Capak, P. and Aussel, H. and Ajiki, M. and McCracken, H. J. and Mobasher, B. and Scoville, N. and Shopbell, P. and Taniguchi, Y. and Thompson, D. and Tribiano, S. and Sasaki, S. and Blain, A. W. and Brusa, M. and Carilli, C. and Comastri, A. and Carollo, C. M. and Cassata, P. and Colbert, J. and Ellis, R. S. and Elvis, M. and Giavalisco, M. and Green, W. and Guzzo, L. and Hasinger, G. and Ilbert, O. and Impey, C. and Jahnke, K. and Kartaltepe, J. and Kneib, J.-P. and Koda, J. and Koekemoer, A. and Komiyama, Y. and Leauthaud, A. and Lefevre, O. and Lilly, S. and Liu, C. and Massey, R. and Miyazaki, S. and Murayama, T. and Nagao, T. and Peacock, J. A. and Pickles, A. and Porciani, C. and Renzini, A. and Rhodes, J. and Rich, M. and Salvato, M. and Sanders, D. B. and Scarlata, C. and Schiminovich, D. and Schinnerer, E. and Scodeggio, M. and Sheth, K. and Shioya, Y. and Tasca, L. A. M. and Taylor, J. E. and Yan, L. and Zamorani, G. (2007) The First Release COSMOS Optical and Near-IR Data and Catalog. Astrophysical Journal Supplement Series, 172 (1). pp. 99-116. ISSN 0067-0049. http://resolver.caltech.edu/CaltechAUTHORS:20100423-094539850
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We present imaging data and photometry for the COSMOS survey in 15 photometric bands between 0.3 and 2.4 μm. These include data taken on the Subaru 8.3 m telescope, the KPNO and CTIO 4 m telescopes, and the CFHT 3.6 m telescope. Special techniques are used to ensure that the relative photometric calibration is better than 1% across the field of view. The absolute photometric accuracy from standard-star measurements is found to be 6%. The absolute calibration is corrected using galaxy spectra, providing colors accurate to 2% or better. Stellar and galaxy colors and counts agree well with the expected values. Finally, as the first step in the scientific analysis of these data we construct panchromatic number counts which confirm that both the geometry of the universe and the galaxy population are evolving.
|Additional Information:||© 2007 American Astronomical Society. Received 2006 September 23; accepted 2007 April 6. We would like to thank the COSMOS team (http://cosmos.astro.caltech.edu), the staff at Caltech, CFHT, CTIO, KPNO, NAOJ, STSCI, TERAPIX, and the University of Hawaii for supporting this work and making it possible. Support for this work was provided by NASA grant HST-GO-09822 and NSF grant OISE-0456439. FLAMINGOS was designed and constructed by the IR instrumentation group (PI: R. Elston) at the University of Florida, Department of Astronomy, with support from NSF grant AST 97-31180 and Kitt Peak National Observatory. Funding for the Sloan Digital Sky Survey (SDSS) has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the US Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is at http://www.sdss.org. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, the Johns Hopkins University, Los Alamos National Laboratory, the Max Planck Institute for Astronomy, the Max Planck Institute for Astrophysics, New Mexico State University, the University of Pittsburgh, Princeton University, the United States Naval Observatory, and the University of Washington. D. T. acknowledges support from NASA through a Long Term Space Astrophysics grant (NAG5-10955, NRA-00-01-LTSA-064). This work is based (in part) on data products produced at the TERAPIX data center located at the Institut d’Astrophysique de Paris.|
|Subject Keywords:||cosmology: observations; galaxies: evolution; large-scale structure of universe; surveys|
|Official Citation:||P. Capak et al 2007 ApJS 172 99 doi: 10.1086/519081|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||23 Apr 2010 18:08|
|Last Modified:||25 Jun 2015 20:38|
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