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THE Zcosmos 10K-BRIGHT SPECTROSCOPIC SAMPLE∗

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THE Zcosmos 10K-BRIGHT SPECTROSCOPIC SAMPLE∗ The Astrophysical Journal Supplement Series, 184:218–229, 2009 October doi:10.1088/0067-0049/184/2/218 C 2009. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE zCOSMOS 10k-BRIGHT SPECTROSCOPIC SAMPLE∗ Simon J. Lilly1, Vincent Le Brun2, Christian Maier1, Vincenzo Mainieri3, Marco Mignoli4, Marco Scodeggio5, Gianni Zamorani4, Marcella Carollo1, Thierry Contini6, Jean-Paul Kneib2, Olivier Le Fevre` 2, Alvio Renzini7, Sandro Bardelli4, Micol Bolzonella4, Angela Bongiorno8, Karina Caputi1, Graziano Coppa4, Olga Cucciati9, Sylvain de la Torre2, Loic de Ravel2, Paolo Franzetti5, Bianca Garilli5, Angela Iovino9, Pawel Kampczyk1, Katarina Kovac1, Christian Knobel1, Fabrice Lamareille6, Jean-Francois Le Borgne6, Roser Pello6, Yingjie Peng1, Enrique Perez-Montero´ 6, Elena Ricciardelli7, John D. Silverman1, Masayuki Tanaka3, Lidia Tasca2, Laurence Tresse2, Daniela Vergani4, Elena Zucca4, Olivier Ilbert10, Mara Salvato11, Pascal Oesch1, Umi Abbas2, Dario Bottini5, Peter Capak11, Alberto Cappi4, Paolo Cassata2, Andrea Cimatti11, Martin Elvis13, Marco Fumana5, Luigi Guzzo9, Gunther Hasinger8, Anton Koekemoer14, Alexei Leauthaud15, Dario Maccagni5, Christian Marinoni16, Henry McCracken16, Pierdomenico Memeo5, Baptiste Meneux8, Cristiano Porciani1, Lucia Pozzetti4, David Sanders10, Roberto Scaramella18, Claudia Scarlata11, Nick Scoville11, Patrick Shopbell11, and Yoshiaki Taniguchi19 1 Institute for Astronomy, ETH Zurich, Wolfgang-Pauli-strasse 27, 8093 Zurich, Switzerland 2 Laboratoire d’Astrophysique de Marseille, 38, rue Fred´ eric´ Joliot-Curie, 13388 Marseille Cedex 13, France 3 European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany 4 INAF Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna, Italy 5 INAF – IASF Milano, Via E. Bassini 15, 20133 Milano, Italy 6 Laboratoire d’Astrophysique de Toulouse/Tarbes, Universite´ de Toulouse, 14 avenue Edouard Belin, 31400 Toulouse, France 7 Dipartimento di Astronomia, Universita di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 8 Max-Planck-Institut fur¨ extraterrestrische Physik, Giessenbachstraße, 85748 Garching, Germany 9 INAF Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy 10 University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822-1839, USA 11 Department of Astronomy, Caltech, MC 105-24, 1200 East California Blvd., Pasadena, CA 91125, USA 12 Dipartimento di Astronomia, Universita` degli Studi di Bologna, Via Ranzani 1, 40127 Bologna, Italy 13 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 14 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 15 Berkeley Lab & Berkeley Center for Cosmological Physics, University of California, Lawrence Berkeley National Lab, 1 Cyclotron Road, MS 50-5005, Berkeley, CA 94720, USA 16 Centre de Physique Theorique, Case 907 – 13288 Marseille cedex 9, France 17 Institut d’Astrophysique de Paris, UMR7095 CNRS, Universite´ Pierre & Marie Curie, 75014 Paris, France 18 INAF – Osservatorio Astronomico di Roma, Osservatorio Astronomico di Roma, Via di Frascati 33, 00040 Monte Porzio Catone, Italy 19 Ehime University, 2-5 Bunkyo-cho, Matsuyama 790-8577 Japan Received 2009 March 19; accepted 2009 August 21; published 2009 September 15 ABSTRACT We present spectroscopic redshifts of a large sample of galaxies with IAB < 22.5 in the COSMOS field, measured from spectra of 10,644 objects that have been obtained in the first two years of observations in the zCOSMOS- bright redshift survey. These include a statistically complete subset of 10,109 objects. The average accuracy of individual redshifts is 110 km s−1, independent of redshift. The reliability of individual redshifts is described by a Confidence Class that has been empirically calibrated through repeat spectroscopic observations of over 600 galaxies. There is very good agreement between spectroscopic and photometric redshifts for the most secure Confidence Classes. For the less secure Confidence Classes, there is a good correspondence between the fraction of objects with a consistent photometric redshift and the spectroscopic repeatability, suggesting that the photometric redshifts can be used to indicate which of the less secure spectroscopic redshifts are likely right and which are probably wrong, and to give an indication of the nature of objects for which we failed to determine a redshift. Using this approach, we can construct a spectroscopic sample that is 99% reliable and which is 88% complete in the sample as a whole, and 95% complete in the redshift range 0.5 <z<0.8. The luminosity and mass completeness levels of the zCOSMOS-bright sample of galaxies is also discussed. Key words: cosmology: observations – galaxies: active – galaxies: distances and redshifts – galaxies: evolution – large-scale structure of universe – quasars: general – surveys Online-only material: color figure, machine-readable table 1. INTRODUCTION ∗ Based on observations undertaken at the European Southern Observatory (ESO) Very Large Telescope (VLT) under Large Program 175.A-0839. Also based on observations with the NASA/ESA Hubble Space Telescope, obtained The zCOSMOS project (Lilly et al. 2007, hereafter ZC-07) at the Space Telescope Science Institute, operated by AURA Inc., under NASA contract NAS 5-26555, with the Subaru Telescope, operated by the National is a major redshift survey of galaxies in the COSMOS field Astronomical Observatory of Japan, with the telescopes of the National using 600 hr of clear dark observing time on the VLT. The Optical Astronomy Observatory, operated by the Association of Universities survey consists of two parts. The first, zCOSMOS-bright, will for Research in Astronomy, Inc. (AURA) under cooperative agreement with ultimately consist of spectra of about 20,000 galaxies selected the National Science Foundation, and with the Canada–France–Hawaii 2 Telescope, operated by the National Research Council of Canada, the Centre to have IAB < 22.5 across the full 1.7 deg of the COSMOS field National de la Recherche Scientifique de France, and the University of Hawaii. (Scoville et al. 2007). It was designed to yield a high and fairly 218 No. 2, 2009 THE zCOSMOS 10k-BRIGHT SPECTROSCOPIC SAMPLE 219 uniform sampling rate across most of the field (about 70%), with images), where the spectroscopic sampling rate is in any case a high success rate in measuring redshifts (approaching 100% lower. Away from these edges, the fraction of added objects is at 0.5 <z<0.8) and to have sufficient velocity accuracy (about very small, being less than 0.5%. A comparison of the magni- 100 km s−1) to efficiently detect cosmic structures down to the tudes for the huge number of objects in both catalogs indicated scale of galaxy groups. The second part, zCOSMOS-deep, will that there is a negligible photometric offset between the CFHT consist of about 10,000 spectra of BAB < 25.25 galaxies, color- and HST photometry. It should be noted that, as a result of the selected to have redshifts in the 1.4 <z<3.0 redshift range and arbitrary HST roll angle, the diffraction spikes from the two lying in the central 1 deg2 region of the COSMOS field. sets of data are at different position angles. Because it is based After the first two observing seasons (2005 Spring and 2006 on high-resolution HST data, without even the effects of HST Spring), 83 of the 180 spectroscopic masks for zCOSMOS- diffraction spikes (because of the CFHT catalog), a negligibly bright have been observed, yielding a total of 10,644 spec- small area is obscured by foreground stars and no attempt at tra from which redshift measurements have been made or at- “masking” was made. The selection magnitude range is 15.0 < tempted. This so-called 10k sample has been used to carry out IAB < 22.5. a number of science investigations, including a reconstruction As noted in our earlier paper, the first 12 masks (7% of the of the galaxy density field to z ∼ 1(Kovacetal.2009a), the program total) were generated from an earlier target catalog production of a first group catalog (Knobel et al. 2009), several that had the same selection criteria but was based on the first studies of galaxy properties as a function of environment and season of HST images. These covered only part of the field redshift (Maier et al. 2009; Bolzonella et al. 2009; Pozetti et al. and their processing did not include subsequent improvements 2009; Cucciati et al. 2009; Iovino et al. 2009; Kovac et al. 2009b; such as correction for the effects of imperfect charge transfer. Tasca et al. 2009; Vergani et al. 2009; Zucca et al. 2009), studies As would be expected, the new catalog does not exactly match of the correlation function (Gilli et al. 2009; Meneux et al. 2009; the old one at the selection boundary IAB = 22.5, because of de la Torre et al. 2009; C. Porciani et al. 2009, in preparation), unavoidable small variations in the photometry. As a result, 172 and studies of active galactic nucleus (AGN; Brusa et al. 2009; of the objects observed in these first 12 masks do not, in fact, Silverman et al. 2009a, 2009b), far-IR (Caputi et al. 2008, 2009), appear in the newer 2006 target catalog. To deal with this small and radio sources (Bardelli et al. 2009). Studies of the merging complication, all 2571 objects in the 2005 target catalog that rate in the sample will be presented by L. de Ravel et al. (2009, would have disappeared in the 2006 version were transferred in preparation) and P. Kampcyzk et al. (2009, in preparation). across into the new catalog, an augmentation of 4.5%. These The redshifts have been used to calibrate photometric redshifts objects have been assigned a distinct target ID number beginning in Mandelbaum et al. (2008). with a “7” instead of the usual “8.” Because all but the first zCOSMOS, as with COSMOS generally, is undertaken in the 12 masks were designed with the newer 2006 catalog, these spirit of a Legacy Program with prompt public release of data objects comprise only 1.6% of the present 10k sample, and products.
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