Galaxy‐scale AGN feedback – theory

Wagner, Alexander Y.; Bicknell, G. V.; Umemura, Masayuki; Sutherland, Ralph S.; Silk, Joseph

doi:10.1002/asna.201512287

Cited by 62 publications

(64 citation statements)

References 68 publications

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“…However, it goes beyond the numerical prescription adopted to estimate the molecular gas available for star formation, as there is accumulating (theoretical and observational) evidence that supports AGN-triggered star formation (e.g. Silk 2013;Bieri et al 2015;Wagner et al 2016;Cresci & Maiolino 2018). This conclusion is expected not to hold in simulations of elliptical galaxies, galaxy groups and clusters, as the AGN feedback is expected and observed to be mainly negative in these systems.…”

Section: Bh-galaxy Coevolutionmentioning

confidence: 99%

Impact of AGN feedback on galaxies and their multiphase ISM across cosmic time

Valentini

Murante

Borgani

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present simulations of galaxy formation, based on the GADGET-3 code, in which a sub-resolution model for star formation and stellar feedback is interfaced with a new model for AGN feedback. Our sub-resolution model describes a multiphase ISM, accounting for hot and cold gas within the same resolution element: we exploit this feature to investigate the impact of coupling AGN feedback energy to the different phases of the ISM over cosmic time. Our fiducial model considers that AGN feedback energy coupling is driven by the covering factors of the hot and cold phases. We perform a suite of cosmological hydrodynamical simulations of disc galaxies (M halo, DM 2 · 10 12 M , at z = 0), to investigate: (i) the effect of different ways of coupling AGN feedback energy to the multiphase ISM; (ii) the impact of different prescriptions for gas accretion (i.e. only cold gas, both cold and hot gas, with the additional possibility of limiting gas accretion from cold gas with high angular momentum); (iii) how different models of gas accretion and coupling of AGN feedback energy affect the coevolution of supermassive BHs and their host galaxy. We find that at least a share of the AGN feedback energy has to couple with the diffuse gas, in order to avoid an excessive growth of the BH mass. When the BH only accretes cold gas, it experiences a growth that is faster than in the case in which both cold and hot gas are accreted. If the accretion of cold gas with high angular momentum is reduced, the BH mass growth is delayed, the BH mass at z = 0 is reduced by up to an order of magnitude, and the BH is prevented from accreting below z 2, when the galaxy disc forms.

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Section: Bh-galaxy Coevolutionmentioning

confidence: 99%

Impact of AGN feedback on galaxies and their multiphase ISM across cosmic time

Valentini

Murante

Borgani

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…There is a large body of literature on feedback processes during the epoch of galaxy formation, including feedback from stars, mainly through supernovae, and from AGN, by radiation and/or jets/outflows (e.g., Cattaneo et al 2009;Alexander & Hickox 2012;Fabian 2012;Kormendy & Ho 2013;Heckman & Best 2014;King & Pounds 2015; Tadhunter 2016 for reviews, and, e.g., Wagner et al 2016;Bongiorno et al 2016;Weinberger et al 2016 for recent papers on the AGN-JFM). In this section I review only the AGN-JFM, and concentrate only on processes that are related to other objects that are reviewed here, in particular to cooling flows in clusters of galaxies.…”

Section: Galaxy Formationmentioning

confidence: 99%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

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I review the influence jets and the bubbles they inflate might have on their ambient gas as they operate through a negative jet feedback mechanism (JFM). I discuss astrophysical systems where jets are observed to influence the ambient gas, in many cases by inflating large, hot, and low-density bubbles, and systems where the operation of the JFM is still a theoretical suggestion. The first group includes cooling flows in galaxies and clusters of galaxies, star-forming galaxies, young stellar objects, and bipolar planetary nebulae. The second group includes core collapse supernovae, the common envelope evolution, the grazing envelope evolution, and intermediate luminosity optical transients. The suggestion that the JFM operates in these four types of systems is based on the assumption that jets are much more common than what is inferred from objects where they are directly observed. Common to all eight types of systems reviewed here is the presence of a compact object inside an extended ambient gas. The ambient gas serves as a potential reservoir of mass to be accreted on to the compact object. If the compact object launches jets as it accretes mass, the jets might reduce the accretion rate as they deposit energy to the ambient gas, or even remove the entire ambient gas, hence closing a negative feedback cycle.

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“…However, the possibility that these effects produce positive feedback (i.e., triggering the star formation) has been suggested both by simulations (e.g., Mellema et al 2002;Gaibler et al 2012;Wagner et al 2016, and references therein) and by observations (van Breugel & Dey 1993;Dey et al 1997;Graham 1998;Mould et al 2000;Oosterloo & Morganti 2005;Croft et al 2006).…”

Section: Introductionmentioning

confidence: 99%

Embedded star formation in the extended narrow line region of Centaurus A: Extreme mixing observed by MUSE

Santoro

Oonk

Morganti

et al. 2016

A&A

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We present a detailed study of the complex ionization structure in a small (∼250 pc) extended narrow line region (ENLR) cloud near Centaurus A using the Multi Unit Spectroscopic Explorer. This cloud is located in the so-called outer filament of ionized gas (about 15 kpc from the nucleus) where jet-induced star formation has been suggested to occur by different studies. We find that, despite the small size, a mixture of ionization mechanisms is operating, resulting in considerable complexity in the spatial ionization structure.The area includes two H ii regions where star formation is occurring and another location where star formation must have ceased very recently. Interestingly, the extreme Balmer decrement of one of the star forming regions (Hα/Hβ obs ∼ 6) indicates that it is still heavily embedded in its natal cocoon of gas and dust. At all three locations a continuum counterpart is found with spectra matching those of O/B stars local to Centaurus A. The H ii regions are embedded in a larger gas complex which is photoionized by the radiation of the central active galactic nucleus (AGN), but the O/B stars affect the spatial ionization pattern in the ENLR cloud very locally. In particular, in the surroundings of the youngest star forming region, we can isolate a tight mixing sequence in the diagnostic diagram going from gas with ionization due to a pure stellar continuum to gas only photoionized by the AGN. These results emphasize the complexity and the mixture of processes occurring in star forming regions under the influence of an AGN radiation. This is relevant for our understanding of AGN-induced star formation suggested to occur in a number of objects, including this region of Centaurus A. They also illustrate that these young stars influence the gas over only a limited region.

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Galaxy‐scale AGN feedback – theory

Cited by 62 publications

References 68 publications

Impact of AGN feedback on galaxies and their multiphase ISM across cosmic time

Impact of AGN feedback on galaxies and their multiphase ISM across cosmic time

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Embedded star formation in the extended narrow line region of Centaurus A: Extreme mixing observed by MUSE

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