AEGIS-X: THE CHANDRA DEEP SURVEY OF THE EXTENDED GROTH STRIP

By E. Laird, K. Nandra, A. Georgakakis, J. Aird, Pauline Barmby, Christopher J. Conselice, A. Coil, Michael Davis, S. Faber, G. Fazio and 4 more. 2008

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We present the AEGIS-X survey, a series of deep Chandra ACIS-I observations of the Extended Groth Strip. The survey comprises pointings at eight separate positions, each with nominal exposure of 200 ks, covering a total area of approximately 0.67 deg2 in a strip of length 2 degrees. We describe in detail an updated version of our data reduction and point-source-detection algorithms used to analyze these data. A total of 1325 band-merged sources have been found to a Poisson probability limit of 4 × 10−6, with limiting fluxes of 5.3 × 10−17 erg cm2 s−1 in the soft (0.5–2 keV) band and 3.8 × 10−16 erg cm−2 s−1 in the hard (2–10 keV) band. We present simulations verifying the validity of our source-detection procedure and showing a very small, <1.5%, contamination rate from spurious sources. Optical/NIR counterparts have been identified from the DEEP2, CFHTLS, and Spitzer/Infrared Array Camera (IRAC) surveys of the same region. Using a likelihood ratio method, we find optical counterparts for 76% of our sources, complete to RAB = 24.1, and, of the 66% of the sources that have IRAC coverage, 94% have a counterpart to a limit of 0.9 μJy at 3.6 μm (mAB = 23.8). After accounting for (small) positional offsets in the eight Chandra fields, the astrometric accuracy of Chandra positions is found to be 0.″8 rms; however, this number depends both on the off-axis angle and the number of detected counts for a given source. All data products described in this paper are made available via a public Web site.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/60b20dce5a3a954f550fe1c7b43bdf373292ec17

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Citations in the corpus

OBSCURATION-DEPENDENT EVOLUTION OF ACTIVE GALACTIC NUCLEI (2015, methodology): “The source detection methodology is similar to that described in Laird et al. (2009) in the case of Chandra data.”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, unknown): “The GOODS-South Field The GOODS-S field is a region of sky located near the southern Chandra Deep Field (Giacconi et al. 2002) that has been targeted for some of the deepest observations ever taken by NASA’s Great Observatories Hubble, Chandra, and Spitzer.”
PRIMUS: THE DEPENDENCE OF AGN ACCRETION ON HOST STELLAR MASS AND COLOR (2011, methodology): “In all our fields we have used the likelihood ratio matching technique (e.g., Sutherland & Saunders 1992; Ciliegi et al. 2003; Brusa et al. 2007; Laird et al. 2009) to robustly identify the counterparts of each X-ray source in the PRIMUS targeting optical photometry (usually the i or R band, see…”
A NEW DIAGNOSTIC OF ACTIVE GALACTIC NUCLEI: REVEALING HIGHLY ABSORBED SYSTEMS AT REDSHIFT >0.3 (2011, methodology): “Spitzer/IRAC photometry is available in all four channels (available through the Spitzer Science Center, also see Barmby et al. 2008, for EGS).”
THE CHANDRA DEEP FIELD-SOUTH SURVEY: 4 Ms SOURCE CATALOGS (2008, methodology): “This procedure has previously been employed in similar forms in a number of studies (e.g., Getman et al. 2005; Nandra et al. 2005; Laird et al. 2009; Lehmer et al. 2009).”
X-ray spectral modelling of the AGN obscuring region in the CDFS: Bayesian model selection and catalogue (2014, methodology): “Data reduction and source detection followed Laird et al. (2009) and is described in detail in Rangel et al. (2013b,a).”
CANDELS: CONSTRAINING THE AGN–MERGER CONNECTION WITH HOST MORPHOLOGIES AT z ∼ 2 (2011, methodology): “2 according to the basic procedure described in Laird et al. (2009).”
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 SURVEY. I. OVERVIEW AND POINT SOURCE CATALOG (2009, background): “For example, the AEGIS-X survey (Laird et al. 2009) has 1032 soft sources, about double the number predicted at the 80% point.”
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).”
Cosmic X-ray surveys of distant active galaxies (2015, background): “…flux; e.g., the I-band magnitudes for AGNs range from brighter than 15th to fainter than 28th magnitude (e.g., Barger et al 2003b; Szokoly et al 2004; Laird et al 2009; Brusa et al 2010; Luo et al 2010; Pineau et al 2011; Rovilos et al 2011; Xue et al 2011; Civano et al 2012; Trichas et al 2012).”
The evolution of the hard X-ray luminosity function of AGN (2009, methodology): “A point source catalogue based on the full 2 Ms exposure obtained has been presented by Alexander et al. (2003); however we use our own reduction and source catalogue, again using the procedure described in Laird et al. (2009).”
THE STAR FORMATION MASS SEQUENCE OUT TO z = 2.5 (2012, methodology): “To search for signatures of AGN, we match the NMBS catalogs within a 1 arcsecond radius to the X-ray point source catalogs from the AEGIS-X survey (Laird et al. 2009) and the Chandra COSMOS survey (Elvis et al. 2009).”
DISSECTING PHOTOMETRIC REDSHIFT FOR ACTIVE GALACTIC NUCLEUS USING XMM- AND CHANDRA-COSMOS SAMPLES (2011, background): “In addition, an accurate and merged photometric AEGIS-X catalog is now available (Barro et al. 2011).”
THE CHANDRA COSMOS SURVEY. III. OPTICAL AND INFRARED IDENTIFICATION OF X-RAY POINT SOURCES (2012, methodology): “…method has become common recently and has been applied first to radio surveys (Ciliegi et al. 2005) and to several medium and faintChandra and XMM-Newtonsurveys (Cardamone et al. 2008, Laird et al. 2009, Aird et al. 2010, Luo et al. 2010, Brusa et al. 2010, Xue et al. 2011, Rovilos et al. 2011).”
A statistical relation between the X-ray spectral index and Eddington ratio of active galactic nuclei in deep surveys (2013, methodology): “The data were screened for hot pixels and cosmic afterglows as described in Laird et al. (2009), astrometric corrections made as described in Rangel et al. (2013) and the source spectra were extracted using the ACIS EXTRACT (AE) software package1 (Broos et al. 2010), using the positions of the…”
EVIDENCE FOR WIDE-SPREAD ACTIVE GALACTIC NUCLEUS-DRIVEN OUTFLOWS IN THE MOST MASSIVE z ∼ 1–2 STAR-FORMING GALAXIES (2014, background): “…1 from the Chandra Deep Fields North/South (Alexander et al. 2003; Xue et al. 2011; Brightman & Ueda 2012), Extended Chandra Deep Field South (Lehmer et al. 2005), AEGIS-X survey (Laird et al. 2009), Subaru XMM Deep Field (Ueda et al. 2008) and the SDSS J1030+0524 QSO field (Farrah et al. 2004).”