The XMM-Newton survey of the ELAIS-S1 field

Puccetti, S.; Fiore, F.; D’Elia, V.; Pillitteri, I.; Feruglio, C.; Grazian, A.; Brusa, M.; Ciliegi, P.; Comastri, A.; Gruppioni, C.; Mignoli, M.; Vignali, C.; Zamorani, G.; Franca, F. La; Sacchi, N.; Franceschini, A.; Berta, S.; Buttery, H.; Dias, J. E.

doi:10.1051/0004-6361:20064904

Cited by 73 publications

(111 citation statements)

References 53 publications

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“…Basilakos et al (2004) found results consistent with ours (γ − 1 = 1.2 ± 0.3 and θ 0 = 48.9 +15.8 −24.5 arcsec) but with much larger error bars. Puccetti et al (2006) are also in agreement with us (θ 0 = 12.8 ± 7.8 arcsec) within their large uncertainties. For a canonical slope of 0.8, Yang et al (2003) found θ 0 = 40±11 arcsec, much larger than ours (θ 0 = 5.9±0.3 arcsec) with a significance of ∼4σ.…”

Section: Resultssupporting

confidence: 91%

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High-precision multi-band measurements of the angular clustering of X-ray sources

Ebrero¹,

Mateos²,

Stewart³

et al. 2009

A&A

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Aims. We aim to study the large-scale structure of an extragalactic serendipitous X-ray survey with unprecedented accuracy thanks to the large statistics involved, and provide insight into the environment of AGN at the epochs when their space density declines (z ∼ 1−2). Methods. In this paper we present the two-point angular correlation function of the X-ray source population of 1063 XMM-Newton observations at high Galactic latitudes, comprising up to ∼30 000 sources over a sky area of ∼125.5 deg 2 , in three energy bands: 0.5-2 (soft), 2-10 (hard), and 4.5-10 (ultrahard) keV. This is the largest survey of serendipitous X-ray sources ever used for clustering analysis. Results. We have measured the angular clustering of our survey and find significant positive clustering signals in the soft and hard bands (∼10σ and ∼5σ, respectively), and a marginal clustering detection in the ultrahard band (<1σ). We find dependency of the clustering strength on the flux limit and no significant differences in the clustering properties between sources with high hardness ratios (and therefore likely to be obscured AGN) and those with low hardness ratios. We deprojected the angular clustering parameters via Limber's equation to compute their typical spatial lengths. From that we have inferred that AGN at redshifts of ∼1 are embedded in dark matter haloes with typical masses of log M DMH 12.60 ± 0.34 h −1 M and lifetimes of t AGN = 3.1−4.5 × 10 8 yr. Conclusions. Our results show that obscured and unobscured objects share similar clustering properties and therefore they both reside in similar environments, in agreement with the unified model of AGN. The short AGN lifetimes derived suggest that AGN activity might be a transient phase that can be experienced several times by a large fraction of galaxies throughout their lives.

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Section: Resultssupporting

confidence: 91%

“…Summary of the fits in different flux-limited subsamples. (Yang et al 2003), COSMOS (Miyaji et al 2007), XMM-2dF (Basilakos et al 2004(Basilakos et al , 2005, ELAIS-S1 (Puccetti et al 2006), XMM-LSS (Gandhi et al 2006) and AXIS ). In Fig.…”

Section: Dependence On the Flux Limitmentioning

confidence: 99%

High-precision multi-band measurements of the angular clustering of X-ray sources

Ebrero¹,

Mateos²,

Stewart³

et al. 2009

A&A

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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

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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“…While XMM-Newton surveys cannot probe very faint fluxes as Chandra, they provide good quality spectroscopy in the whole 0.5−8 keV band for a large number of sources. The large effective area of XMM-Newton has been exploited in several surveys, including the Lockman Hole (with 1 Ms of exposure, Brunner et al 2008), the ELAIS-S1 field (Puccetti et al 2006), COSMOS , and 2XMM (Mateos et al 2008).…”

Section: Introductionmentioning

confidence: 99%

The XMM deep survey in the CDF-S

Ranalli¹,

Comastri²,

Vignali³

et al. 2013

A&A

Self Cite

128

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Nuclear obscuration plays a key role in the initial phases of AGN growth, yet not many highly obscured active galactic nuclei (AGN) are currently known beyond the local Universe, and their search is an active topic of research. The XMM-Newton survey in the Chandra Deep Field South (XMM-CDFS) aims at detecting and studying the spectral properties of a significant number of obscured and Compton-thick (N H > ∼ 10 24 cm −2 ) AGN. The large effective area of XMM-Newton in the 2-10 and 5-10 keV bands, coupled with a 3.45 Ms nominal exposure time (2.82 and 2.45 Ms after light curve cleaning for MOS and PN, respectively), allows us to build clean samples in both bands, and makes the XMM-CDFS the deepest XMM-Newton survey currently published in the 5-10 keV band. The large multi-wavelength and spectroscopic coverage of the CDFS area allows for an immediate and abundant scientific return. In this paper, we present the data reduction of the XMM-CDFS observations, the method for source detection in the 2-10 and 5-10 keV bands, and the resulting catalogues. A number of 339 and 137 sources are listed in the above bands with flux limits of 6.6 × 10 −16 and 9.5× 10 −16 erg s −1 cm −2 , respectively. The flux limits at 50% of the maximum sky coverage are 1.8× 10 −15 and 4.0× 10 −15 erg s −1 cm −2 , respectively. The catalogues have been cross-correlated with the Chandra ones: 315 and 130 identifications have been found with a likelihood-ratio method, respectively. A number of 15 new sources, previously undetected by Chandra, is found; 5 of them lie in the 4 Ms area. Redshifts, either spectroscopic or photometric, are available for ∼95% of the sources. The number counts in both bands are presented and compared to other works. The survey coverage has been calculated with the help of two extensive sets of simulations, one set per band. The simulations have been produced with a newly-developed simulator, written with the aim of the most careful reproduction of the background spatial properties. For this reason, we present a detailed decomposition of the XMM-Newton background into its components: cosmic, particle, and residual soft protons. The three components have different spatial distributions. The importance of these three components depends on the band and on the camera; the particle background is the most important one (80-90% of the background counts), followed by the soft protons (4-20%).

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The XMM-Newton survey of the ELAIS-S1 field

Cited by 73 publications

References 53 publications

High-precision multi-band measurements of the angular clustering of X-ray sources

High-precision multi-band measurements of the angular clustering of X-ray sources

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

The XMM deep survey in the CDF-S

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