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Cosmos Photometric Redshifts with 30-Bands for 2-deg^2

Ilbert, O. and Capak, P. and Salvato, M. and Aussel, H. and McCracken, H. J. and Sanders, D. B. and Scoville, N. and Kartaltepe, J. and Arnouts, S. and Le Floc'h, E. and Mobasher, B. and Taniguchi, Y. and Lamareille, F. and Leauthaud, A. and Sasaki, S. and Thompson, D. and Zamojski, M. and Zamorani, G. and Bardelli, S. and Bolzonella, M. and Bongiorno, A. and Brusa, M. and Caputi, K. I. and Carollo, C. M. and Contini, T. and Cook, R. and Coppa, G. and Cucciati, O. and de la Torre, S. and de Ravel, L. and Franzetti, P. and Garilli, B. and Hasinger, G. and Iovino, A. and Kampczyk, P. and Kneib, J.-P. and Knobel, C. and Kovac, K. and Le Borgne, J. F. and Le Brun, V. and Le Fèvre, O. and Lilly, S. and Looper, D. and Maier, C. and Mainieri, V. and Mellier, Y. and Mignoli, M. and Murayama, T. and Pellò, R. and Peng, Y. and Pérez-Montero, E. and Renzini, A. and Ricciardelli, E. and Schiminovich, D. and Scodeggio, M. and Shioya, Y. and Silverman, J. and Surace, J. A. and Tanaka, M. and Tasca, L. and Tresse, L. and Vergani, D. and Zucca, E. (2009) Cosmos Photometric Redshifts with 30-Bands for 2-deg^2. Astrophysical Journal, 690 (2). pp. 1236-1249. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20090804-134612379

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Abstract

We present accurate photometric redshifts (photo-z) in the 2-deg^2 COSMOS field. The redshifts are computed with 30 broad, intermediate, and narrowbands covering the UV (Galaxy Evolution Explorer), visible near-IR (NIR; Subaru, Canada-France-Hawaii Telescope (CFHT), United Kingdom Infrared Telescope, and National Optical Astronomy Observatory), and mid-IR (Spitzer/IRAC). A χ^2 template-fitting method (Le Phare) was used and calibrated with large spectroscopic samples from the Very Large Telescope Visible Multi-Object Spectrograph and the Keck Deep Extragalactic Imaging Multi-Object Spectrograph. We develop and implement a new method which accounts for the contributions from emission lines ([O II], Hβ, Hα, and Lyα) to the spectral energy distributions (SEDs). The treatment of emission lines improves the photo-z accuracy by a factor of 2.5. Comparison of the derived photo-z with 4148 spectroscopic redshifts (i.e., Δz = z_s – z_p) indicates a dispersion of at σΔ_z/(1+z_s) = 0.007 at i^+_(AB) < 22.5, a factor of 2-6 times more accurate than earlier photo-z in the COSMOS, CFHT Legacy Survey, and the Classifying Object by Medium-Band Observations-17 survey fields. At fainter magnitudes i^+_( AB) < 24 and z < 1.25, the accuracy is σΔ_z/(1+z_s) = 0.012. The deep NIR and Infrared Array Camera coverage enables the photo-z to be extended to z ~ 2, albeit with a lower accuracy (σΔ_z/(1+z_s) = 0.06 at i^+_(AB) ~ 24). The redshift distribution of large magnitude-selected samples is derived and the median redshift is found to range from z m = 0.66 at 22 < i^+_(AB) < 22.5 to z_m = 1.06 at 24.5 < i^+_(AB) < 25. At i^+_(AB) < 26.0, the multiwavelength COSMOS catalog includes approximately 607,617 objects. The COSMOS-30 photo-z enables the full exploitation of this survey for studies of galaxy and large-scale structure evolution at high redshift.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/690/2/1236DOIArticle
http://www.iop.org/EJ/abstract/0004-637X/690/2/1236/PublisherArticle
ORCID:
AuthorORCID
Scoville, N.0000-0002-0438-3323
Surace, J. A.0000-0001-7291-0087
Additional Information:© 2009 The American Astronomical Society. Received 2008 August 15, accepted for publication 2008 September 10. Published 2008 December 8. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. The HST COSMOS program was supported through NASA grant HST-GO-09822. More information on the COSMOS survey is available at Web site http://www.astro.caltech.edu/cosmos. We also greatly appreciate the hospitality provided by the Aspen Center for Physics where this manuscript was completed. This article is based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc., under NASA contract NAS 5-26555. It is also based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. The research is also based on data collected at: the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESAscience mission with instruments and contributions directly funded by ESAMember States and NASA; the European Southern Observatory under Large Program 175.A-0839, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation; and the Canada–France–Hawaii Telescope (CFHT) with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the NRC and CADC of Canada, the CNRS of France, TERAPIX, and the University of Hawaii.
Group:COSMOS, Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASAHST-GO-09822
NASANAS 5-26555
NASA1407
ESA Member StatesUNSPECIFIED
European Southern Observatory175.A-0839
Association of Universities for Research in Astronomy, Inc. (AURA)UNSPECIFIED
NSFUNSPECIFIED
Canada-France-Hawaii Telescope (CFHT)UNSPECIFIED
National Research Council (NRC)UNSPECIFIED
Canadian Astronomy Data Centre (CADC) of CanadaUNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
TERAPIXUNSPECIFIED
University of HawaiiUNSPECIFIED
Subject Keywords:galaxies: distances and redshifts; galaxies: evolution; galaxies: formation
Record Number:CaltechAUTHORS:20090804-134612379
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20090804-134612379
Official Citation:Cosmos Photometric Redshifts with 30-Bands for 2-deg2 O. Ilbert, P. Capak, M. Salvato, H. Aussel, H. J. McCracken, D. B. Sanders, N. Scoville, J. Kartaltepe, S. Arnouts, E. Le Floc'h, B. Mobasher, Y. Taniguchi, F. Lamareille, A. Leauthaud, S. Sasaki, D. Thompson, M. Zamojski, G. Zamorani, S. Bardelli, M. Bolzonella, A. Bongiorno, M. Brusa, K. I. Caputi, C. M. Carollo, T. Contini, R. Cook, G. Coppa, O. Cucciati, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, G. Hasinger, A. Iovino, P. Kampczyk, J.-P. Kneib, C. Knobel, K. Kovac, J. F. Le Borgne, V. Le Brun, O. Le Fèvre, S. Lilly, D. Looper, C. Maier, V. Mainieri, Y. Mellier, M. Mignoli, T. Murayama, R. Pellò, Y. Peng, E. Pérez-Montero, A. Renzini, E. Ricciardelli, D. Schiminovich, M. Scodeggio, Y. Shioya, J. Silverman, J. Surace, M. Tanaka, L. Tasca, L. Tresse, D. Vergani, and E. Zucca 2009 ApJ 690 1236-1249 doi: 10.1088/0004-637X/690/2/1236
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:14794
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:01 Sep 2009 22:25
Last Modified:01 Mar 2017 20:15

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