A Front in a Puddle

Booth, David E.

doi:10.1002/j.1477-8696.1985.tb03744.x

Cited by 197 publications

(383 citation statements)

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“…Feedback from AGN has, for example, been invoked to explain the low SFRs of high-mass galaxies (e.g. Di Matteo, Springel & Hernquist 2005;Bower et al 2006;Croton et al 2006;Booth & Schaye 2009a) and the suppression of cooling flows in clusters of galaxies (e.g. Churazov et al 2001;Dalla Vecchia et al 2004;Ruszkowski, Brüggen & Begelman 2004;Cattaneo & Teyssier 2007).…”

Section: Agn Feedbackmentioning

confidence: 99%

“…White & Frenk 1991;Hernquist & Springel 2003;Bower et al 2006;Croton et al 2006;Somerville et al 2008;Fontanot et al 2009) or hydrodynamical simulations (e.g. Nagamine, Cen & Ostriker 2000;Pearce et al 2001;Ascasibar et al 2002;Murali et al 2002;Sommer-Larsen, Götz & Portinari 2003;Springel & Hernquist 2003b;Kereš et al 2005;Nagamine et al 2006;Di Matteo et al 2008;Oppenheimer & Davé 2008;Choi & Nagamine 2009;Crain et al 2009;Booth & Schaye 2009a) to study the SFH of the Universe.…”

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confidence: 99%

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The physics driving the cosmic star formation history

Schaye

Vecchia

Booth

et al. 2010

Monthly Notices of the Royal Astronomical Society

893

1,142

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We investigate the physics driving the cosmic star formation (SF) history using the more than fifty large, cosmological, hydrodynamical simulations that together comprise the OverWhelmingly Large Simulations (OWLS) project. We systematically vary the parameters of the model to determine which physical processes are dominant and which aspects of the model are robust. Generically, we find that SF is limited by the build-up of dark matter haloes at high redshift, reaches a broad maximum at intermediate redshift, then decreases as it is quenched by lower cooling rates in hotter and lower density gas, gas exhaustion, and self-regulated feedback from stars and black holes. The higher redshift SF is therefore mostly determined by the cosmological parameters and to a lesser extent by photo-heating from reionization. The location and height of the peak in the SF history, and the steepness of the decline towards the present, depend on the physics and implementation of stellar and black hole feedback. Mass loss from intermediate-mass stars and metal-line cooling both boost the SF rate at late times. Galaxies form stars in a self-regulated fashion at a rate controlled by the balance between, on the one hand, feedback from massive stars and black holes and, on the other hand, gas cooling and accretion. Paradoxically, the SF rate is highly insensitive to the assumed SF law. This can be understood in terms of self-regulation: if the SF efficiency is changed, then galaxies adjust their gas fractions so as to achieve the same rate of production of massive stars. Self-regulated feedback from accreting black holes is required to match the steep decline in the observed SF rate below redshift two, although more extreme feedback from SF, for example in the form of a top-heavy IMF at high gas pressures, can help.Comment: Accepted for publication in MNRAS, 27 pages and 18 figures. Revised version: minor change

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Section: Agn Feedbackmentioning

confidence: 99%

mentioning

confidence: 99%

The physics driving the cosmic star formation history

Schaye

Vecchia

Booth

et al. 2010

Monthly Notices of the Royal Astronomical Society

893

1,142

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“…If each SN-II releases 10 51 erg, the above choice of parameters corresponds to assuming that SNe-II power galactic outflows with nearly unity efficiency for a Salpeter IMF (see Springel & Hernquist 2003). Furthermore, we include in our simulations the effect of feedback energy released by gas accretion on to supermassive BHs, following the scheme originally introduced by SDH05 (see also Di Matteo et al 2005, 2008Booth & Schaye 2009). We refer to SDH05 for a more detailed description.…”

Section: Feedback Modelsmentioning

confidence: 99%

“…In this model, BHs are treated as sink particles which accrete from the surrounding gas according to a Bondi accretion rate (e.g. Bondi 1952), with an upper limit provided by the Eddington rate (see also Booth & Schaye 2009). This model was used by Bhattacharya, di Matteo & Kosowsky (2008), who run cosmological simulations to study the effect of AGN feedback on galaxy groups.…”

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confidence: 99%

Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters

Fabjan¹,

Borgani²,

Tornatore³

et al. 2010

Monthly Notices of the Royal Astronomical Society

253

311

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We present a study of the effect of active galactic nuclei (AGN) feedback on metal enrichment and thermal properties of the intracluster medium (ICM) in hydrodynamical simulations of galaxy clusters. The simulations are performed using a version of the TreePM–sphgadget‐2 code, which also follows chemodynamical evolution by accounting for metal enrichment contributed by different stellar populations. We carry out cosmological simulations for a set of galaxy clusters, covering the mass range M200≃ (0.1–2.2) × 1015 h−1 M⊙. Besides runs not including any efficient form of energy feedback, we carry out simulations including three different feedback schemes: (i) kinetic feedback in the form of galactic winds triggered by supernova explosions; (ii) AGN feedback from gas accretion on to supermassive black holes (BHs) and (iii) AGN feedback in which a ‘radio mode’ is included with an efficient thermal coupling of the extracted energy, whenever BHs enter in a quiescent accretion phase. Besides investigating the resulting thermal properties of the ICM, we analyse in detail the effect that these feedback models have on the ICM metal enrichment. We find that AGN feedback has the desired effect of quenching star formation in the brightest cluster galaxies at z < 4 and provides correct temperature profiles in the central regions of galaxy groups. However, its effect is not yet sufficient to create ‘cool cores’ in massive clusters while generating an excess of entropy in central regions of galaxy groups. As for the pattern of metal distribution, AGN feedback creates a widespread enrichment in the outskirts of clusters, thanks to its efficiency in displacing enriched gas from galactic haloes to the intergalactic medium. This turns into profiles of iron abundance, ZFe, which are in better agreement with observational results, and into a more pristine enrichment of the ICM around and beyond the cluster virial regions. Following the pattern of the relative abundances of silicon and iron, we conclude that a significant fraction of the ICM enrichment is contributed in simulations by a diffuse population of intracluster stars. Our simulations also predict that profiles of the ZSi/ZFe abundance ratio do not increase at increasing radii, at least out to 0.5Rvir. Our results clearly show that different sources of energy feedback leave distinct imprints in the enrichment pattern of the ICM. They further demonstrate that such imprints are more evident when looking at external regions, approaching the cluster virial boundaries.

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“…It is e.g. often assumed that a BH of mass M BH accretes mass from the surrounding interstellar medium (ISM) at a rate proportional to the Bondi rate (Bondi 1952): where ρ is the surrounding gas density, c s is the sound speed and f ∼ 10-100 takes into account the fact that the sphere of influence of the BH is not always resolved (Booth & Schaye 2009). Moreover, these same calculations assume that the BH's impact on its host galaxy can be approximated by depositing thermal energy released by accretion back into the surrounding gas.…”

Section: Introductionmentioning

confidence: 99%

Self-regulated black hole growth via momentum deposition in galaxy merger simulations

DeBuhr¹,

Quataert²,

Ma³

et al. 2010

Monthly Notices of the Royal Astronomical Society: Letters

116

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We perform hydrodynamical simulations of major galaxy mergers using new methods for calculating the growth of massive black holes (BH) in galactic nuclei and their impact on the surrounding galaxy. We model BH growth by including a subgrid model for accretion produced by angular momentum transport on unresolved scales. The impact of the BH's radiation on surrounding gas is approximated by depositing momentum into the ambient gas, which produces an outward force away from the BH. We argue that these phenomenological models for BH growth and feedback better approximate the interaction between the BH and dense gas in galaxies than previous models. We show that this physics leads to self‐regulated BH growth: during the peak of activity, the accretion rate on to the BH is largely determined by the physics of BH feedback, not the subgrid accretion model. The BH significantly modifies the gas dynamics in the galactic nucleus (≲300 pc), but does not generate large‐scale galactic outflows. Integrated over an entire galaxy merger, BH feedback has little effect on the total number of stars formed, but is crucial for setting the BH’s mass.

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A Front in a Puddle

Cited by 197 publications

References 0 publications

The physics driving the cosmic star formation history

The physics driving the cosmic star formation history

Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters

Self-regulated black hole growth via momentum deposition in galaxy merger simulations

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