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SEGUE, and the future of large scale surveys of the Galaxy

Published online by Cambridge University Press:  01 June 2008

Timothy C. Beers ,
Young Sun Lee  and
Daniela Carollo
Timothy C. Beers
Affiliation:
Department of Physics & Astronomy, CSCE: Center for the Study of Cosmic Evolution, and JINA: Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, MI 48824, USA email: [email protected], [email protected]
Young Sun Lee
Affiliation:
Department of Physics & Astronomy, CSCE: Center for the Study of Cosmic Evolution, and JINA: Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, MI 48824, USA email: [email protected], [email protected]
Daniela Carollo
Affiliation:
Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo Observatory, Cotter Road, Weston, ACT 2611, Australia, and INAF-Osservatorio Astronomico di Torino, 10025 Pino Torinese, Italy email: [email protected]
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Abstract

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The Sloan Extension for Galactic Exploration and Understanding (SEGUE) has now been completed. This is one of three surveys that were executed as part of the first extension of the Sloan Digital Sky Survey (SDSS-II), which consist of LEGACY, SUPERNOVA SURVEY, and SEGUE. The SEGUE program has obtained over 3600 square degrees of ugriz imaging of the sky outside the original SDSS-I footprint. The regions of sky targeted for SEGUE imaging were primarily at lower Galactic latitudes (|b| < 35°), in order to better sample the disk/halo interface of the Milky Way. SEGUE also obtained medium-resolution (R = 2000) spectroscopy, over the wavelength range 3800-9200 Å, for over 200,000 stars in 200 selected areas over the sky available from Apache Point, New Mexico. We discuss the determination of stellar atmospheric parameters (Teff, log g, and [Fe/H]) for these stars, and highlight several of the scientific results obtained to date. The proposed second extension of SDSS, known as SDSS-III, will include SEGUE-2, a program to roughly double the numbers of stars with available spectroscopy, as well as APOGEE, a program to obtain high-resolution (R = 20000) near-IR spectroscopy for over 100,000 stars in the disk, bulge and halo populations of the Galaxy. Other massive spectroscopic surveys of interest to Galactic science are also briefly discussed.

Keywords

Astronomical data bases: surveystechniques: spectroscopicmethods: data analysisstars: fundamental parametersGalaxy: diskhalo
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S254: The Galaxy Disk in Cosmological Context , June 2008 , pp. 461 - 468
Copyright
Copyright © International Astronomical Union 2009

References

Adelman-McCarthy, J. K., Agüeros, M. A., Allah, S. S, Allende Prieto, C., & Anderson, K. S. J., et al. 2008, ApJS, 175, 297Google Scholar
Allende Prieto, C., Beers, T. C., Wilhelm, R., Newberg, H. J., & Rockosi, C. M., et al. 2006, ApJ, 636, 804Google Scholar
Allende Prieto, C., Sivarani, T., Beers, T. C., Lee, Y. S., & Koesterke, L. et al. 2008, AJ, in press (arXiv:0710.5780)Google Scholar
Beers, T. C., Rossi, S., Norris, J. E., Ryan, S. G., & Shefler, T. 1999, AJ, 117, 981CrossRefGoogle Scholar
Belokurov, V., Zucker, D. B., Evans, N. W., Gilmore, G., & Vidrih, S., et al. 2006, ApJ, 642, L137CrossRefGoogle Scholar
Carollo, D., Beers, T. C., Lee, Y. S., Chiba, M., & Norris, J. E., et al. 2007, Nature, 450, 1020Google Scholar
Cenarro, A. J., Cardiel, N, Gorgas, J., Peletier, R. F., Vazdekis, A., & Prada, F. 2001, MNRAS, 326, 959Google Scholar
Ivezic, Z., Sesar, B., Juric, M., Bond, N., & Dalcanton, J., et al. 2008, ApJ, in press (arXiv:0804.3850)Google Scholar
Kirby, E. N., Simon, J. D., Geha, M., Guhathakurta, P., & Frebel, A. 2008, ApJ, submitted (arXiv:0807.1925)Google Scholar
Lee, Y. S., Beers, T. C., Sivarani, T., Allende Prieto, C., & Koesterke, L., et al. 2008, AJ, in press (arXiv:0710.5645)Google Scholar
Lee, Y. S., Beers, T. C., Sivarani, T., Johnson, J. A., & An, D., et al. 2008, AJ, in press (arXiv:0710.5778)Google Scholar
Re Fiorentin, P., Bailer-Jones, C. A. L., Lee, Y. S., Beers, T. C., & Sivarani, T., et al. 2007, A&A, 467, 1373Google Scholar
Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525Google Scholar
Wilhelm, R., Beers, T. C., & Gray, R. O. 1999, AJ, 117, 2308Google Scholar
Xue, X.-X., Rix, H.-W., Zhao, G., Re Fiorentin, P., & Naab, T., et al. 2008, ApJ, in press (arXiv:0801.1232)Google Scholar
Zucker, D. B., Belokurov, V., Evans, N. W., Wilkinson, M. I., Irwin, M. J., et al. 2006, ApJ, 643, L103CrossRefGoogle Scholar