X-Ray Properties of AGN in Brightest Cluster Galaxies. I. A Systematic Study of the Chandra Archive in the 0.2 &lt; z &lt; 0.3 and 0.55 &lt; z &lt; 0.75 Redshift Range

Yang, Lilan; Tozzi, P.; Yu, Heng; Lusso, Elisabeta; Gaspari, M.; Gilli, R.; Nardini, E.; Risaliti, G.

doi:10.3847/1538-4357/aabfd7

Cited by 21 publications

(15 citation statements)

References 107 publications

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“…1, right panel). The SED fit indicates the BCG is hosting an obscured Type 2 AGN (as also pointed out by the analysis of Chandra data by Yang et al 2018) whose emission does not contribute to the galaxy overall optical emission. The CIGALE analysis allows us to estimate the BCG star formation activity equal to ‡ ∼14.5 M /yr, thus locating the galaxy firmly along the main-sequence of galaxies as defined by Speagle et al 2014.…”

Section: Data Analysis and Resultssupporting

confidence: 61%

A MUSE inquiry into the physical processes taking place within the Abell 2667 Brightest Cluster Galaxy

Iani

Rodighiero

Fritz³

et al. 2019

Proc. IAU

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Brightest cluster galaxies (BCGs) residing in cool-core clusters are known to be the stage of intricate baryon cycle phenomena (e.g. gas inflows, AGN outflows, star formation feedback). The scenarios describing the observed properties of these galaxies are still controversial, suffering from limitations due to the spatial resolving power of the instruments, specifically for galaxies beyond the Local Universe. However, the dramatic improvements introduced by the integral-field unit instruments (e.g. MUSE) could shed light on the physical processes driving the evolution of these galaxies. We present an extensive analysis of the stellar and gas properties (i.e. kinematics, stellar mass, star formation rate) of the radio-loud BCG sitting at the centre of the X-ray luminous cool-core cluster Abell 2667 (z = 0.23), based on MUSE data. Our results indicate that the BCG is a massive elliptical, hosting an AGN that is possibly undergoing accretion of cold star-forming clouds of ICM or galactic cannibalism.

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Section: Data Analysis and Resultssupporting

confidence: 61%

A MUSE inquiry into the physical processes taking place within the Abell 2667 Brightest Cluster Galaxy

Iani

Rodighiero

Fritz³

et al. 2019

Proc. IAU

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“…This prediction is broadly consistent with direct measurements by Ehlert et al (2014), who find that 2.9 -4.6% of Brightest Cluster Galaxies (BCGs), assumed to be the central galaxies of high mass parent haloes, are found to host an X-ray bright AGN. In contrast, Yang et al (2018) find that ∼18% of BCGs host an X-ray luminous AGN ( X > 10 42 erg s −1 ) within a sample of virialised clusters and Noordeh et al (2020) find 1 out of 7 of the BCGs in their sample has an X-ray luminous AGN, ostensibly higher than our estimate, although these studies are subject to small number statistics and there may be additional selection effects in the construction of high-mass cluster samples that are not incorporated into our model predictions.…”

Section: Hod Modelling and The Agn Satellite Fractionmentioning

confidence: 90%

The AGN–galaxy–halo connection: the distribution of AGN host halo masses to z = 2.5

Aird

Coil²

2021

Monthly Notices of the Royal Astronomical Society

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It is widely reported, based on clustering measurements of observed active galactic nuclei (AGN) samples, that AGN reside in similar mass host dark matter halos across the bulk of cosmic time, with log $\mathcal {M}/\mathcal {M}_{\odot }\sim 12.5-13.0$ to z ∼ 2.5. We show that this is due in part to the AGN fraction in galaxies rising with increasing stellar mass, combined with AGN observational selection effects that exacerbate this trend. Here, we use AGN specific accretion rate distribution functions determined as a function of stellar mass and redshift for star-forming and quiescent galaxies separately, combined with the latest galaxy-halo connection models, to determine the parent and sub-halo mass distribution function of AGN to various observational limits. We find that while the median (sub-)halo mass of AGN, $\approx 10^{12}\mathcal {M}_{\odot }$, is fairly constant with luminosity, specific accretion rate, and redshift, the full halo mass distribution function is broad, spanning several orders of magnitude. We show that widely used methods to infer a typical dark matter halo mass based on an observed AGN clustering amplitude can result in biased, systematically high host halo masses. While the AGN satellite fraction rises with increasing parent halo mass, we find that the central galaxy is often not an AGN. Our results elucidate the physical causes for the apparent uniformity of AGN host halos across cosmic time and underscore the importance of accounting for AGN selection biases when interpreting observational AGN clustering results. We further show that AGN clustering is most easily interpreted in terms of the relative bias to galaxy samples, not from absolute bias measurements alone.

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“…The process by which cold clumps carry the accretion flow onto the central SMBH (rather than Bondi-type accretion of the hot gas) is the cold feedback mechanism (Pizzolato & Soker 2005, 2010Gaspari et al 2013;Gaspari, Brighenti, & Temi 2015;; note that some studies use other terms for this mechanism, like chaotic cold accretion, e.g., McKinley et al 2021). There are many papers in recent years that support the cold feedback mechanism (e.g., a small sample of recent papers, Babyk et al 2018;Gaspari et al 2018;Ji et al 2018;Prasad et al 2018;Pulido et al 2018;Voit 2018a;Yang et al 2018;Choudhury et al 2019;Iani et al 2019;Rose et al 2019;Russell et al 2019;Stern et al 2019;Storchi-Bergmann, & Schnorr-Müller 2019;Vantyghem et al 2019;Voit 2019;Hardcastle & Croston 2020;Martz et al 2020;Prasad et al 2020;Eckert et al 2021;Maccagni et al 2021;Pasini et al 2021;Qiu et al 2021;Singh, Voit, & Nath 2021).…”

Section: Introductionmentioning

confidence: 99%

Jittering jets by negative angular momentum feedback in cooling flows

Soker¹

2021

Preprint

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I apply the jittering jets in cooling flow scenario to explain the perpendicular to each other and almost coeval two pairs of bubbles in the cooling flow galaxy cluster RBS 797, and conclude that the interaction of the jets with the cold dense clumps that feed the supermassive black hole (SMBH) takes place in the zone where the gravitational influence of the SMBH and that of the cluster are about equal. According to the jittering jets in cooling flow scenario jets uplift and entrain cold and dense clumps, impart the clumps velocity perpendicular to the original jets' direction, and 'drop' them closer to the jets' axis. The angular momentum of these clumps is at a very high angle to the original jets' axis. When these clumps feed the SMBH in the next outburst the new jets' axis is at a high angle to the axis of the first pair of jets. I apply this scenario to recent observations that show the two perpendicular pairs of bubbles in RBS 797 to have a small age difference of < 10 Myr, and conclude that the jets-clumps interaction takes place in a distance of about ≈ 10 − 100 pc from the SMBH. Interestingly, in this zone the escape velocity from the SMBH is about equal to the sound speed of the intracluster medium (ICM). I discuss the implications of this finding.

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X-Ray Properties of AGN in Brightest Cluster Galaxies. I. A Systematic Study of the Chandra Archive in the 0.2 < z < 0.3 and 0.55 < z < 0.75 Redshift Range

Cited by 21 publications

References 107 publications

A MUSE inquiry into the physical processes taking place within the Abell 2667 Brightest Cluster Galaxy

A MUSE inquiry into the physical processes taking place within the Abell 2667 Brightest Cluster Galaxy

The AGN–galaxy–halo connection: the distribution of AGN host halo masses to z = 2.5

Jittering jets by negative angular momentum feedback in cooling flows

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