The <i>XMM-Newton</i> serendipitous survey

Ebrero, J.; Carrera, Francisco J.; Page, M. J.; Silverman, J. D.; Barcons, X.; Ceballos, M. T.; Corral, A.; Ceca, R. Della; Watson, M. G.

doi:10.1051/0004-6361:200810919

Cited by 125 publications

(232 citation statements)

References 68 publications

(146 reference statements)

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“…Our approach differs from most prior studies of the evolution of the XLF, which instead attempt to find a model that directly describes the total XLF, either using an LDDE parametrization or some form of luminosity and density evolution (e.g. Ebrero et al 2009;Yencho et al 2009;Aird et al 2010). …”

Section: Comparison With Previous Studies Of the X-ray Luminosity Funmentioning

confidence: 99%

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

357

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: Comparison With Previous Studies Of the X-ray Luminosity Funmentioning

confidence: 99%

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

357

559

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“…4.4). The median redshifts and luminosities have been derived from the LDDE best-fit luminosity function of Ebrero et al (2009). In Fig.…”

Section: Dependence On the X-ray Luminosity And Redshiftmentioning

confidence: 99%

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

Ebrero¹,

Mateos²,

Stewart³

et al. 2009

A&A

Self Cite

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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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“…From X-ray studies, it is now well established that a LDDE model provides a more accurate description of the evolutionary properties of AGN (Hasinger et al 2005;Ueda et al 2003;La Franca et al 2005;Silverman et al 2008;Ebrero et al 2009), and this is the case also in the optical domain for at least type-1 AGN (Bongiorno et al 2007, hereafter B07). We can describe the LF as a function of redshift with where…”

Section: Model Fittingmentioning

confidence: 99%

The [O iii] emission line luminosity function of optically selected type-2 AGN from zCOSMOS$^{\rm,}$

Bongiorno

Mignoli

Zamorani

et al. 2010

A&A

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Aims. We present a catalog of 213 type-2 AGN selected from the zCOSMOS survey. The selected sample covers a wide redshift range (0.15 < z < 0.92) and is deeper than any other previous study, encompassing the luminosity range 10 5.5 L < L [OIII] < 10 9.1 L . We explore the intrinsic properties of these AGN and the relation to their X-ray emission (derived from the XMM-COSMOS observations). We study their evolution Results. Combining our sample with one drawn from SDSS, we found that the best description of the evolution of type-2 AGN is a luminositydependent density evolution model. Moreover, using the type-1 AGN LF we were able to constrain the fraction of type-2 AGN to the total (type-1 + type-2) AGN population. We found that the type-2 fraction decreases with luminosity, in agreement with the most recent results, and shows signs of a slight increase with redshift. However, the trend with luminosity is visible only after combining the SDSS+zCOSMOS samples. From the COSMOS data points alone, the type-2 fraction seems to be quite constant with luminosity.

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The XMM-Newton serendipitous survey

Cited by 125 publications

References 68 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

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

The [O iii] emission line luminosity function of optically selected type-2 AGN from zCOSMOS$^{\rm,}$

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