Maqola

Spectroscopic Target Selection in the Sloan Digital Sky Survey: The Main Galaxy Sample

Michael A. StraussPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544David H. WeinbergDepartment of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210Robert H. LuptonPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544Vijay K. NarayananPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544James AnnisFermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510Mariangela BernardiDepartment of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637Michael R. BlantonFermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510Scott BurlesDepartment of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637Andrew J. ConnollyDepartment of Physics and Astronomy, University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA 15260Julianne J. DalcantonDepartment of Astronomy, University of Washington, Box 351580, Seattle, WA 98195Mamoru DoiInstitute of Astronomy, School of Science, University of Tokyo, Mitaka, Tokyo 181-0015, JapanDaniel J. EisensteinDepartment of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637Joshua A. FriemanDepartment of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637M. FukugitaInstitute for Advanced Study, Einstein Drive, Princeton, NJ 08540James E. GunnPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544Željko IvezićPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544S. KentFermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510Rita S. J. KimDepartment of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Avenue, Baltimore, MD 21218G. R. KnappPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544Richard G. KronDepartment of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637Jeffrey A. MunnUS Naval Observatory, Flagstaff Station, P.O. Box 1149, Flagstaff, AZ 86002-1149Heidi Jo NewbergDepartment of Physics, Rensselaer Polytechnic Institute, SC1C25, Troy, NY 12180Robert C. NicholDepartment of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15232Sadanori OkamuraDepartment of Astronomy, School of Science, University of Tokyo, Tokyo 181-0033, JapanThomas QuinnDepartment of Astronomy, University of Washington, Box 351580, Seattle, WA 98195M. RichmondDepartment of Physics, Rochester Institute of Technology, 85 Lomb Memorial Drive, Rochester, NY 14623-5603David J. SchlegelPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544Kazuhiro ShimasakuDepartment of Astronomy, School of Science, University of Tokyo, Tokyo 181-0033, JapanMark SubbaRaoDepartment of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637Alexander S. SzalayDepartment of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Avenue, Baltimore, MD 21218Dan Vanden BerkFermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510Michael S. VogeleyDepartment of Physics, Drexel University, 3141 Chestnut Street, Philadelphia, PA 19104B. YannyFermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510Naoki YasudaNational Astronomical Observatory, Mitaka, Tokyo 181-8588, JapanDonald G. YorkDepartment of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637Idit ZehaviDepartment of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637

2002en

ABI

Annotatsiya

We describe the algorithm that selects the main sample of galaxies for spectroscopy in the Sloan Digital Sky Survey from the photometric data obtained by the imaging survey. Galaxy photometric properties are measured using the Petrosian magnitude system, which measures flux in apertures determined by the shape of the surface brightness profile. The metric aperture used is essentially independent of cosmological surface brightness dimming, foreground extinction, sky brightness, and the galaxy central surface brightness. The main galaxy sample consists of galaxies with r-band Petrosian magnitude r < 17.77 and r-band Petrosian half-light surface brightness < 24.5 magnitudes per square arcsec. These cuts select about 90 galaxy targets per square degree, with a median redshift of 0.104. We carry out a number of tests to show that (a) our star-galaxy separation criterion is effective at eliminating nearly all stellar contamination while removing almost no genuine galaxies, (b) the fraction of galaxies eliminated by our surface brightness cut is very small (0.1%), (c) the completeness of the sample is high, exceeding 99%, and (d) the reproducibility of target selection based on repeated imaging scans is consistent with the expected random photometric errors. (abridged)

Hali tarjima qilinmagan

Identifikatorlar

DOI: 10.1086/342343

Iqtiboslar va manbalar

2 ta iqtibos0 ta foydalanilgan manba

Koʻrsatkichlar — AkademScholar