<i>AEGIS-X:</i>
                    THE
                    <i>CHANDRA</i>
                    DEEP SURVEY OF THE EXTENDED GROTH STRIP

Laird, E. S.; Nandra, K.; Georgakakis, A.; Aird, James; Barmby, P.; Conselice, Christopher J.; Coil, Alison L.; Davis, Marc; Faber, S. M.; Fazio, G. G.; Guhathakurta, Puragra; Koo, David C.; Sarajedini, Vicki L.; Willmer, Christopher N. A.

doi:10.1088/0067-0049/180/1/102

Cited by 224 publications

(329 citation statements)

References 41 publications

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“…In the EGS field we also identify two distinct surveys: 1) the series of eight pointings that reach a nominal depth of ∼200ks and were presented in Laird et al (2009), which we refer to as the AEGIS-XW(ide) survey; and 2) the AEGIS-XD(eep) survey (Nandra et al 2015) which took three of the original 200ks to a depth of ∼ 800ks. We adopt the deeper AEGIS-XD observations when available.…”

Section: Chandra X-ray Datamentioning

confidence: 99%

“…The X-ray data from all of our surveys were reduced with our own pipeline procedure, which is described in detail by Laird et al (2009) and Nandra et al (2015). We performed point source detection using the procedure described by Laird et al (2009) and applied a false Poisson probability threshold of < 4 × 10 −6 to generate catalogues of detected sources in the soft (0.5-2 keV), hard (2-7 keV), full (0.5-7 keV) or ultrahard (4-7 keV) observed energy bands.…”

Section: Chandra X-ray Datamentioning

confidence: 99%

“…We performed point source detection using the procedure described by Laird et al (2009) and applied a false Poisson probability threshold of < 4 × 10 −6 to generate catalogues of detected sources in the soft (0.5-2 keV), hard (2-7 keV), full (0.5-7 keV) or ultrahard (4-7 keV) observed energy bands. We combined the source lists in each band to create a merged catalogue, which is used in the counterpart identification procedure described in Section 2.2 below.…”

Section: Chandra X-ray Datamentioning

confidence: 99%

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The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z∼ 5

Aird

Coil

Georgakakis

et al. 2015

Monthly Notices of the Royal Astronomical Society

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373

559

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We present new measurements of the evolution of the X-ray luminosity functions (XLFs) of unabsorbed and absorbed Active Galactic Nuclei (AGNs) out to z ∼ 5. We construct samples containing 2957 sources detected at hard (2-7 keV) X-ray energies and 4351 sources detected at soft (0.5-2 keV) energies from a compilation of Chandra surveys supplemented by wide-area surveys from ASCA and ROSAT. We consider the hard and soft X-ray samples separately and find that the XLF based on either (initially neglecting absorption effects) is best described by a new flexible model parametrization where the break luminosity, normalization and faint-end slope all evolve with redshift. We then incorporate absorption effects, separately modelling the evolution of the XLFs of unabsorbed (20 < log N H < 22) and absorbed (22 < log N H < 24) AGNs, seeking a model that can reconcile both the hard-and soft-band samples. We find that the absorbed AGN XLF has a lower break luminosity, a higher normalization, and a steeper faint-end slope than the unabsorbed AGN XLF out to z ∼ 2. Hence, absorbed AGNs dominate at low luminosities, with the absorbed fraction falling rapidly as luminosity increases. Both XLFs undergo strong luminosity evolution which shifts the transition in the absorbed fraction to higher luminosities at higher redshifts. The evolution in the shape of the total XLF is primarily driven by the changing mix of unabsorbed and absorbed populations.

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Section: Chandra X-ray Datamentioning

confidence: 99%

Section: Chandra X-ray Datamentioning

confidence: 99%

Section: Chandra X-ray Datamentioning

confidence: 99%

See 1 more Smart Citation

The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z∼ 5

Aird

Coil

Georgakakis

et al. 2015

Monthly Notices of the Royal Astronomical Society

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373

559

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“…We match the NIR-selected catalogues with X-ray detected sources in the Chandra imaging of our fields (Alexander et al 2003;Xue et al 2011;Nandra et al 2015;Civano et al 2016), where all the Chandra data have been reprocessed using our own procedures (see Laird et al 2009;Georgakakis et al 2014;Nandra et al 2015;Aird et al 2015). We also extract X-ray data (total counts, background counts, and effective exposures) at the positions of the remaining NIR-selected sources that are not matched to a significant X-ray detection, We extract counts within a circular aperture that corresponds to a 70 per cent enclosed energy fraction for the exposure-weighted Chandra point spread function at each source position.…”

Section: Data and Sample Selectionmentioning

confidence: 99%

X-rays across the galaxy population – II. The distribution of AGN accretion rates as a function of stellar mass and redshift

Aird

Coil

Georgakakis

2017

Monthly Notices of the Royal Astronomical Society

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167

266

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We use deep Chandra X-ray imaging to measure the distribution of specific black hole accretion rates (L X relative to the stellar mass of the galaxy) and thus trace AGN activity within star-forming and quiescent galaxies, as a function of stellar mass (from 10 8.5 -10 11.5 M ⊙ ) and redshift (to z ∼ 4). We adopt near-infrared selected samples of galaxies from the CANDELS and UltraVISTA surveys, extract X-ray data for every galaxy, and use a flexible Bayesian method to combine these data and to measure the probability distribution function of specific black hole accretion rates, λ sBHAR . We identify a broad distribution of λ sBHAR in both starforming and quiescent galaxies-likely reflecting the stochastic nature of AGN fuelling-with a roughly power-law shape that rises toward lower λ sBHAR , a steep cutoff at λ sBHAR 0.1−1 (in Eddington equivalent units), and a turnover or flattening at λ sBHAR 10 −3 − 10 −2 . We find that the probability of a star-forming galaxy hosting a moderate λ sBHAR AGN depends on stellar mass and evolves with redshift, shifting toward higher λ sBHAR at higher redshifts. This evolution is truncated at a point corresponding to the Eddington limit, indicating black holes may self-regulate their growth at high redshifts when copious gas is available. The probability of a quiescent galaxy hosting an AGN is generally lower than that of a star-forming galaxy, shows signs of suppression at the highest stellar masses, and evolves strongly with redshift. The AGN duty cycle in high-redshift (z 2) quiescent galaxies thus reaches ∼20 per cent, comparable to the duty cycle in star-forming galaxies of equivalent stellar mass and redshift.

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“…MLE takes into account the distance between an X-ray source and ancillary objects within the search radius, the astrometric errors of the X-ray and ancillary sources, and the magnitude distribution of ancillary sources in the background to determine whether a potential multi-wavelength counterpart is more likely to be a background source or a true match. This method has been implemented in many X-ray surveys to identify reliable counterparts (e.g., Brusa et al 2007Brusa et al , 2010Cardamone et al 2008;Laird et al 2009;Luo et al 2010;Civano et al 2012;LaMassa et al 2013a;Marchesi et al 2015).…”

Section: Multi-wavelength Catalog Matchingmentioning

confidence: 99%

THE 31 DEG² RELEASE OF THE STRIPE 82 X-RAY SURVEY: THE POINT SOURCE CATALOG

LaMassa

Urry²,

Cappelluti

et al. 2016

ApJ

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We release the next installment of the Stripe 82 X-ray survey point-source catalog, which currently covers 31.3 deg 2 of the Sloan Digital Sky Survey (SDSS) Stripe 82 Legacy field. In total, 6181 unique X-ray sources are significantly detected with XMM-Newton (>5σ) and Chandra (>4.5σ). This catalog release includes data from XMM-Newton cycle AO 13, which approximately doubled the Stripe 82X survey area. The flux limits of the Stripe 82X survey are 8.7×10 −16 erg s −1 cm −2 , 4.7×10 −15 erg s −1 cm −2 , and 2.1×10 −15 erg s −1 cm −2 in the soft (0.5-2 keV), hard (2-10 keV), and full bands (0.5-10 keV), respectively, with approximate half-area survey flux limits of 5.4×10 −15 erg s −1 cm −2 , 2.9×10 −14 erg s −1 cm −2 , and 1.7×10 −14 erg s −1 cm −2 . We matched the X-ray source lists to available multi-wavelength catalogs, including updated matches to the previous release of the Stripe 82X survey; 88% of the sample is matched to a multi-wavelength counterpart. Due to the wide area of Stripe 82X and rich ancillary multi-wavelength data, including coadded SDSS photometry, mid-infrared WISE coverage, near-infrared coverage from UKIDSS and VISTA Hemisphere Survey, ultraviolet coverage from GALEX, radio coverage from FIRST, and far-infrared coverage from Herschel, as well as existing ∼30% optical spectroscopic completeness, we are beginning to uncover rare objects, such as obscured high-luminosity active galactic nuclei at high-redshift. The Stripe 82X point source catalog is a valuable data set for constraining how this population grows and evolves, as well as for studying how they interact with the galaxies in which they live.

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

Cited by 224 publications

References 41 publications

The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z∼ 5

The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z∼ 5

X-rays across the galaxy population – II. The distribution of AGN accretion rates as a function of stellar mass and redshift

THE 31 DEG² RELEASE OF THE STRIPE 82 X-RAY SURVEY: THE POINT SOURCE CATALOG

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

Cited by 224 publications

References 41 publications

The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z∼ 5

The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z∼ 5

X-rays across the galaxy population – II. The distribution of AGN accretion rates as a function of stellar mass and redshift

THE 31 DEG2 RELEASE OF THE STRIPE 82 X-RAY SURVEY: THE POINT SOURCE CATALOG

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Product

Resources

About

THE 31 DEG² RELEASE OF THE STRIPE 82 X-RAY SURVEY: THE POINT SOURCE CATALOG