Chandra Deep Field South: The 1 Ms Catalog

By R. Giacconi, Andrew Zirm, Junxian Wang, Piero Rosati, M. Nonino, P. Tozzi, R. Gilli, V. Mainieri, G. Hasinger, Lisa J. Kewley and 8 more. 2002

485 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/a2b0f944b58d85cd0f209cd6bac7641684308778

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Citations in the corpus

Lyα Emission-Line Galaxies at z = 3.1 in the Extended Chandra Deep Field-South (2007, unknown): “…(GEMS; Rix et al. 2004); deep groundbasedUBVRIzJHK photometry from theMultiwavelength Survey by Yale-Chile (MUSYC; Gawiser et al. 2006b); mid- and far-IR observations from Spitzer, GOODS, and MUSYC; and deep X-ray data from Chandra (Giacconi et al. 2002; Alexander et al. 2003; Lehmer et al. 2005).”
Mass-to-Light Ratios of Field Early-Type Galaxies at z ~ 1 from Ultradeep Spectroscopy: Evidence for Mass-dependent Evolution (2005, background): “Giacconi et al. (2002) and Alexander et al. (2003) provide catalogs of the CDFS data.”
The evolution of the hard X-ray luminosity function of AGN (2009, methodology): “The Chandra Deep Fields-North (CDF-N; Alexander et al. 2003) and Chandra Deep Fields-South (CDF-S; Giacconi et al. 2002) have been key in studies of the XLF, providing the deepest available X-ray data and substantial programmes of spectroscopic follow-up of the X-ray sources to determine redshifts.”
AGN Host Galaxies at z ~ 0.4-1.3: Bulge-dominated and Lacking Merger-AGN Connection (2005, background): “The 1–2 Ms Chandra Deep Fields (CDF-N and CDF-S; Brandt et al. 2001; Giacconi et al. 2002), which have now resolved much of the cosmic X-ray background into moderate-luminosity AGNs at (Alexander et al. 2003; Barger et al. 2003;z ∼ 1 Szokoly et al. 2004), provide a unique AGN sample to probe these…”
THE CHANDRA COSMOS LEGACY SURVEY: OPTICAL/IR IDENTIFICATIONS (2015, background): “Chandra and XMM-Newton studies extended this relation to harder bands (Hornschemeier et al. 2001, 2-8 keV; Alexander et al. 2001, 2-8 keV; Giacconi et al. 2002, 0.5-10 keV; Fiore et al. 2003, 2-10 keV; Della Ceca et al. 2004, 4.5-7.5 keV; Cocchia et al. 2007, 2-10 keV).”
THE 2 Ms CHANDRA DEEP FIELD-NORTH SURVEY AND THE 250 Ks EXTENDED CHANDRA DEEP FIELD-SOUTH SURVEY: IMPROVED POINT-SOURCE CATALOGS (2016, background): “Below we summarize the most significant results for CDFN and E-CDF-S, respectively.”
The unresolved hard X-ray background: the missing source population implied by the Chandra and XMM-Newton deep fields (2004, background): “The Chandra Deep Field North (CDF-N) and Chandra Deep Field South (CDF-S) probe down to ∼1.4–2.8 × 10−16 erg cm−2s−1 (over 2–8 keV) and resolve ∼70–90 per cent of the background in this broad, hard band (Giacconi et al. 2002; Moretti et al. 2002; Alexander et al. 2003; and references therein).”
Multiwavelength Study of Massive Galaxies at z ~ 2. II. Widespread Compton-thick Active Galactic Nuclei and the Concurrent Growth of Black Holes and Bulges (2007, methodology): “The deepest X-ray surveys available to date, performed with the Chandra satellite in the Chandra Deep Field South (Giacconi et al. 2002; GOODS-South field, GOODSS hereafter),Chandra Deep Field North (Alexander et al. 2003a; GOODS-North, GOODS-N hereafter), and with XMM-Newton(e.g., Hasinger 2004 in ”
The HELLAS2XMM survey IV. Optical identifications and the evolution of the accretion luminosity in the Universe (2003, background): “Furthermore, the thick crosses, which represent the median with the quartile range in three flux intervals, show a general trend in the spectral shape, which becomes harder as the flux decreases (see e.g. Giacconi et al. 2002 and references therein).”
GMASS ultradeep spectroscopy of galaxies at $z$ ~ 2 - II. Superdense passive galaxies: how did they form and evolve? (2008, methodology): “We searched for individual emission from the 13 objects in the present sample by cross-correlating the IRAC positions of our targets with the positions of X-ray sources as catalogued by Giacconi et al. (2002) and Alexander et al. (2003).”
The Great Observatories Origins Deep Survey: Initial Results from Optical and Near-Infrared Imaging (2003, methodology): “THE CXO DATA CXO data in the GOODS fields were taken before the GOODS project began and are available from theCXO archive (Giacconi et al. 2002; Alexander et al. 2003).”
AEGIS-X: THE CHANDRA DEEP SURVEY OF THE EXTENDED GROTH STRIP (2008, methodology): “…to the total observed counts, and thus provides a better description of the nature of faint sources than classical approaches normally employed (e.g. Giacconi et al. 2002; Alexander et al. 2003; Kim et al. 2007). π(S) is the prior probability distribution, and reflects our prior knowledge of the…”
THE EVOLUTION OF X-RAY CLUSTERS OF GALAXIES (2002, methodology): “We have included the recent data from the Chandra Deep Fields North (Bauer et al. 2002) and South (Giacconi et al 2002), which have extended the number counts by two decades.”
Cosmological Evolution of the Hard X-Ray Active Galactic Nucleus Luminosity Function and the Origin of the Hard X-Ray Background (2003, background): “He compiled only spectroscopically identified sources in the Chandra deep field south (Giacconi et al. 2002), CDFN, Lockman Hole, Lynx field, and SSA field.”
Spitzer Power-Law Active Galactic Nucleus Candidates in the Chandra Deep Field-North (2007, background): “…withChandraandXMM-Newtonhave now resolved 70-90% of the cosmic X-ray background (CXRB) at 2-8 keV into discreet sources (Mushotzky et al. 2000; Giacconi et al. 2002; Alexander et al. 2003; Bauer et al. 2004; Worsley et al. 2004, 2005), detecting the majority of the Xray unobscured AGN…”
A synthesis model for AGN evolution: supermassive black holes growth and feedback modes (2008, background): “The latter two limits have been chosen to match the observational limits of recent deep (Chandra Deep Field South, CDFS; Giacconi et al. 2002) and medium-deep (XMM-COSMOS, XCosmos; Hasinger et al. ) surveys.”
Cosmic X-Ray Background and Earth Albedo Spectra with Swift BAT (2008, background): “The deepest X-ray surveys to date (Giacconi et al. 2002; Alexander et al. 2003; Hasinger 2004) have shown that up to virtually 100% of the<2 keV CXB radiation is accounted for by active galactic nuclei (AGNs) hosting accreting supermassive black holes (SMBHs).”