Luminosity-dependent evolution of soft X-ray selected AGN

Hasinger, G.; Miyaji, Takeshi; Schmidt, Maarten

doi:10.1051/0004-6361:20042134

Cited by 678 publications

(1,106 citation statements)

References 68 publications

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“…-, as reported by Gilli et al (2007) themselves, seems to be due to the assumed XLF for type-1 AGNs (from Hasinger et al 2005), which probably is contaminated at the level …”

Section: ´----mentioning

confidence: 55%

The NuSTAR Extragalactic Surveys: X-Ray Spectroscopic Analysis of the Bright Hard-band Selected Sample

Zappacosta

Comastri

Civano

et al. 2018

ApJ

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We discuss the spectral analysis of a sample of 63 active galactic nuclei (AGN) detected above a limiting flux of S 8 24 keV 7 10 14 =´-( -) erg s cm 1 2 --in the multi-tiered NuSTAR extragalactic survey program. The sources span a redshift range z 0 2.1 = -(median z 0.58 á ñ = ). The spectral analysis is performed over the broad 0.5-24keV energy range, combining NuSTAR with Chandra and/or XMM-Newton data and employing empirical and physically motivated models. This constitutes the largest sample of AGN selected at 10 keV > to be homogeneously spectrally analyzed at these flux levels. We study the distribution of spectral parameters such as photon index, column density (N H ), reflection parameter (R), and 10-40keV luminosity (L X ). Heavily obscured ( N log cm 23AGN constitute ∼25% (15-17 sources) and ∼2-3% (1-2 sources) of the sample, respectively. The observed N H distribution agrees fairly well with predictions of cosmic X-ray background population-synthesis models (CXBPSM). We estimate the intrinsic fraction of AGN as a function of N H , accounting for the bias against obscured AGN in a flux-selected sample. The fraction of CT AGN relative to N log cm 20 24AGN is poorly constrained, formally in the range 2-56% (90% upper limit of 66%). We derived a fraction ( f abs ) of obscured AGN ( N log cm 22 24as a function of L X in agreement with CXBPSM and previous z 1 < X-ray determinations. Furthermore, f abs at z 0.1 0.5 = -and L log erg s 43.6 44.3agrees with observational measurements/trends obtained over larger redshift intervals. We report a significant anti-correlation of R with L X (confirmed by our companion paper on stacked spectra) with considerable scatter around the median R values.

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“…-, as reported by Gilli et al (2007) themselves, seems to be due to the assumed XLF for type-1 AGNs (from Hasinger et al 2005), which probably is contaminated at the level …”

Section: ´----mentioning

confidence: 55%

The NuSTAR Extragalactic Surveys: X-Ray Spectroscopic Analysis of the Bright Hard-band Selected Sample

Zappacosta

Comastri

Civano

et al. 2018

ApJ

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“…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%

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

Brunner¹,

Cappelluti²,

Hasinger³

et al. 2007

A&A

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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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“…For example, the number density of soft X-ray sources with νL ν > 10 46 erg s −1 is measured to be ∼ 5 × 10 −11 Mpc −3 at z ∼ 1 and inferred (but not measured) to be much lower than ∼ 10 −12 Mpc −3 at z ∼ 0, based on the LF evolution measured at lower νL ν (see, e.g. Figure 5 of Hasinger et al 2005). Long-term monitoring surveys offer much better prospects for constraining the source population than snapshot surveys.…”

Section: High Energy Photon Spectrummentioning

confidence: 99%

Constraints on the local sources of ultra high-energy cosmic rays

Waxman

Loeb

2009

J. Cosmol. Astropart. Phys.

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Ultra high-energy cosmic rays (UHECRs) are believed to be protons accelerated in magnetized plasma outflows of extra-Galactic sources. The acceleration of protons to ∼ 10 20 eV requires a source power L > 10 47 erg s −1 . The absence of steady sources of sufficient power within the GZK horizon of 100 Mpc, implies that UHECR sources are transient. We show that UHECR "flares" should be accompanied by strong X-ray and γ-ray emission, and that X-ray and γ-ray surveys constrain flares which last less than a decade to satisfy at least one of the following conditions: (i) L > 10 50 erg s −1 ; (ii) the power carried by accelerated electrons is lower by a factor > 10 2 than the power carried by magnetic fields or by > 10 3 than the power in accelerated protons; or (iii) the sources exist only at low redshifts, z ≪ 1. The implausibility of requirements (ii) and (iii) argue in favor of transient sources with L > 10 50 erg s −1 .

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Luminosity-dependent evolution of soft X-ray selected AGN

Cited by 678 publications

References 68 publications

The NuSTAR Extragalactic Surveys: X-Ray Spectroscopic Analysis of the Bright Hard-band Selected Sample

The NuSTAR Extragalactic Surveys: X-Ray Spectroscopic Analysis of the Bright Hard-band Selected Sample

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

Constraints on the local sources of ultra high-energy cosmic rays

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