THE CHANDRA COSMOS SURVEY. I. OVERVIEW AND POINT SOURCE CATALOG

By M. Elvis, F. Civano, C. Vignali, S. Puccetti, Fabrizio Fiore, N. Cappelluti, Tom Aldcroft, A. Fruscione, G. Zamorani, A. Comastri and 33 more. 2009

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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 10h, +02o) 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.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/eade171670ec24d51dc05c13db9d661cddd9b449

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Citations in the corpus

EVIDENCE FOR PopIII-LIKE STELLAR POPULATIONS IN THE MOST LUMINOUS Lyα EMITTERS AT THE EPOCH OF REIONIZATION: SPECTROSCOPIC CONFIRMATION (2015, background): “We find no detection in the Xrays, with a limit of < 1044 erg s−1 (Elvis et al. 2009).”
The bright end of the galaxy luminosity function at z≃7: before the onset of mass quenching? (2013, methodology): “The COSMOS field is imaged by the Chandra-COSMOS survey (Elvis et al. 2009), which has a limiting depth of 1.9×10−16 ergs/s/cm2/Hz in the 0.5-2.0 keV channel and 7.3×10−16 ergs/s/cm2/Hz in the 2-10 keV channel.”
The ALPINE-ALMA [CII] survey (2020, methodology): “…deep NIR YJHK imaging from the UltraVista Survey (McCracken et al. 2012), SPITZER 3.6 and 4.5 µm imaging (Sanders et al. 2007), with good X-ray coverage with both XMM-Newton (Hasinger et al. 2007) and Chandra (Elvis et al. 2009; Civano et al. 2016), as well as radio waves (Smolčić et al. 2017).”
A remarkably flat relationship between the average star formation rate and AGN luminosity for distant X-ray AGN. (2015, methodology): “…of AGN for our study, we use the publicly available X-ray catalogues for the CDF-N (Alexander et al. 2003b), CDF-S (Xue et al. 2010) and COSMOS (Cappelluti et al. 2009; Elvis et al. 2009) fields, restricted to the areas covered by PEP/GOODSH and HerMES observations as described above (see Fig.”
zCOSMOS – 10k-bright spectroscopic sample - The bimodality in the galaxy stellar mass function: exploring its evolution with redshift (2009, background): “COSMOS observations include good coverage of the field with multiband photometry from the UV (with GALEX, Zamojski et al. 2007), optical (with Subaru and CFHT, Taniguchi et al. 2007, Capak et al. 2007), NIR (with CTIO, KPNO, Capak et al. 2007, and CFHT, McCracken et al. 2010), to MIR and FIR (S-COSM”
THE COSMOS2015 CATALOG: EXPLORING THE 1 < z < 6 UNIVERSE WITH HALF A MILLION GALAXIES (2016, methodology): “Note that the X-ray detected sources from XMMCOSMOS (Hasinger et al. 2007; Cappelluti et al. 2007; Brusa et al. 2010) and Chandra COSMOS (Elvis et al. 2009; Civano et al. 2012) are flagged and not used here.”
IDENTIFYING LUMINOUS ACTIVE GALACTIC NUCLEI IN DEEP SURVEYS: REVISED IRAC SELECTION CRITERIA (2012, methodology): “The full catalog of Chandra sources contains 1761 sources, 1010 of which have optical/NIR and IRAC counterparts from Elvis et al. (2009) and Civano et al. (2011, in prep.) that meet the criteria described above.”
THE VLA-COSMOS SURVEY. IV. DEEP DATA AND JOINT CATALOG (2010, background): “…an equatorial field with a size of 2 deg2 (for an overview, see Scoville et al. 2007b) ranging from X-ray XMM-Newton and Chandra (Hasinger et al. 2007; Elvis et al. 2009), UV GALEX (Zamojski et al. 2007), optical and near-infrared groundbased (Taniguchi et al. 2007; Capak et al. 2007), optical…”
OBSCURATION-DEPENDENT EVOLUTION OF ACTIVE GALACTIC NUCLEI (2015, methodology): “In the COSMOS field we use the region covered by the Chandra observations performed between November 2006 and June 2007 (C-COSMOS, Elvis et al. 2009).”
A PUBLIC Ks-SELECTED CATALOG IN THE COSMOS/UltraVISTA FIELD: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR POPULATION PARAMETERS, (2013, methodology): “It contains X-ray data from XMM − Newton (Hasinger et al. 2007), and Chandra (Elvis et al. 2009), UV imaging from the GALEX satellite (Martin et al. 2005), extensive optical broad-band and optical mediumband imaging from the CFHT and Subaru telescopes (Taniguchi et al. 2007; Capak et al. 2007),…”
Observational evidence for intermediate-mass black holes (2017, methodology): “Using a stacking analysis of early-type galaxies in the Chandra COSMOS survey (0.9 deg2, 1.8 Ms; Elvis et al. 2009; Civano et al. 2012) and after removing the contribution from XRBs and hot gas to the X-ray emission, Paggi et al. (2016) also found that highly absorbed AGN are present in low-mass…”
A WEAK LENSING STUDY OF X-RAY GROUPS IN THE COSMOS SURVEY: FORM AND EVOLUTION OF THE MASS–LUMINOSITY RELATION (2009, methodology): “We have therefore developed a method to correct for this effect directly from the data by using the high-resolution Chandra observations of the COSMOS field which cover a contiguous area of 0.5 degrees2 with the best PSF (3′′, Elvis et al. 2009), sufficient to distinguish between cool-cores and AGN.”
THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY X-RAY MISSION (2013, methodology): “Huge strides have been made with sensitive surveys undertaken by the Chandra and XMM-Newton observatories (e.g., Alexander et al. 2003; Harrison et al. 2003; Luo et al. 2008; Elvis et al. 2009; Laird et al. 2009).”
THE CHANDRA COSMOS LEGACY SURVEY: OPTICAL/IR IDENTIFICATIONS (2015, methodology): “The Chandra COSMOS-Legacy project, i.e., the combination of the 1.8 Ms C-COSMOS survey (Elvis et al 2009) with 2.8 Ms of new Chandra ACIS-I observations (Paper I) is exploring a new region of the area versus flux space, by using an unusually large total exposure time (4.6 Ms total) with respect to…”
THE CHANDRA COSMOS LEGACY SURVEY: OVERVIEW AND POINT SOURCE CATALOG (2016, background): “Indeed, the large (1.8 Ms) Chandra COSMOS survey (C-COSMOS; Elvis et al. 2009, E09; Puccetti et al. 2009, P09; Civano et al. 2012) has already contributed significantly to the study of the early epochs of the Universe, finding: three luminous AGN residing in protoclusters between z∼4.55 and 5.3…”
3D-HST: A WIDE-FIELD GRISM SPECTROSCOPIC SURVEY WITH THE HUBBLE SPACE TELESCOPE (2012, background): “The galaxy is identified as an X-ray source by Elvis et al. (2009), but its distant redshift has not otherwise been identified; it has zphot = 0.48 in the catalog from Ilbert et al. (2009) and is too faint (i = 22.6) to be included in the zCOSMOS-bright sample (Lilly et al. 2007).”
THE XMM-NEWTON WIDE-FIELD SURVEY IN THE COSMOS FIELD (XMM-COSMOS): DEMOGRAPHY AND MULTIWAVELENGTH PROPERTIES OF OBSCURED AND UNOBSCURED LUMINOUS ACTIVE GALACTIC NUCLEI (2010, methodology): “The XMM-COSMOS sample presented in this catalog consists therefore of 1797 X-ray sources, 850 with Chandra detection (47.3%).”
THE 2 Ms CHANDRA DEEP FIELD-NORTH SURVEY AND THE 250 Ks EXTENDED CHANDRA DEEP FIELD-SOUTH SURVEY: IMPROVED POINT-SOURCE CATALOGS (2016, methodology): “…gain of net counts at 7–8 keV is modest due to increasing background toward high energies; and (3) the upper energy bound of 7 keV has been adopted for source detection and/or X-ray photometry by a number of other cataloging works (e.g., Elvis et al. 2009; Laird et al. 2009; Nandra et al. 2015).”