The Extended Chandra Deep Field-South Survey: Chandra Point-Source Catalogs

By B. Lehmer, W. N. Brandt, D. Alexander, F. E. Bauer, D. P. Schneider, P. Tozzi, Jacqueline Bergeron, G. Garmire, R. Giacconi, R. Gilli and 10 more. 2005

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We present Chandra point-source catalogs for the Extended Chandra Deep Field-South (E-CDF-S) survey. The E-CDF-S consists of four contiguous 250 ks Chandra observations covering an approximately square region of total solid angle ≈0.3 deg2, which flank the existing ≈1 Ms Chandra Deep Field-South (CDF-S). The survey reaches sensitivity limits of ≈1.1 × 10-16 and ≈6.7 × 10-16 ergs cm-2 s-1 for the 0.5-2.0 and 2-8 keV bands, respectively. We detect 762 distinct X-ray point sources within the E-CDF-S exposure; 589 of these sources are new (i.e., not previously detected in the ≈1 Ms CDF-S). This brings the total number of X-ray point sources detected in the E-CDF-S region to 915 (via the E-CDF-S and ≈1 Ms CDF-S observations). Source positions are determined using matched-filter and centroiding techniques; the median positional uncertainty is ≈0.″35. The basic X-ray and optical properties of these sources indicate a variety of source types, although absorbed active galactic nuclei (AGNs) seem to dominate. In addition to our main Chandra catalog, we constructed a supplementary source catalog containing 33 lower significance X-ray point sources that have bright optical counterparts (R < 23). These sources generally have X-ray-to-optical flux ratios expected for normal and starburst galaxies, which lack a strong AGN component. We present basic number-count results for our main Chandra catalog and find good agreement with the ≈1 Ms CDF-S for sources with 0.5-2.0 and 2-8 keV fluxes greater than 3 × 10-16 and 1 × 10-15 ergs cm-2 s-1, respectively. Furthermore, three extended sources are detected in the 0.5-2.0 keV band, which are found to be likely associated with galaxy groups or poor clusters at z ≈ 0.1-0.7; these have typical rest-frame 0.5-2.0 keV luminosities of (1-5) × 1042 ergs s-1.

Subfields: Computational Mechanics, Electrical and Electronic Engineering, Instrumentation

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Citations in the corpus

The deepest Herschel-PACS far-infrared survey: number counts and infrared luminosity functions from combined PEP/GOODS-H observations (2013, background): “…from an AGN, Magnelli et al. (2009, 2011) excluded from their sample all X-ray AGNs, i.e., sources detected in the GOODS-S/N Chandra catalogues (Alexander et al. 2003; Lehmer et al. 2005) with either LX[0.5−8.0 keV]> 3× 1042 erg s−1 or a hardness ratio greater than 0.8 (Bauer et al. 2004).”
THE CHANDRA DEEP FIELD-SOUTH SURVEY: 4 Ms SOURCE CATALOGS (2008, background): “…at the more typical false-positive probability threshold of 10−6 or 10−7 used in previous CDF studies (e.g., Alexander et al. 2003, hereafter A03; Lehmer et al. 2005, hereafter L05; L08), but also allows for flexibility in including additional legitimate sources that fall below the 10−6 or…”
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A statistical relation between the X-ray spectral index and Eddington ratio of active galactic nuclei in deep surveys (2013, methodology): “R-band magnitudes were taken from Brusa et al. (2010) and Lehmer et al. (2005) for COSMOS and E-CDF-S, respectively.”
DISSECTING PHOTOMETRIC REDSHIFT FOR ACTIVE GALACTIC NUCLEUS USING XMM- AND CHANDRA-COSMOS SAMPLES (2011, background): “The constraint of source redshifts has been a primary goal of deep pencil-beam (e.g., HUDF: Williams et al. (1996)), wide-area (e.g. AEGIS: Davis et al. (2007); COSMOS: Scoville et al. (2007), GOODS: Giavalisco et al. (2004); ECDFS: Lehmer et al. (2005); CFHTLS: Cuillandre & Bertin (2006)), as well ”
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).”
THE CHANDRA SOURCE CATALOG (2009, methodology): “…algorithm (Freeman et al. 2002). wavdetect has been used successfully with Chandra data by a number of authors (e.g., Brandt et al. 2001; Giaconni et al. 2002; Lehmer et al. 2005; Kim et al. 2007; Muno et al. 2009), and its capabilities and limitations are well known (e.g., Valtchanov et al. 2001).”
AN ALMA SURVEY OF SUBMILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: SOURCE CATALOG AND MULTIPLICITY (2013, background): “We therefore used ALMA in Cycle 0 to observe a large sample of submillimeter galaxies in the Extended Chandra Deep Field South (ECDFS), a 30′ × 30′ field with deep, multi–wavelength coverage from the radio to the X–ray (Giacconi et al. 2001; Giavalisco et al. 2004; Lehmer et al. 2005; Beckwith et al”
The X-Ray-to-Optical Properties of Optically Selected Active Galaxies over Wide Luminosity and Redshift Ranges (2006, methodology): “Table 1 lists the properties of the COMBO-17 AGN sample, including the COMBO-17 ID from Wolf et al. (2004), the E-CDF-S ID from Lehmer et al. (2005), the sources’ positions and redshifts, monochromatic 2500̊A and 2 keV fluxes and luminosities,αOX, the effective X-ray power-law photon index (Γ), R,…”
The 0.4 < z < 1.3 star formation history of the Universe as viewed in the far-infrared (2009, methodology): “Finally for the ECDF-S we used the 250 Ksec Chandra observations, which flank the 1 Ms CDF-S observations (Lehmer et al. 2005).”
ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: SURVEY DESCRIPTION (2016, background): “The UDF is situated in the 30′ Extended Chandra Deep Field South (ECDFS Lehmer et al. 2005) / GOODS-South (Giavalisco et al. 2004) / CANDELS (Grogin et al. 2011; Koekemoer et al. 2011) region, so the large–scale structure around this field is well quantified.”
Lyα Emission-Line Galaxies at z = 3.1 in the Extended Chandra Deep Field-South (2007, methodology): “…(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).”
THE 2 Ms CHANDRA DEEP FIELD-NORTH SURVEY AND THE 250 Ks EXTENDED CHANDRA DEEP FIELD-SOUTH SURVEY: IMPROVED POINT-SOURCE CATALOGS (2016, methodology): “…CDF-S, Luo et al. 2008; 4 Ms CDF-S, Xue et al. 2011, hereafter X11) are the two deepest Chandra surveys, and the latter is complemented by the 1Ms Extended-Chandra Deep Field-South (E-CDF-S, which consists of four flanking, contiguous 250 ks Chandra observations; Lehmer et al. 2005, hereafter L05).”
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