan State University, East Lansing, MI 48824.), AM(Department of Physics and Astronomy, Center for the Study of Cosmic Evolution (CSCE) and Joint Institute for Nuclear Astrophysics (JINA), Michigan State University, East Lansing, MI 48824.), AN(Research School of Astronomy and Astrophysics, Australian National University, Weston ACT 2611, Australia.), AO(Max Planck Institut für Astronomie, 69117 Heidelberg, Germany.), AP(Max Planck Institut für Astronomie, 69117 Heidelberg, Germany.; Department of Physics, University of Ljubljana, 1000 Ljubljana, Slovenia.), AQ(Lawrence Berkeley National Laboratory, Berkeley, CA 94720.), AR(Department of Physics and Astronomy, John Hopkins University, Baltimore, MD 21218.), AS(Princeton University Observatory, Princeton, NJ 08544.), AT(Princeton University Observatory, Princeton, NJ 08544.), AU(Princeton University Observatory, Princeton, NJ 08544.), AV(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.), AW(Department of Physics and Astronomy, Austin Peay State University, Clarksville, TN 37044.), AX(Fermi National Accelerator Laboratory, Batavia, IL 60510.), AY(Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan.), AZ(Department of Astronomy, Graduate School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan.), BA(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba, Japan.), BB(Fermi National Accelerator Laboratory, Batavia, IL 60510.), BC(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.), BD(US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86002.), BE(US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86002.), BF(Department of Astronomy, University of Washington, Seattle, WA 98195.), BG(Department of Astronomy, University of Washington, Seattle, WA 98195.), BH(Department of Astronomy, University of Washington, Seattle, WA 98195.), BI(Department of Astronomy, University of Washington, Seattle, WA 98195.), BJ(Department of Astronomy, University of Washington, Seattle, WA 98195.), BK(Department of Astronomy, University of Washington, Seattle, WA 98195.), BL(Department of Astronomy, University of Washington, Seattle, WA 98195.), BM(Department of Astronomy, University of Washington, Seattle, WA 98195.), BN(Department of Astronomy, University of Washington, Seattle, WA 98195.), BO(Apache Point Observatory, Sunspot, NM 88349-0059.), BP(Apache Point Observatory, Sunspot, NM 88349-0059.), BQ(Apache Point Observatory, Sunspot, NM 88349-0059.), BR(Apache Point Observatory, Sunspot, NM 88349-0059.), BS(Apache Point Observatory, Sunspot, NM 88349-0059.), BT(Apache Point Observatory, Sunspot, NM 88349-0059.), BU(Apache Point Observatory, Sunspot, NM 88349-0059.), BV(Apache Point Observatory, Sunspot, NM 88349-0059.), BW(Lawrence Berkeley National Laboratory, Berkeley, CA 94720.), BX(US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86002.), BY(Apache Point Observatory, Sunspot, NM 88349-0059.), BZ(Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802.), CA(University of Chicago, Astronomy and Astrophysics Center, and Enrico Fermi Institute, Chicago, IL 60637.)
Publication:
The Astrophysical Journal, Volume 684, Issue 1, pp. 287-325. (ApJ Homepage)
Publication Date:
09/2008
Origin:
UCP
ApJ Keywords:
Galaxy: Halo, Galaxy: Kinematics and Dynamics, Galaxy: Stellar Content, Galaxy: Structure, Methods: Data Analysis, Stars: Statistics
DOI:
10.1086/589678
Bibliographic Code:
2008ApJ...684..287I

Abstract

Using effective temperature and metallicity derived from SDSS spectra for ~60,000 F- and G-type main-sequence stars (0.2<g-r<0.6), we develop polynomial models for estimating these parameters from the SDSS u-g and g-r colors. These photometric estimates have similar error properties as those determined from SDSS spectra. We apply this method to SDSS photometric data for over 2 million F/G stars and measure the unbiased metallicity distribution for a complete volume-limited sample of stars at distances between 500 pc and 8 kpc. The metallicity distribution can be exquisitely modeled using two components with a spatially varying number ratio, which correspond to disk and halo. The two components also possess the kinematics expected for disk and halo stars. The metallicity of the halo component is spatially invariant, while the median disk metallicity smoothly decreases with distance from the Galactic plane from -0.6 at 500 pc to -0.8 beyond several kiloparsecs. The absence of a correlation between metallicity and kinematics for disk stars is in a conflict with the traditional decomposition in terms of thin and thick disks. We detect coherent substructures in the kinematics-metallicity space, such as the Monoceros stream, which rotates faster than the LSR, and has a median metallicity of [Fe/H]=-0.95, with an rms scatter of only ~0.15 dex. We extrapolate our results to the performance expected from the Large Synoptic Survey Telescope (LSST) and estimate that LSST will obtain metallicity measurements accurate to 0.2 dex or better, with proper-motion measurements accurate to ~0.5 mas yr-1, for about 200 million F/G dwarf stars within a distance limit of ~100 kpc (g<23.5).
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