THE CHANDRA DEEP FIELD-SOUTH SURVEY: 4 Ms SOURCE CATALOGS

By Yongquan Xue, B. Luo, W. N. Brandt, F. E. Bauer, B. Lehmer, Patrick S. Broos, D. Schneider, D. M. Alexander, M. Brusa, A. Comastri and 16 more. 2008

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We present source catalogs for the 4 Ms Chandra Deep Field-South (CDF-S), which is the deepest Chandra survey to date and covers an area of 464.5 arcmin2. We provide a main Chandra source catalog, which contains 740 X-ray sources that are detected with wavdetect at a false-positive probability threshold of 10−5 in at least one of three X-ray bands (0.5–8 keV, full band; 0.5–2 keV, soft band; and 2–8 keV, hard band) and also satisfy a binomial-probability source-selection criterion of P < 0.004 (i.e., the probability of sources not being real is less than 0.004); this approach is designed to maximize the number of reliable sources detected. A total of 300 main-catalog sources are new compared to the previous 2 Ms CDF-S main-catalog sources. We determine X-ray source positions using centroid and matched-filter techniques and obtain a median positional uncertainty of ≈0.″42. We also provide a supplementary catalog, which consists of 36 sources that are detected with wavdetect at a false-positive probability threshold of 10−5, satisfy the condition of 0.004 < P < 0.1, and have an optical counterpart with R < 24. Multiwavelength identifications, basic optical/infrared/radio photometry, and spectroscopic/photometric redshifts are provided for the X-ray sources in the main and supplementary catalogs. Seven hundred sixteen (≈97%) of the 740 main-catalog sources have multiwavelength counterparts, with 673 (≈94% of 716) having either spectroscopic or photometric redshifts. The 740 main-catalog sources span broad ranges of full-band flux and 0.5–8 keV luminosity; the 300 new main-catalog sources span similar ranges although they tend to be systematically lower. Basic analyses of the X-ray and multiwavelength properties of the sources indicate that >75% of the main-catalog sources are active galactic nuclei (AGNs); of the 300 new main-catalog sources, about 35% are likely normal and starburst galaxies, reflecting the rise of normal and starburst galaxies at the very faint flux levels uniquely accessible to the 4 Ms CDF-S. Near the center of the 4 Ms CDF-S (i.e., within an off-axis angle of 3′), the observed AGN and galaxy source densities have reached 9800+1300 − 1100 deg−2 and 6900+1100 − 900 deg−2, respectively. Simulations show that our main catalog is highly reliable and is reasonably complete. The mean backgrounds (corrected for vignetting and exposure-time variations) are 0.063 and 0.178 counts Ms−1 pixel−1 (for a pixel size of 0.″492) for the soft and hard bands, respectively; the majority of the pixels have zero background counts. The 4 Ms CDF-S reaches on-axis flux limits of ≈3.2 × 10−17, 9.1 × 10−18, and 5.5 × 10−17 erg cm−2 s−1 for the full, soft, and hard bands, respectively. An increase in the CDF-S exposure time by a factor of ≈2–2.5 would provide further significant gains and probe key unexplored discovery space.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/3e2e977568459a4fdc8e9d702850055c360dece5

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Citations in the corpus

The LABOCA survey of the Extended Chandra Deep Field South: A photometric redshift survey of submillimetre galaxies (2010, methodology): “6 SU M M A RY A N D C O N C L U S I O N S We use deep multicolour imaging of the ECDF-S in 17 bands to derive the photometric properties of the counterparts of SMGs in the LESS LABOCA survey of the ECDF-S (Weiß et al. 2009; Biggs et al. 2011).”
Cosmic X-ray surveys of distant active galaxies (2015, methodology): “A few indepth applications of these methods include Alexander et al (2005a), Brusa et al (2010), Laird et al (2010), Xue et al (2011), Lehmer et al (2012), Civano et al (2012), and Wang et al (2013).”
HST WFC3/IR OBSERVATIONS OF ACTIVE GALACTIC NUCLEUS HOST GALAXIES AT z ∼ 2: SUPERMASSIVE BLACK HOLES GROW IN DISK GALAXIES (2010, methodology): “Sample Selection We select AGN using X-ray data from the deep 2 Ms Chandra Deep Field South observations (Luo et al. 2008) in the WFC3 Early Release Science (ERS) field covered by the near-infrared mosaic (Windhorst et al. 2010).”
CANDELS: CONSTRAINING THE AGN–MERGER CONNECTION WITH HOST MORPHOLOGIES AT z ∼ 2 (2011, methodology): “…taken with HST/WFC3 as part of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS; Grogin et al. 2011; Koekemoer et al. 2011) with the 4 Ms Chandra observations of the Chandra Deep Field South (CDF-S; Xue et al. 2011), the deepest X-ray observations obtained to date.”
Tracing the cosmic growth of supermassive black holes to z ∼ 3 with Herschel (2014, methodology): “Olsen et al. (2013) analysed a mass-selected sample at z ∼2 within the Chandra Deep Field-South (CDF-S) and ended up with a high fraction (43–65 per cent) of star-forming galaxies likely hosting an AGN, according to the X-ray classification taken from Xue et al. (2011).”
A deep ALMA image of the Hubble Ultra Deep Field (2016, methodology): “As listed in Table 3, the catalogue produced by Xue et al. (2011) also yields detections of three more galaxies in our sample, but these detections are > 20 times fainter than the obvious X-ray AGN, and, depending on the adopted extinction correction, may in fact be explained by the star formation…”
X-RAY BINARY EVOLUTION ACROSS COSMIC TIME (2012, background): “Recent ultradeep Chandra and multiwavelength surveys (e.g. Xue et al. 2011) have permitted robust observational tests of these correlations in distant galaxies (see also the review of Brandt & Hasinger 2005).”
The MUSE Hubble Ultra Deep Field Survey: I. Survey description, data reduction and source detection (2017, background): “Thanks to a large range of ancillary data taken with other telescopes, Article published by EDP Sciences A1, page 1 of 20 including for example Chandra (Xue et al. 2011; Luo et al. 2017), XMM (Comastri et al. 2011), ALMA (Walter et al. 2016; Dunlop et al. 2017), Spitzer/IRAC (Labbé et al. 2015), and”
THE EVOLUTION OF GALAXY NUMBER DENSITY AT z < 8 AND ITS IMPLICATIONS (2016, methodology): “%) of X-ray sources down to ∼ 3 ×10−17ergcm−2s−1 over 464.5 arcmin2 at 0.5-8 keV are detected in deep optical data as part of the deepest 4 Msec Chandra imaging of the universe (Xue et al. 2011) in the HUDF area.”
THE CHANDRA COSMOS LEGACY SURVEY: OVERVIEW AND POINT SOURCE CATALOG (2016, background): “In the same Figure we compare our data with the 4 Ms CDFS (Xue et al. 2011) and the large area Stripe82 survey (LaMassa et al. 2013a,b) source flux distributions, respectively to the left and to the right of COSMOSLegacy flux distribution.”
The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies (2017, neutral): “Third, the object must not have a match in X-ray AGN catalogs compiled for the GOODS-North and GOODSSouth fields (e.g., Shao et al. 2010; Xue et al. 2011).”
What drives the growth of black holes (2011, background): “For example, the deepest X-ray surveys (the Chandra Deep Fields; CDFs; Brandt et al. 2001; Giacconi et al. 2002; Alexander et al. 2003b; Luo et al. 2008; Xue et al. 2011) can detect low-luminosity AGNs similar to NGC 4051 (see Fig.”
BLAST: RESOLVING THE COSMIC SUBMILLIMETER BACKGROUND (2009, background): “We find that 480 FIDEL sources meet this criteria, which is similar to the expected number of X-ray–detected AGN, based on the source density reported by (Luo et al. 2008).”
CANDELS MULTI-WAVELENGTH CATALOGS: SOURCE DETECTION AND PHOTOMETRY IN THE GOODS-SOUTH FIELD (2013, methodology): “…Origins Deep Survey (GOODS, Giavalisco et al. 2004); in the mid-IR (3.6–24 µm) wavelength with Spitzer as part of the GOODS Spitzer Legacy Program (PI: M. Dickinson); and in the X-ray with the deepest Chandra sky survey ever taken, with a total integration time of 4 Ms (Xue et al. 2011).”
STELLAR MASSES FROM THE CANDELS SURVEY: THE GOODS-SOUTH AND UDS FIELDS (2014, methodology): “Finally, CANDELS catalogs have been cross-matched with X-ray sources from the Chandra 4 Ms catalogs of Xue et al. (2011) and Rangel et al. (2013) (see Hsu et al. 2014) in the GOODS-S field and with the XMM-Newton sample of Ueda et al. (2008) in the UDS field.”