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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 448114.0, MPI für Astronomie / Publikationen_mpia
The Chandra COSMOS Survey. I. Overview and point source catalog
Authors:Elvis, Martin; Civano, Francesca; Vignali, Cristian; Puccetti, Simonetta; Fiore, Fabrizio; Cappelluti, Nico; Aldcroft, T. L.; Fruscione, Antonella; Zamorani, G.; Comastri, Andrea; Brusa, Marcella; Gilli, Roberto; Miyaji, Takamitsu; Damiani, Francesco; Koekemoer, Anton M.; Finoguenov, Alexis; Brunner, Hermann; Urry, C. M.; Silverman, John; Mainieri, Vincenzo; Hasinger, Guenther; Griffiths, Richard; Carollo, Marcella; Hao, Heng; Guzzo, Luigi; Blain, Andrew; Calzetti, Daniela; Carilli, C.; Capak, Peter; Ettori, Stefano; Fabbiano, Giuseppina; Impey, Chris; Lilly, Simon; Mobasher, Bahram; Rich, Michael; Salvato, Mara; Sanders, D. B.; Schinnerer, Eva; Scoville, N.; Shopbell, Patrick; Taylor, James E.; Taniguchi, Yoshiaki; Volonteri, Marta
Date of Publication (YYYY-MM-DD):2009
Title of Journal:The Astrophysical Journal Supplement Series
Start Page:158
End Page:171
Review Status:not specified
Audience:Experts Only
Abstract / Description:The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8 Ms, Chandra program that has imaged the central 0.5 deg2 of the COSMOS field (centered at 10 h , +02 o ) with an effective exposure of ~160 ks, and an outer 0.4 deg2 area with an effective exposure of ~80 ks. The limiting source detection depths are 1.9 × 10-16 erg cm-2 s-1 in the soft (0.5-2 keV) band, 7.3 × 10-16 erg cm-2 s-1 in the hard (2-10 keV) band, and 5.7 × 10-16 erg cm-2 s-1 in the full (0.5-10 keV) band. Here we describe the strategy, design, and execution of the C-COSMOS survey, and present the catalog of 1761 point sources detected at a probability of being spurious of <2 × 10-5 (1655 in the full, 1340 in the soft, and 1017 in the hard bands). By using a grid of 36 heavily (~50%) overlapping pointing positions with the ACIS-I imager, a remarkably uniform (±12%) exposure across the inner 0.5 deg2 field was obtained, leading to a sharply defined lower flux limit. The widely different point-spread functions obtained in each exposure at each point in the field required a novel source detection method, because of the overlapping tiling strategy, which is described in a companion paper. This method produced reliable sources down to a 7-12 counts, as verified by the resulting logN-logS curve, with subarcsecond positions, enabling optical and infrared identifications of virtually all sources, as reported in a second companion paper. The full catalog is described here in detail and is available online.
Free Keywords:catalogs; cosmology: observations; galaxies: evolution; quasars: general; surveys; X-rays: general
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/abs/2009ApJS..184..158E [ID No:1]
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