SEGUE: A SPECTROSCOPIC SURVEY OF 240,000 STARS WITH<i>g</i>= 14-20
B. Yanny(Fermi National Accelerator Laboratory), Constance M. Rockosi(University of California, Santa Cruz), Heidi Jo Newberg(Rensselaer Polytechnic Institute), G. R. Knapp(Princeton University), Jennifer Adelman-McCarthy(Fermi National Accelerator Laboratory), Bonnie Alcorn(Fermi National Accelerator Laboratory), S. Allam(Fermi National Accelerator Laboratory), Carlos Allende Prieto(University College London), Deokkeun An(The Ohio State University), Kurt S. Anderson(New Mexico State University), Scott F. Anderson(University of Washington), Coryn A. L. Bailer‐Jones(Max Planck Institute for Astronomy), Steve Bastian(Fermi National Accelerator Laboratory), Timothy C. Beers(Joint Institute for Nuclear Astrophysics), Eric F. Bell(Max Planck Institute for Astronomy), Vasily Belokurov(University of Cambridge), Dmitry Bizyaev(Crow Canyon Archaeological Center), Norm Blythe(Crow Canyon Archaeological Center), John J. Bochanski(University of Washington), William N. Boroski(Fermi National Accelerator Laboratory), J. Brinchmann(Centro de Astrofísica da Universidade do Porto), J. Brinkmann(Crow Canyon Archaeological Center), H. Brewington(Crow Canyon Archaeological Center), Larry Carey(University of Washington), K. M. Cudworth(University of Chicago), Michael L. Evans(University of Washington), N. W. Evans(University of Cambridge), Evalyn Gates(University of Chicago), B. T. Gänsicke(University of Warwick), Bruce Gillespie(Crow Canyon Archaeological Center), Gerald F. Gilmore(University of Cambridge), A. Nebot Gómez-Morán(Leibniz Institute for Astrophysics Potsdam), E. K. Grebel(Heidelberg University), Jim Greenwell(University of Washington), James E. Gunn(Princeton University), C. Jordan(Crow Canyon Archaeological Center), Wendell P. Jordan(Crow Canyon Archaeological Center), Paul Harding(Case Western Reserve University), Hugh C. Harris(United States Naval Observatory), John S. Hendry(Fermi National Accelerator Laboratory), Diana Holder(Crow Canyon Archaeological Center), Inese I. Ivans(Princeton University), Željko Ivezić(University of Washington), Sebastian Jester(Max Planck Institute for Astronomy), Jennifer A. Johnson(The Ohio State University), S. Kent(Fermi National Accelerator Laboratory), S. J. Kleinman(Crow Canyon Archaeological Center), A. Y. Kniazev(Max Planck Institute for Astronomy), J. Krzesiński(Crow Canyon Archaeological Center), Richard G. Kron(University of Chicago), N. Kuropatkin(Fermi National Accelerator Laboratory), Svetlana Lebedeva(Fermi National Accelerator Laboratory), Young Sun Lee(Joint Institute for Nuclear Astrophysics), R. French Leger(Fermi National Accelerator Laboratory), Sébastien Lépine(American Museum of Natural History), S. E. Levine(United States Naval Observatory), H. Lin(Fermi National Accelerator Laboratory), Daniel C. Long(Crow Canyon Archaeological Center), Craig Loomis(Princeton University), Robert H. Lupton(Princeton University), O. Malanushenko(Crow Canyon Archaeological Center), Viktor Malanushenko(Crow Canyon Archaeological Center), B. Margon(University of California, Santa Cruz), David Martínez‐Delgado(Max Planck Institute for Astronomy), P. McGehee(California Institute of Technology), D. Monet(United States Naval Observatory), Heather Morrison(Case Western Reserve University), Jeffrey A. Munn(United States Naval Observatory), Eric H. Neilsen(Fermi National Accelerator Laboratory), A. Nitta(Crow Canyon Archaeological Center), John E. Norris(Australian National University), Dan Oravetz(Crow Canyon Archaeological Center), Russell Owen(University of Washington), Nikhil Padmanabhan(Lawrence Berkeley National Laboratory), Kaike Pan(Crow Canyon Archaeological Center), Ruth Peterson(Fermi National Accelerator Laboratory), Jeffrey R. Pier(United States Naval Observatory), Jared Platson(Fermi National Accelerator Laboratory), P. Re Fiorentin(University of Ljubljana), Gordon T. Richards(Drexel University), Hans‐Walter Rix(Max Planck Institute for Astronomy), David J. Schlegel(Lawrence Berkeley National Laboratory), Donald P. Schneider(Pennsylvania State University), M. R. Schreiber(University of Valparaíso), A. Schwope(Leibniz Institute for Astrophysics Potsdam), Valena C. Sibley(Fermi National Accelerator Laboratory), Audrey Simmons(Crow Canyon Archaeological Center), Stephanie A. Snedden(Crow Canyon Archaeological Center), J. A. Smith(Austin Peay State University), L.G. Stark(University of Washington), Fritz Stauffer(Crow Canyon Archaeological Center), Matthias Steinmetz(Leibniz Institute for Astrophysics Potsdam), Chris Stoughton(Fermi National Accelerator Laboratory), Mark SubbaRao(Adler Planetarium), Alexander S. Szalay(Johns Hopkins University), Paula Szkody(University of Washington), Aniruddha R. Thakar(Johns Hopkins University), T. Sivarani(Joint Institute for Nuclear Astrophysics), D. L. Tucker(Fermi National Accelerator Laboratory), Alan Uomoto(Carnegie Observatories), Dan Vanden Berk(Pennsylvania State University), S. Vidrih(Heidelberg University), Yogesh Wadadekar(National Centre for Radio Astrophysics), S. Watters(Crow Canyon Archaeological Center), R. Wilhelm(Texas Tech University), Rosemary F. Ġ. Wyse(Johns Hopkins University), Jean Yarger(Crow Canyon Archaeological Center), D. B. Zucker(University of Cambridge)
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Abstract
The Sloan Extension for Galactic Understanding and Exploration (SEGUE) Survey obtained ≈240,000 moderateresolution (R ~ 1800) spectra from 3900 Å to 9000 Å of fainter Milky Way stars (14.0 < g < 20.3) of a wide \nvariety of spectral types, both main-sequence and evolved objects, with the goal of studying the kinematics and \npopulations of our Galaxy and its halo. The spectra are clustered in 212 regions spaced over three quarters of the \nsky. Radial velocity accuracies for stars are σ(RV) ~ 4 km s^(−1) at g < 18, degrading to σ(RV) ~ 15 km s^(−1) \nat g ~ 20. For stars with signal-to-noise ratio >10 per resolution element, stellar atmospheric parameters are estimated, including metallicity, surface gravity, and effective temperature. SEGUE obtained 3500 deg^2 of additional \nugriz imaging (primarily at low Galactic latitudes) providing precise multicolor photometry (σ(g, r, i) ~ 2%), \n(σ(u, z) ~ 3%) and astrometry (≈0".1) for spectroscopic target selection. The stellar spectra, imaging data, and \nderived parameter catalogs for this survey are publicly available as part of Sloan Digital Sky Survey Data Release 7.
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