XBootes: An X‐Ray Survey of the NDWFS Bootes Field. II. The X‐Ray Source Catalog

Kenter, A.; Murray, Stephen S.; Forman, W.; Jones, Christine; Green, Paul; Kochanek, C. S.; Vikhlinin, A.; Fabricant, Daniel G.; Fazio, G. G.; Brand, Kate; Brown, M. J. I.; Dey, Arjun; Jannuzi, Buell T.; Najita, J.; McNamara, B. R.; Shields, J. C.; Rieke, M. J.

doi:10.1086/444379

Cited by 135 publications

(173 citation statements)

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“…1.-Chandra images, in the 0.5-2 keV energy band binned with 4" resolution, for three sources originally classified by Kenter et al (2005) as extended, that we found in deeper Chandra observations to be point-like. Fig.…”

Section: Agn and Galaxy Evolution Survey (Ages)mentioning

confidence: 61%

“…Using a wavelet decomposition, Kenter et al (2005) detected 3293 point sources in the full 0.5-7 keV band with n ≥ 4 X-ray counts. In addition, they detected 41 2 extended sources at a existence threshold equivalent to ≈ 3σ, using 0.5-2 keV band images.…”

Section: X-boötes Surveymentioning

confidence: 99%

“…We excluded all counts coming from the point sources catalogued in Kenter et al (2005) from both the background and source counts. In addition, we visually inspected the deep fields in the Boötes region to eliminate the point sources that were not catalogued by Kenter et al (2005). To avoid the survey border effect and the contamination by other extended sources inside the ring, the median sector count rate was determined and sectors with lower than 2σ or higher than 3σ deviation from the median of all the sectors were discarded from further calculations.…”

Section: X-ray Propertiesmentioning

confidence: 99%

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X-Ray-Selected Galaxy Groups in Boötes

Vajgel

Jones

Lopes

et al. 2014

ApJ

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We present the X-ray and optical properties of the galaxy groups selected in the Chandra X-Boötes survey. We used follow-up Chandra observations to better define the group sample and their X-ray properties. Group redshifts were measured from the AGES spectroscopic data. We used photometric data from the NOAO Deep Wide Field Survey (NDWFS) to estimate the group richness (N gals ) and the optical luminosity (L opt ). Our final sample comprises 32 systems at z < 1.75, with 14 below z = 0.35. For these 14 systems we estimate velocity dispersions (σ gr ) and perform a virial analysis to obtain the radii (R 200 and R 500 ) and total masses (M 200 and M 500 ) for groups with at least five galaxy members. We use the Chandra X-ray observations to derive the X-ray luminosity (L X ). We examine the performance of the group properties σ gr , L opt and L X , as proxies for the group mass. Understanding how well these observables measure the total mass is important to estimate how precisely the cluster/group mass function is determined. Exploring the scaling relations built with the X-Boötes sample and comparing these with samples from the literature, we find a break in the L X -M 500 relation at approximately. Thus, the mass-luminosity relation for galaxy groups cannot be described by the same power law as galaxy clusters. A possible explanation for this break is the dynamical friction, tidal interactions and projection effects which reduce the velocity dispersion values of the galaxy groups. By extending the cluster luminosity function to the group regime, we predict the number of groups that new X-ray surveys, particularly eROSITA, will detect. Based on our cluster/group luminosity function estimates, eROSITA will identify ∼1800 groups (L X = 10 41 − 10 43 ergs s −1 ) within a distance of 200 Mpc. Since groups lie in large scale filaments, this group sample will map the large scale structure of the local universe.

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Section: Agn and Galaxy Evolution Survey (Ages)mentioning

confidence: 61%

Section: X-boötes Surveymentioning

confidence: 99%

Section: X-ray Propertiesmentioning

confidence: 99%

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X-Ray-Selected Galaxy Groups in Boötes

Vajgel

Jones

Lopes

et al. 2014

ApJ

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“…The former refer to AGN at 0.25 < z < 0.8 selected in different wavebands. The radio data are taken from the Westerbork Synthesis Radio Telescope 1.4 GHz radio survey (de Vries et al 2002), the X-ray data are from the XBootes survey, covering the full AGES (AGN and Galaxy Evolution Survey) spectroscopic region Kenter et al 2005), while the mid-infared data are from A37, page 10 of 20 We also show some of the paths in the M BH (t) − M * (t) plane followed, during their evolution, by BHs (and by their host galaxies) reaching a final mass of M BH (z = 0) ≥ 10 9 M . the Spitzer IRAC Shallow Survey covering the full AGES field in all four IRAC bands (Eisenhardt et al 2004).…”

Section: The Distributions Of the Eddington Ratiomentioning

confidence: 99%

Triggering active galactic nuclei in hierarchical galaxy formation: disk instability vs. interactions

Menci

Gatti

Fiore

et al. 2014

A&A

141

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Using a state-of-the-art semi analytic model for galaxy formation, we investigated in detail the effects of black hole (BH) accretion triggered by disk instabilities (DI) in isolated galaxies on the evolution of the AGN population. Specifically, we took on, developed, and expanded the Hopkins & Quataert (2011, MNRAS, 411, 1027 model for the mass inflow following disk perturbations, based on a physical description of nuclear inflows and tested against aimed N-body simulations. We compared the evolution of AGN due to such a DI accretion mode with that arising in a scenario where galaxy interactions (IT mode) produce the sudden destabilization of large quantities of gas feeding the AGN; this constitutes the standard AGN feeding mode implemented in the earliest versions of most semi-analytic models. To study the maximal contribution of DI to the evolution of the AGN population, we extended and developed the DI model to assess the effects of changing the assumed disk surface density profile, and to obtain lower limits for the nuclear star formation rates associated to the DI accretion mode. We obtained the following results: i) For AGN with luminosity M 1450 > ∼ −26, the DI mode can provide the BH accretion needed to match the observed AGN luminosity functions up to z ≈ 4.5. In such a luminosity range and redshift, it constitutes a viable candidate mechanism to fuel AGN, and can compete with the IT scenario as the main driver of cosmological evolution of the AGN population. ii) The DI scenario cannot provide the observed abundance of high-luminosity QSO with M 1450 ≤ −26 AGN, as well as the abundance of high-redhshift z > ∼ 4.5 QSO with M 1450 ≤ −24. As found in our earliest works, the IT scenario provides an acceptable match to the observed luminosity functions up to z ≈ 6. iii) The dispersion of the distributions of Eddington ratio λ for low-and intermediate-luminosity AGN (bolometric L AGN = 10 43 −10 45 erg s −1 ) is predicted to be much smaller in the DI scenario compared to the IT mode. iv) The above conclusions concerning the DI mode are robust with respect to the explored variants of the DI model. We discuss the physical origin of our findings. Finally, we discuss how it is possible to pin down the dominant fueling mechanism of AGN in the low-intermediate luminosity range M 1450 > ∼ −26 where the DI and the IT modes are both viable candidates as the main drivers of the AGN evolution. We show that an interesting discriminant could be provided by the fraction of AGN with high Eddington ratios λ ≥ 0.5, since it increases with luminosity in the IT case, while the opposite is true in the DI scenario.

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“…While the deep, small area Chandra Deep Field South Survey (0.13 deg 2 ; Giacconi et al 2001;Xue et al 2011) has uncovered the faintest AGNs and has entered the flux regime where the number density of non-active galaxies surpasses that of active systems (Lehmer et al 2012), and medium-area surveys like XMM-Newton and Chandra-COSMOS (2.2 deg 2 ; Cappelluti et al 2007;Hasinger et al 2007;Elvis et al 2009;Brusa et al 2010;Civano et al 2012Civano et al , 2015Marchesi et al 2015) have identified nearly 2,000 moderate-luminosity AGNs (10 43 erg s −1 <L x < 10 44 erg s −1 ), the L x >10 45 erg s −1 population has been a missing tier in our hard X-ray census of supermassive black hole growth. This population began to be revealed with larger area (∼10 deg 2 ) surveys, such as XBoötes (9 deg 2 ; Kenter et al 2005;Murray et al 2005) and the Chandra Multi-wavelength Project (ChaMP, 10 deg 2 ; Kim et al 2007), as well as the more recent XMM-Newton survey in the Herschel ATLAS field (7.1 deg 2 ; Ranalli et al 2015). The advent of the widest-area surveys (>15 deg 2 ), including the "Stripe 82X" survey (LaMassa et al 2013a(LaMassa et al , 2013b, which, as we discuss below, now reaches ∼31.3 deg 2 , as well as the 50 deg 2 XMM-XXL (PI: Pierre) and the ∼877 deg 2 XMM-Serendipitous (Rosen et al 2015) surveys, provides a chance to study the evolution of the most luminous AGN in unprecedented detail.…”

Section: Introductionmentioning

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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XBootes: An X‐Ray Survey of the NDWFS Bootes Field. II. The X‐Ray Source Catalog

Cited by 135 publications

References 16 publications

X-Ray-Selected Galaxy Groups in Boötes

X-Ray-Selected Galaxy Groups in Boötes

Triggering active galactic nuclei in hierarchical galaxy formation: disk instability vs. interactions

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

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XBootes: An X‐Ray Survey of the NDWFS Bootes Field. II. The X‐Ray Source Catalog

Cited by 135 publications

References 16 publications

X-Ray-Selected Galaxy Groups in Boötes

X-Ray-Selected Galaxy Groups in Boötes

Triggering active galactic nuclei in hierarchical galaxy formation: disk instability vs. interactions

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

Contact Info

Product

Resources

About

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