The XXL Survey

Plionis, M.; Koutoulidis, L.; Koulouridis, E.; Moscardini, L.; Lidman, C.; Pierre, M.; Adami, C.; Chiappetti, L.; Faccioli, L.; Fotopoulou, S.; Pacaud, F.; Paltani, S.

doi:10.1051/0004-6361/201832970

Cited by 11 publications

(9 citation statements)

References 64 publications

(64 reference statements)

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“…In fact, this observation has been already recognised in the X-ray community (e.g. Leauthaud et al 2015;Mendez et al 2016;Powell et al 2018;Plionis et al 2018;Krishnan et al 2020). All these studies find no significant differences in the clustering properties of X-ray AGN compared to a matched galaxy sample.…”

Section: Qsos and The Dark Matter Halo Mass Functionsupporting

confidence: 57%

Quasars at intermediate redshift are not special; but they are often satellites

Alam

Ross

Eftekharzadeh

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Understanding the links between the activity of supermassive black holes (SMBH) at the centres of galaxies and their host dark matter haloes is a key question in modern astrophysics. The final data release of the SDSS-IV eBOSS provides the largest contemporary spectroscopic sample of galaxies and QSOs. Using this sample and covering the redshift interval z = 0.7 − 1.1, we have measured the clustering properties of the eBOSS QSOs, Emission Line Galaxies (ELGs) and Luminous Red Galaxies (LRGs). We have also measured the fraction of QSOs as a function of the overdensity defined by the galaxy population. Using these measurements, we investigate how QSOs populate and sample the galaxy population, and how the host dark-matter haloes of QSOs sample the underlying halo distribution. We find that the probability of a galaxy hosting a QSO is independent of the host dark matter halo mass of the galaxy. We also find that about 60% of eBOSS QSOs are hosted by LRGs and about 20-40% of QSOs are hosted by satellite galaxies. We find a slight preference for QSOs to populate satellite galaxies over central galaxies. This is connected to the host halo mass distribution of different types of galaxies. Based on our analysis, QSOs should be hosted by a very broad distribution of haloes, and their occurrence should be modulated only by the efficiency of galaxy formation processes.

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Section: Qsos and The Dark Matter Halo Mass Functionsupporting

confidence: 57%

Quasars at intermediate redshift are not special; but they are often satellites

Alam

Ross

Eftekharzadeh

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Nevertheless, another interesting part of the general agreement is the fact that an optical host-galaxy magnitude limited AGN sample agrees quite well with the underline X-ray AGN sample, represented by the simulation data. In a forthcoming paper (Plionis et al 2018), which studies the AGN clustering in much greater detail, we perform a thorough and consistent comparison of the simulations and the XXL pointsource redshift data.…”

Section: Summary and Discussionmentioning

confidence: 99%

The XXL Survey

Koulouridis

Faccioli

Brun

et al. 2018

A&A

Self Cite

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Modern cosmological simulations heavily rely on feedback from active galactic nuclei (AGN) in order to stave off overcooling in massive galaxies, and galaxy groups and clusters. Given that AGN are a key component of such simulations, an important independent test is whether or not the simulations capture the broad demographics of the observed AGN population. However, to date, comparisons between observed and simulated AGN populations have been relatively limited. Here, we have used the cosmo-OWLS suite of cosmological hydrodynamical simulations to produce realistic synthetic catalogs of X-ray AGN out to z = 3, with the aim of comparing the catalogs to the observed X-ray AGN population in the XXL survey and other recent surveys. We focused on the unabsorbed X-ray luminosity function (XLF), the Eddington ratio distribution, the black hole mass function, and the projected clustering of X-ray AGN. To compute the unabsorbed XLF of the simulated AGN, we used recent empirically-determined (luminosity-dependent) bolometric corrections, in order to convert the simulated bolometric luminosity into an observable X-ray luminosity. We show that, using these corrections, the simulated AGN sample accurately reproduces the observed XLF over 3 orders of magnitude in X-ray luminosity in all redshift bins from z = 0 out to z = 3. To compare to the observed Eddington ratio distribution and the clustering of AGN, we produced detailed “XMM-Newton-detected” catalogs of the simulated AGN. This requires the production of synthetic X-ray images extracted from light cones of the simulations, which self-consistently contain both the X-ray AGN and the emission from diffuse, hot gas within galaxies, galaxy groups, and clusters and that fold in the relevant instrumental effects of XMM-Newton. We apply a luminosity- and redshift-dependent obscuration function for the AGN and employ the same AGN detection algorithm as used for the real XXL survey. We demonstrate that the detected population of simulated AGN reproduces the observed Eddington ratio distribution and projected clustering from XXL quite well. Based on these comparisons, we conclude that the simulations have a broadly realistic population of AGN and that our synthetic X-ray AGN catalogs should be useful for interpreting additional trends (e.g. environmental dependencies) and as a helpful tool for quantifying AGN contamination in galaxy group and cluster X-ray surveys.

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“…Clustering measurements of different types of AGN have been carried out by several groups exploiting data from multiple surveys in diverse wavebands. Different typical hosting halo masses are found in studies at different bands, ranging from ∼10 12 solar mass for optically selected quasars (e.g., Croom et al 2005, Porciani & Norberg 2006, Shen et al 2013Ross et al 2009) to dense environment typical of galaxy groups for X-ray selected AGN (Hickox et al 2009;Cappelluti et al 2010;Krumpe et al 2010;Mountrichas et al 2013;Koutoulidis et al 2013, Plionis et al 2018). However, this difference in the typical halo mass of X-ray compared to optically selected AGN may not be present at low redshift (e.g.…”

Section: Introductionmentioning

confidence: 99%

ChandraCOSMOS Legacy Survey: Clustering dependence of Type 2 active galactic nuclei on host galaxy properties

Allevato

Viitanen

Finoguenov

et al. 2019

A&A

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Aims. We perform clustering measurements of 800 X-ray selected Chandra COSMOS Legacy (CCL) Type 2 AGN with known spectroscopic redshift to probe the halo mass dependence on AGN host galaxy properties, such as galaxy stellar mass M star , star formation rate (SFR) and specific black hole accretion rate λ BHAR , in the redshift range z = [0 -3]. Methods. We split the sample of AGN with known spectroscopic redshits according to M star , SFR and λ BHAR , while matching the distributions in terms of the other parameters, including redshift. We measure the projected two-point correlation function w p (r p ) and model it with the 2-halo term to derive the large-scale bias b and the corresponding typical mass of the hosting halo, for the different subsamples.Results. We found no significant dependence of the large-scale bias and typical halo mass on galaxy stellar mass and specific BHAR for CCL Type 2 AGN at mean z∼1, while a negative dependence on SFR is observed, with lower SFR AGN residing in richer environment. Mock catalogs of AGN matched to have the same X-ray luminosity, stellar mass, λ BHAR and SFR of CCL Type 2 AGN, almost reproduce the observed M star − M h , λ BHAR − M h and SFR-M h relations, when assuming a fraction of satellite AGN f sat AGN ∼ 0.15, which corresponds to a ratio between the probabilities of satellite and central AGN of being active Q ∼ 2. Mock matched normal galaxies follow a slightly steeper M star − M h relation -with low mass mock galaxies residing in less massive halos than mock AGN of similar mass, and are less biased than mock AGN with similar specific BHAR and SFR, at least for Q > 1.

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The XXL Survey

Cited by 11 publications

References 64 publications

Quasars at intermediate redshift are not special; but they are often satellites

Quasars at intermediate redshift are not special; but they are often satellites

The XXL Survey

ChandraCOSMOS Legacy Survey: Clustering dependence of Type 2 active galactic nuclei on host galaxy properties

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