The Chandra Deep Field North Survey. XIII. 2 Ms Point-Source Catalogs

By D. Alexander, F. E. Bauer, W. N. Brandt, D. P. Schneider, A. Hornschemeier, C. Vignali, A. Barger, Patrick S. Broos, L. Cowie, G. Garmire and 4 more. 2003

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We present point-source catalogs for the ≈2 Ms exposure of the Chandra Deep Field North, currently the deepest X-ray observation of the universe in the 0.5–8.0 keV band. Five hundred and three (503) X-ray sources are detected over an ≈448 arcmin2 area in up to seven X-ray bands. Twenty (20) of these X-ray sources lie in the central ≈5.3 arcmin2 Hubble Deep Field North (13,600 sources deg-2). The on-axis sensitivity limits are ≈2.5 × 10-17 ergs cm-2 s-1 (0.5–2.0 keV) and ≈1.4 × 10-16 ergs cm-2 s-1 (2–8 keV). Source positions are determined using matched-filter and centroiding techniques; the median positional uncertainty is ≈0.″3. The X-ray colors of the detected sources indicate a broad variety of source types, although absorbed AGNs (including a small number of possible Compton-thick sources) are clearly the dominant type. We also match lower significance X-ray sources to optical counterparts and provide a list of 79 optically bright (R ≲ 23) lower significance Chandra sources. The majority of these sources appear to be starburst and normal galaxies. The average backgrounds in the 0.5–2.0 keV and 2–8 keV bands are 0.056 and 0.135 counts Ms-1 pixel-1, respectively. The background count distributions are very similar to Poisson distributions. We show that this ≈2 Ms exposure is approximately photon limited in all seven X-ray bands for regions close to the aim point, and we predict that exposures up to ≈25 Ms (0.5–2.0 keV) and ≈4 Ms (2–8 keV) should remain nearly photon limited. We demonstrate that this observation does not suffer from source confusion within ≈6′ of the aim point, and future observations are unlikely to be source-confusion limited within ≈3′ of the aim point even for source densities exceeding 100,000 deg-2. These analyses directly show that Chandra can achieve significantly higher sensitivities in an efficient, nearly photon-limited manner and be largely free of source confusion. To allow consistent comparisons, we have also produced point-source catalogs for the ≈1 Ms Chandra Deep Field South (CDF-S). Three hundred and twenty-six (326) X-ray sources are included in the main Chandra catalog, and an additional 42 optically bright X-ray sources are included in a lower significance Chandra catalog. We find good agreement with the photometry of the previously published CDF-S catalogs; however, we provide significantly improved positional accuracy.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/996c636b330c9e939136c6f374220c72f3287f78

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Citations in the corpus

The Hubble Deep Field North SCUBA Super-map - III. Optical and near-infrared properties of submillimetre galaxies (2005, background): “TheChandra 2 Msec image (Alexander et al. 2003) provides the deepest X-ray survey of any part of the sky.”
TOWARD THE STANDARD POPULATION SYNTHESIS MODEL OF THE X-RAY BACKGROUND: EVOLUTION OF X-RAY LUMINOSITY AND ABSORPTION FUNCTIONS OF ACTIVE GALACTIC NUCLEI INCLUDING COMPTON-THICK POPULATIONS (2014, methodology): “The 2-Ms catalog containing 503 sources from a survey area of 0.124 deg2 is presented by Alexander et al. (2003).”
THE CHANDRA DEEP FIELD-SOUTH SURVEY: 4 Ms SOURCE CATALOGS (2008, neutral): “…quality to those produced by runningWAVDETECT 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…”
Unveiling Obscured Accretion in the Chandra Deep Field-South (2007, background): “Sources with a direct X-ray detection Eighteen of the 135 sources have an X-ray detection in Alexander et al. (2003).”
The X-Ray-to-Optical Properties of Optically Selected Active Galaxies over Wide Luminosity and Redshift Ranges (2006, methodology): “To obtain monochromatic 2 keV X-ray luminosities (or upper limits) for these COMBO-17 AGNs, we match the sources to the E-CDF-S and theChandraDeep Field-South (CDF-S; Alexander et al. 2003) X-ray catalogs.”
AGN Host Galaxies at z ~ 0.4-1.3: Bulge-dominated and Lacking Merger-AGN Connection (2005, methodology): “…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 locally observed SMBH-host…”
CLUSTERING OF LOW-REDSHIFT (z ⩽ 2.2) QUASARS FROM THE SLOAN DIGITAL SKY SURVEY (2008, background): “Gilli et al. (2005) obtained a sample of nearly 260 AGN in the Chandra Deep Field North (CDF-N, Alexander et al. 2003; Barger et al. 2003) and South (CDF-S, Rosati et al. 2002) with spectroscopic redshifts.”
DUST OBSCURATION AND METALLICITY AT HIGH REDSHIFT: NEW INFERENCES FROM UV, Hα, AND 8 μm OBSERVATIONS OF z ∼ 2 STAR-FORMING GALAXIES (2010, methodology): “To accomplish this, we made several stacks of the deep Chandra 2 Ms X-ray data in the GOODS-North field (Alexander et al. 2003) for galaxies in both the Hα and larger UV samples, restricting the analysis to those galaxies with spectroscopic redshifts.”
THE EVOLUTION OF THE GALAXY REST-FRAME ULTRAVIOLET LUMINOSITY FUNCTION OVER THE FIRST TWO BILLION YEARS (2014, methodology): “In the GOODS-S field, we used the 4 Msec Chandra Deep Field—South (CDF-S) catalog of Xue et al. (2011); in GOODS-N, we used the 2Msec Chandra Deep Field—North catalog of Alexander et al. (2003).”
A Spectroscopic Survey of Redshift 1.4 ≲ z ≲ 3.0 Galaxies in the GOODS-North Field: Survey Description, Catalogs, and Properties (2006, background): “We further identify at least 3 of 11 AGNs in our sample that appear to be heavily dust obscured based on their power-law SEDs longward of 2 m (rest frame) and lack of detection in the deepChandra 2Ms data (Alexander et al. 2003).”
Swift BAT Survey of AGNs (2007, methodology): “With the recent Chandra and XMM data (e.g., Alexander et al. 2003; Giacconi et al. 2002; Yang et al. 2004;Mainieri et al. 2002, 2005; Szokoly et al. 2004; Zheng et al. 2004; Barger et al. 2001, 2003) there has been great progress in understanding the origin of the X-ray background and the evolution…”
Spitzer Observations of Massive, Red Galaxies at High Redshift (2005, methodology): “In this study we use the main and supplementary Chandra catalogs of Alexander et al. (2003).”
Luminosity-dependent evolution of soft X-ray selected AGN : New Chandra and XMM-Newton surveys (2005, methodology): “The flux–solid angle relation has been calculated from the “limiting flux map”, where the counts limit is divided by the soft–band exposure map (in seconds) and multiplied by the conversion factor of 5 · 10−12 erg s−1 cm−2 (Alexander et al., 2003).”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, positive): “Furthermore, the field has been targeted for deep Chandra observations that have a total integration time of 2 Ms (Alexander et al. 2003).”
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).”
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.”
COLOR–MAGNITUDE RELATIONS OF ACTIVE AND NON-ACTIVE GALAXIES IN THE CHANDRA DEEP FIELDS: HIGH-REDSHIFT CONSTRAINTS AND STELLAR-MASS SELECTION EFFECTS (2010, methodology): “In this paper, we aim to assess the role of AGNs in galaxy evolution by means of CMD analyses through the galaxy formation epoch, using the 2 Ms CDF surveys (e.g., Alexander et al. 2003; Luo et al. 2008) as well as superb complementary ultradeep multiwavelength data.”
GOODS-HERSCHEL: STAR FORMATION, DUST ATTENUATION, AND THE FIR–RADIO CORRELATION ON THE MAIN SEQUENCE OF STAR-FORMING GALAXIES UP TO z ≃ 4 (2014, background): “However, we do not attempt to remove from the star-forming galaxy sample those X-ray sources detected in the 2-MsCHANDRA data (Alexander et al. 2003; Bauer et al. 2004) whose optical-toNIR emission is dominated by the host galaxy.”