The Resolved Fraction of the Cosmic X‐Ray Background

Moretti, A.; Campana, S.; Lazzati, Davide; Tagliaferri, G.; Uk, IoA Cambridge

doi:10.1086/374335

Cited by 364 publications

(572 citation statements)

References 53 publications

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“…Also in this band the bestfit parameters are in excellent agreement with those of the XMM-COSMOS survey with smaller errors on α 2 due to a better sampling of the flux interval below the knee of the relation. A direct comparison with the compilation of Moretti et al (2003) who obtained α 2 = 1.44 ± 0.13 also shows a 1σ consistency. The bright end slope, α 1 = 2.2 ± 0.12 measured in this work is somewhat flatter than the expected Euclidean 2.5.…”

Section: Discussionsupporting

confidence: 74%

“…In the other energy bands our fits reproduce well the behaviour of the log N − log S relations also at the bright end side, though the bright end slopes remain slightly flatter that the canonical α 1 = 2.5. The data are compared to those obtained in the XMM-COSMOS survey , the HELLAS2XMM survey (Baldi et al 2002), the compilations of X-ray surveys produced by Moretti et al (2003) and Hasinger et al (2005), the Beppo-Sax survey (Fiore et al 2001;Giommi et al 2000), the Chandra deep surveys CDFN and CDFS (Rosati et al 2002;Bauer et al 2004), the RDSS (Hasinger et al 1993), the extended CDFS (Lehmer et al 2005), the ELAIS-S1 survey (Puccetti et al 2006) and the XMM-HBS survey (Della Ceca et al 2004). The black dashed lines represents the prediction of the X-ray background model of Gilli et al (2007).…”

Section: Number Countsmentioning

confidence: 99%

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XMM-Newtonobservations of the Lockman Hole: X-ray source catalogue and number counts

Brunner¹,

Cappelluti²,

Hasinger³

et al. 2007

A&A

130

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Context. The Lockman Hole field represents the sky area of lowest Galactic line-of-sight column density N H = 5.7 × 10 19 cm −2 . It was observed by the XMM-Newton X-ray observatory in 18 pointings for a total of 1.16 Ms (raw EPIC pn observing time) constituting the deepest XMM-Newton exposure so far. After the removal of time intervals with high particle background, the final effective exposure was 637 ks. Aims. We present a catalogue of the X-ray sources detected in the central 0.196 deg 2 of the field and discuss the derived number counts and X-ray colours. Methods. The analysis was performed using the XMM-SAS data analysis package version 6.0. The detection sensitivity and fraction of spurious detections was calibrated using Monte Carlo simulations. Results. In the 0.5−2.0 keV band, a sensitivity limit (defined as the faintest detectable source) of 1.9 × 10 −16 erg cm −2 s −1 was reached. The 2.0−10.0 keV band and 5.0−10.0 keV band sensitivity limits were 9×10 −16 erg cm −2 s −1 and 1.8×10 −15 erg cm −2 s −1 , respectively. A total of 409 sources above a detection likelihood of 10 (3.9 sigma) were found within a radius of 15 off the field centre, of which 340, 266, and 98 sources were detected in the soft, hard, and very hard bands, respectively. The number counts in each energy band are in close agreement with results from previous surveys and with the synthesis models of the X-ray background. Six percent of the Compton-thick source candidates have been selected from the X-ray colour-colour diagram. This fraction is consistent with the most recent predictions of X-ray background population synthesis models at our flux limits. We also estimated, for the first time, the log N − log S relation for Compton-thick AGN.

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Section: Discussionsupporting

confidence: 74%

Section: Number Countsmentioning

confidence: 99%

XMM-Newtonobservations of the Lockman Hole: X-ray source catalogue and number counts

Brunner¹,

Cappelluti²,

Hasinger³

et al. 2007

A&A

130

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“…The normalizations of the power-law components of the Chandraspectra were free in the fit, but the powerlaw normalizations of ObsIDs 16235 and 16305 were linked since the observations were taken close in time. The powerlaw normalization of the ROSAT spectrum was fixed tó -8.85 10 7 photons keV −1 cm −2 s −1 arcmin −2 (Moretti et al 2003). The instrumental background-subtracted spectra were modeled with xspec 25 v12.8.2 (Arnaud 1996).…”

Section: Chandra Background Modelingmentioning

confidence: 99%

Chandra and JVLA Observations of HST Frontier Fields Cluster MACS J0717.5+3745

Weeren

Ogrean

Jones

et al. 2017

ApJ

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To investigate the relationship between thermal and non-thermal components in merger galaxy clusters, we present deep JVLA and Chandraobservations of the HST Frontier Fields cluster MACSJ0717.5+3745. The Chandraimage shows a complex merger event, with at least four components belonging to different merging subclusters. Northwestof the cluster, ∼0.7 Mpc from the center, there is a ram-pressure-stripped core that appears to have traversed the densest parts of the cluster after entering the intracluster medium (ICM) from the direction of a galaxy filament to the southeast. We detect a density discontinuity north-northeastof this core, which we speculate is associated with a cold front. Our radio images reveal new details for the complex radio relic and radio halo in this cluster. In addition, we discover several new filamentary radio sources with sizes of 100-300kpc. A few of these seem to be connected to the main radio relic, while others are either embedded within the radio halo or projected onto it. A narrow-angled-tailed (NAT) radio galaxy, a cluster member, is located at the center of the radio relic. The steep spectrum tails of this active galactic nucleuslead into the large radio relic where the radio spectrum flattens again. This morphological connection between the NAT radio galaxy and relic provides evidence for reacceleration (revival) of fossil electrons. The presence of hot 20 keV ICM gas detected by Chandranear the relic location provides additional support for this re-acceleration scenario.

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“…We expect that there is a significant contribution from background AGN at these faint luminosities. Moretti et al (2003) consider the AGN contribution in a hard (2-10 keV) and soft (1-2 keV) energy band. We assume a standard AGN spectrum, a power law model with Γ = 1.44 (following Rosati et al 2002), to calculate the AGN flux in our 0.3-10 keV band.…”

Section: Agn Contaminationmentioning

confidence: 99%

“…We can then estimate the shape of the CLF intrinsic to the M 31 disc by removing the background AGN contribution according to Moretti et al (2003). In Fig.…”

Section: Agn Contaminationmentioning

confidence: 99%

An X-ray spectral survey of the disc of M 31 with XMM-Newton

Greening¹,

Barnard²,

Kolb³

et al. 2009

A&A

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Aims. We present the results of a complete spectral survey of the X-ray point sources detected in five XMM-Newton observations along the major axis of M 31 but avoiding the central bulge, aimed at establishing the population characteristics of X-ray sources in this galaxy. Methods. We obtained background subtracted spectra and lightcurves for each of the 335 X-ray point sources detected across the five observations from 2002. We also correlate our source list with those of earlier X-ray surveys and radio, optical and infra-red catalogues. Sources with more than 50 source counts are individually spectrally fit in order to create the most accurate luminosity functions of M 31 to date. Results. Based on the spectral fitting of these sources with a power law model, we observe a broad range of best fit photon index. From this distribution of best fit index, we identify 16 strong high mass X-ray binary system candidates in M 31. We show the first cumulative luminosity functions created using the best fit spectral model to each source with more than 50 source counts in the disc of M 31. The cumulative luminosity functions show a distinct flattening in the X-ray luminosity L X interval 37.0 log L X erg s −1 37.5. Such a feature may also be present in the X-ray populations of several other galaxies, but at a much lower statistical significance. We investigate the number of AGN present in our source list and find that above L X ∼ 1.4 × 10 36 erg s −1 the observed population is statistically dominated by the point source population of M 31.

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The Resolved Fraction of the Cosmic X‐Ray Background

Cited by 364 publications

References 53 publications

XMM-Newtonobservations of the Lockman Hole: X-ray source catalogue and number counts

XMM-Newtonobservations of the Lockman Hole: X-ray source catalogue and number counts

Chandra and JVLA Observations of HST Frontier Fields Cluster MACS J0717.5+3745

An X-ray spectral survey of the disc of M 31 with XMM-Newton

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