The XMM deep survey in the CDF-S

Iwasawa, K.; Gilli, R.; Vignali, C.; Comastri, A.; Brandt, W. N.; Ranalli, P.; Vito, F.; Cappelluti, N.; Carrera, Francisco J.; Falocco, S.; Georgantopoulos, I.; Mainieri, V.; Paolillo, M.

doi:10.1051/0004-6361/201220036

Cited by 62 publications

(91 citation statements)

References 76 publications

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“…16 to be flat at z = 3−5 at F obsc ≈ 0.5. F obsc is usually found to increase with redshift up to z ≈ 2−2.5, and then saturates at higher redshifts (e.g., Treister & Urry 2006, Hasinger 2008, Iwasawa et al 2012, Buchner et al 2015, Liu et al 2017. We probe such behavior up to z ∼ 6.…”

Section: Obscured Agn Fraction Versus Redshiftmentioning

confidence: 99%

High-redshift AGN in the Chandra Deep Fields: the obscured fraction and space density of the sub-L* population

Vito

Brandt

Yang

et al. 2017

Monthly Notices of the Royal Astronomical Society

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164

184

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We investigate the population of high-redshift (3 z < 6) AGN selected in the two deepest X-ray surveys, the 7 Ms Chandra Deep Field-South and 2 Ms Chandra Deep Field-North. Their outstanding sensitivity and spectral characterization of faint sources allow us to focus on the sub-L * regime (logL X 44), poorly sampled by previous works using shallower data, and the obscured population. Taking fully into account the individual photometric-redshift probability distribution functions, the final sample consists of ≈ 102 X-ray selected AGN at 3 z < 6. The fraction of AGN obscured by column densities logN H > 23 is ∼ 0.6 − 0.8, once incompleteness effects are taken into account, with no strong dependence on redshift or luminosity. We derived the high-redshift AGN number counts down to F 0.5−2 keV = 7 × 10 −18 erg cm −2 s −1 , extending previous results to fainter fluxes, especially at z > 4. We put the tightest constraints to date on the low-luminosity end of AGN luminosity function at high redshift. The space-density, in particular, declines at z > 3 at all luminosities, with only a marginally steeper slope for low-luminosity AGN. By comparing the evolution of the AGN and galaxy densities, we suggest that such a decline at high luminosities is mainly driven by the underlying galaxy population, while at low luminosities there are hints of an intrinsic evolution of the parameters driving nuclear activity. Also, the black-hole accretion rate density and star-formation rate density, which are usually found to evolve similarly at z 3, appear to diverge at higher redshifts.

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Section: Obscured Agn Fraction Versus Redshiftmentioning

confidence: 99%

High-redshift AGN in the Chandra Deep Fields: the obscured fraction and space density of the sub-L* population

Vito

Brandt

Yang

et al. 2017

Monthly Notices of the Royal Astronomical Society

Self Cite

164

184

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“…To search for more redshifts and updates, we checked spectroscopic redshifts in recent works (Cooper et al 2011;Coppin et al 2012;Kurk et al 2013). Finally, in four cases, redshifts have been estimated by the clear presence of an iron emission line (Iwasawa et al 2012;Georgantopoulos et al 2013). …”

Section: Chandra and Optical Identification And Redshiftsmentioning

confidence: 99%

“…If the hardness of these sources is due to obscuration, then the non-detection by Chandra in the 0.5−2 keV band would also be justified. None of these sources was included in the Iwasawa et al (2012) paper because their PWXDetect significance is below the threshold set in that paper (except for source 407 which has however a low number of counts). Further study of these sources may help shed light on the obscured AGN population responsible for the missing fraction of the cosmic X-ray background, and will be presented in a further paper of this series (Ranalli et al, in prep.).…”

Section: New Sourcesmentioning

confidence: 99%

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The XMM deep survey in the CDF-S

Ranalli¹,

Comastri²,

Vignali³

et al. 2013

A&A

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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 emission line is interpreted as neutral iron Kα emission, and the absorption line is most likely due to a blueshifted highly ionized iron transition associated with outflowing gas with a velocity of ∼0.1c. The spectral "peculiarity" of this source came out in the search for obscured AGN at high redshift selected in the XMM-Newton observations of the Chandra Deep Field-South (XMM-CDFS) by means of restframe X-ray colors (Iwasawa et al 2012). This source is listed as number 352 in the 3 Ms XMM-Newton 2−10 keV source catalog by Ranalli et al (2013); hereafter, we refer to this source as PID352.…”

Section: Introductionmentioning

confidence: 99%

The XMM deep survey in the CDF-S

Vignali

Iwasawa

Comastri

et al. 2015

A&A

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In active galactic nuclei (AGN)-galaxy co-evolution models, AGN winds and outflows are often invoked to explain why super-massive black holes and galaxies stop growing efficiently at a certain phase of their lives. They are commonly referred to as the leading actors of feedback processes. Evidence of ultra-fast (v > ∼ 0.05c) outflows in the innermost regions of AGN has been collected in the past decade by sensitive X-ray observations for sizable samples of AGN, mostly at low redshift. Here we present ultra-deep XMM-Newton and Chandra spectral data of an obscured (N H ≈ 2 × 10 23 cm −2 ), intrinsically luminous (L 2−10 keV ≈ 4 × 10 44 erg s −1 ) quasar (named PID352) at z ≈ 1.6 (derived from the X-ray spectral analysis) in the Chandra Deep Field-South. The source is characterized by an iron emission and absorption line complex at observed energies of E ≈ 2−3 keV. While the emission line is interpreted as being due to neutral iron (consistent with the presence of cold absorption), the absorption feature is due to highly ionized iron transitions (FeXXV, FeXXVI) with an outflowing velocity of 0.14 +0.02 −0.06 c, as derived from photoionization models. The mass outflow rate -∼2 M yr −1 -is similar to the source accretion rate, and the derived mechanical energy rate is ∼9.5 × 10 44 erg s −1 , corresponding to 9% of the source bolometric luminosity. PID352 represents one of the few cases where indications of X-ray outflowing gas have been observed at high redshift thus far. This wind is powerful enough to provide feedback on the host galaxy.

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The XMM deep survey in the CDF-S

Cited by 62 publications

References 76 publications

High-redshift AGN in the Chandra Deep Fields: the obscured fraction and space density of the sub-L* population

High-redshift AGN in the Chandra Deep Fields: the obscured fraction and space density of the sub-L* population

The XMM deep survey in the CDF-S

The XMM deep survey in the CDF-S

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