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

DeBuhr, Jackson; Quataert, Eliot; Ma, Chung‐Pei; Hopkins, Philip F.

doi:10.1111/j.1745-3933.2010.00881.x

Cited by 98 publications

(123 citation statements)

References 31 publications

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“…Several recent works have implemented momentum-driven winds in hydrodynamic simulations via radiation pressure on dust (Debuhr et al 2011(Debuhr et al , 2010) and via BLR winds (Choi et al 2014a(Choi et al , 2012 and found that these winds can play a significant role in modulating the growth of the black hole and the galaxy. The star formation remains quenched over a much longer timescale in the simulations that include momentum-feedback, because the density of hot gas near the center of the halos is significantly reduced (Choi et al 2014b).…”

Section: Agn Feedbackmentioning

confidence: 99%

Physical Models of Galaxy Formation in a Cosmological Framework

Somerville

Davé

2015

Annu. Rev. Astron. Astrophys.

1,343

1,111

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Modeling galaxy formation in a cosmological context presents one of the greatest challenges in astrophysics today, due to the vast range of scales and numerous physical processes involved. Here we review the current status of models that employ two leading techniques to simulate the physics of galaxy formation: semi-analytic models and numerical hydrodynamic simulations. We focus on a set of observational targets that describe the evolution of the global and structural properties of galaxies from roughly Cosmic High Noon (z ∼ 2-3) to the present. Although minor discrepancies remain, overall, models show remarkable convergence between different methods and make predictions that are in qualitative agreement with observations. Modelers seem to have converged on a core set of physical processes that are critical for shaping galaxy properties. This core set includes cosmological accretion, strong stellar-driven winds that are more efficient at low masses, black hole feedback that preferentially suppresses star formation at high masses, and structural and morphological evolution through merging and environmental processes. However, all cosmological models currently adopt phenomenological implementations of many of these core processes, which must be tuned to observations. Many details of how these diverse processes interact within a hierarchical structure formation setting remain poorly understood. Emerging multi-scale simulations are helping to bridge the gap between stellar and cosmological scales, placing models on a firmer, more physically grounded footing. Concurrently, upcoming telescope facilities will provide new challenges and constraints for models, particularly by directly constraining inflows and outflows through observations of gas in and around galaxies.

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Section: Agn Feedbackmentioning

confidence: 99%

Physical Models of Galaxy Formation in a Cosmological Framework

Somerville

Davé

2015

Annu. Rev. Astron. Astrophys.

1,343

1,111

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“…In general, the rateṀ accr of gas accretion onto the BH is possibly only a fraction of the rateṀ inj at which the gas is supplied from the reservoir toward the BH, i.e.,Ṁ accr = f accrṀinj due to possible outflows (Begelman 2012;Watarai 2006;Ohsuga 2007;Li 2012); the net effect is a kind of self-regulation (see Debuhr et al 2010Debuhr et al , 2011Debuhr et al , 2012. Depending on the local physical conditions, accretion and outflow rates, mass-to-radiation efficiencies and Eddington ratios are expected to fluctuate on very short time scales (e.g., Ohsuga 2007; Li 2012); we stress that in the model we refer to quantities averaged over the timescale needed by the BH to acquire its final mass.…”

Section: The Accretion Rate and The Effect Of Feedbackmentioning

confidence: 99%

The Coevolution of Supermassive Black Holes and Massive Galaxies at High Redshift

Lapi

Raimundo

Aversa

et al. 2014

ApJ

114

115

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We exploit the recent, wide samples of far-infrared (FIR) selected galaxies followed-up in X rays and of X-ray/optically selected active galactic nuclei (AGNs) followed-up in the FIR band, along with the classic data on AGN and stellar luminosity functions at high redshift z 1.5, to probe different stages in the coevolution of supermassive black holes (BHs) and host galaxies. The results of our analysis indicate the following scenario: (i) the star formation in the host galaxy proceeds within a heavily dust-enshrouded medium at an almost constant rate over a timescale 0.5 − 1 Gyr, and then abruptly declines due to quasar feedback; over the same timescale, (ii) part of the interstellar medium loses angular momentum, reaches the circum-nuclear regions at a rate proportional to the star formation and is temporarily stored into a massive reservoir/proto-torus wherefrom it can be promptly accreted; (iii) the BH grows by accretion in a self-regulated regime with radiative power that can slightly exceed the Eddington limit L/L Edd 4, particularly at the highest redshifts; (iv) for massive BHs the ensuing energy feedback at its maximum exceeds the stellar one and removes the interstellar gas, thus stopping the star formation and the fueling of the reservoir; (v) afterwards, if the latter has retained enough gas, a phase of supply-limited accretion follows exponentially declining with a timescale of about 2 e-folding times. We also discuss how the detailed properties and the specific evolution of the reservoir can be investigated via coordinated, high-resolution observations of starforming, strongly-lensed galaxies in the (sub-)mm band with ALMA and in the X-ray band with Chandra and the next generation X-ray instruments.

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“…While these measurements have been carried out for a select set of objects (e.g., Chartas et al 2007;Moe et al 2009;Dunn et al 2010;Borguet et al 2013;Chamberlain et al 2015), it is still unclear how these results generalize to AGNs as a whole. At the same time it is still an open question whether AGN outflows triggered by galaxy interactions actually quench star formation in massive, high-redshift galaxies (e.g., Fontanot et al 2009;Pipino et al 2009;Debuhr et al 2010;Ostriker et al 2010;FaucherGiguère & Quataert 2012;Newton & Kay 2013;Feldmann & Mayer 2015).…”

Section: Introductionmentioning

confidence: 99%

Constraining Agn Feedback in Massive Ellipticals With South Pole Telescope Measurements of the Thermal Sunyaev–zel’dovich Effect

Spacek

Scannapieco

Cohen

et al. 2016

ApJ

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Energetic feedback due to active galactic nuclei (AGNs) is likely to play an important role in the observed antihierarchical trend in the evolution of galaxies, and yet the energy injected into the circumgalactic medium by this process is largely unknown. One promising approach to constrain this feedback is through measurements of spectral distortions in the cosmic microwave background due to the thermal Sunyaev-Zeldovich (tSZ) effect, whose magnitude is directly proportional to the energy input by AGNs. With current instruments, making such measurements requires stacking large numbers of objects to increase signal-to-noise. While one possible target for such stacks is AGNs themselves, these are relatively scarce sources that contain contaminating emission that complicates tSZ measurements. Here we adopt an alternative approach and co-add South Pole Telescope SZ (SPT-SZ) survey data around a large set of massive quiescent elliptical galaxies at  z 0.5, which are much more numerous and less contaminated than active AGNs, yet are subject to the same feedback processes from the AGNs they hosted in the past. We use data from the Blanco Cosmology Survey and VISTA Hemisphere Survey to create a large catalog of galaxies split up into two redshift bins: one with 3394 galaxies at   z 0.5 1.0 and one with 924 galaxies at   z 1.0 1.5, with typical stellar masses of´ M 1.5 10 . 11We then co-add the emission around these galaxies, resulting in a measured tSZ signal at s 2.2 significance for the lower redshift bin and a contaminating signal at s 1.1 for the higher redshift bin. To remove contamination due to dust emission, we use SPT-SZ source counts to model a contaminant source population in both the SPT-SZ bands and Planck highfrequency bands for a subset of 937 galaxies in the low-redshift bin and 240 galaxies in the high-redshift bin. This increases our detection to s 3.6 for low redshifts and s 0.9 for high redshifts. We find the mean angularly integrated Compton-y values to be- 60 erg, respectively. These numbers are higher than expected from simple theoretical models that do not include AGN feedback, and serve as constraints that can be applied to current simulations of massive galaxy formation.

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

Cited by 98 publications

References 31 publications

Physical Models of Galaxy Formation in a Cosmological Framework

Physical Models of Galaxy Formation in a Cosmological Framework

The Coevolution of Supermassive Black Holes and Massive Galaxies at High Redshift

Constraining Agn Feedback in Massive Ellipticals With South Pole Telescope Measurements of the Thermal Sunyaev–zel’dovich Effect

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