Black hole -- galaxy scaling relations in FIRE: the importance of black hole location and mergers

Çatmabacak, Onur; Feldmann, Robert; Anglés-Alcázar, Daniel; Faucher-Giguère, Claude-André; Hopkins, Philip F.; Kereš, Dušan

doi:10.48550/arxiv.2007.12185

Cited by 7 publications

(8 citation statements)

References 122 publications

(172 reference statements)

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“…This transition has been identified in the FIRE simulations for massive (M > 10 10 M ) galaxies at different redshifts (Muratov et al 2015;Anglés-Alcázar et al 2017b,c;Faucher-Giguère 2018;Ma et al 2017a,b) and coincides with the virialization of the inner halo (Stern et al 2020). The early bursty epoch represents yet another qualitatively distinct regime for black hole growth, where sub-grid accretion calculations predict short (∼1 Myr) accretion episodes that can reach or even exceed the Eddington rate fol-lowed by longer periods of inactivity owing to stellar feedback continuously evacuating gas from galactic nuclei (Figure 9, middle panel; Anglés-Alcázar et al 2017c;Çatmabacak et al 2020;Byrne et al in prep.). These early conditions should be investigated in future hyper-refinement simulations.…”

Section: Diversity Of Accretion Phases On Cosmological Timescalesmentioning

confidence: 99%

Cosmological simulations of quasar fueling to sub-parsec scales using Lagrangian hyper-refinement

Anglés-Alcázar,

Quataert,

Hopkins

et al. 2020

Preprint

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We present cosmological hydrodynamic simulations of a quasar-mass halo (M halo ≈ 10 12.5 M at z = 2) that for the first time resolve gas transport down to the inner 0.1 pc surrounding the central massive black hole. We model a multi-phase interstellar medium including stellar feedback by supernovae, stellar winds, and radiation, and a hyper-Lagrangian refinement technique increasing the resolution dynamically approaching the black hole. We do not include black hole feedback. We show that the sub-pc inflow rate (1) can reach ∼6 M yr −1 roughly in steady state during the epoch of peak nuclear gas density (z ∼ 2), sufficient to power a luminous quasar, (2) is highly time variable in the pre-quasar phase, spanning 0.001-10 M yr −1 on Myr timescales, and (3) is limited to short (∼2 Myr) active phases (0.01-0.1 M yr −1 ) followed by longer periods of inactivity at lower nuclear gas density and late times (z ∼ 1), owing to the formation of a hot central cavity. Inflowing gas is primarily cool, rotational support dominates over turbulence and thermal pressure, and star formation can consume as much gas as provided by inflows across 1 pc-10 kpc. Gravitational torques from multi-scale stellar non-axisymmetries dominate angular momentum transport over gas self-torquing and pressure gradients, with accretion weakly dependent on black hole mass. Sub-pc inflow rates correlate with nuclear (but decouple from global) star formation and can exceed the Eddington rate by ×10. The black hole can move ∼10 pc from the galaxy center on ∼0.1 Myr. Accreting gas forms pc-scale, rotationally supported, obscuring structures often misaligned with the galaxy-scale disk. These simulations open a new avenue to investigate black hole-galaxy co-evolution.

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Section: Diversity Of Accretion Phases On Cosmological Timescalesmentioning

confidence: 99%

Cosmological simulations of quasar fueling to sub-parsec scales using Lagrangian hyper-refinement

Anglés-Alcázar,

Quataert,

Hopkins

et al. 2020

Preprint

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“…The last row shows the range of variation of each parameter; for the cosmological parameters the range of variation is Ωm ∈[0.1 -0.5], σ 8 ∈ [0.6 -1.0]. We emphasize that simulations with stellar feedback strongly suppresses black hole growth in lower mass galaxies (Anglés-Alcázar et al 2017c;C ¸atmabacak et al 2020). Black hole particles are repositioned to the location of the potential minimum within the FoF host group if it is found within a distance < 4×R 0 , where R 0 is the size of the black hole kernel enclosing the nearest 256 gas elements.…”

Section: Simbamentioning

confidence: 99%

The CAMELS project: Cosmology and Astrophysics with MachinE Learning Simulations

Villaescusa-Navarro,

Anglés-Alcázar,

Genel

et al. 2020

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We present the Cosmology and Astrophysics with MachinE Learning Simulations -CAMELSproject. CAMELS is a suite of 4,233 cosmological simulations of (25 h −1 Mpc) 3 volume each: 2,184 state-of-the-art (magneto-)hydrodynamic simulations run with the AREPO and GIZMO codes, employing the same baryonic subgrid physics as the IllustrisTNG and SIMBA simulations, and 2,049 N-body simulations. The goal of the CAMELS project is to provide theory predictions for different observables as a function of cosmology and astrophysics, and it is the largest suite of cosmological (magneto-)hydrodynamic simulations designed to train machine learning algorithms. CAMELS contains thousands of different cosmological and astrophysical models by way of varying Ω m , σ 8 , and four parameters controlling stellar and AGN feedback, following the evolution of more than 100 billion particles and fluid elements over a combined volume of (400 h −1 Mpc) 3 . We describe the simulations in detail and characterize the large range of conditions represented in terms of the matter power spectrum, cosmic star-formation rate density, galaxy stellar mass function, halo baryon fractions, and several galaxy scaling relations. We show that the IllustrisTNG and SIMBA suites produce roughly similar distributions of galaxy properties over the full parameter space but significantly different halo baryon fractions and baryonic effects on the matter power spectrum. This emphasizes the need for marginalizing over baryonic effects to extract the maximum amount of information from cosmological surveys. We illustrate the unique potential of CAMELS using several machine learning applications, including non-linear interpolation, parameter estimation, symbolic regression, data generation with Generative Adversarial Networks (GANs), dimensionality reduction, and anomaly detection.

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“…Intense UV radiation and energetic supernovae associated with massive star formation heat the interstellar medium and potentially induce mass loss from galactic disks (e.g., Hopkins et al 2011Hopkins et al , 2012Li et al 2015Li et al , 2017Kim & Ostriker 2018). Cosmological hydrodynamical simulations, which explore the coevolutionary process of galaxies and SMBHs, have shown that stellar feedback substantially regulates the mass budget in the nuclear regions and suppresses mass feeding to the central BHs (e.g., Dubois et al 2015;Habouzit et al 2017;Anglés-Alcázar et al 2017;Angles-Alcazar et al 2020;Çatmabacak et al 2020). Latif et al (2018) also demonstrated that the combination between stellar and AGN feedback prevents seed BHs from growing to M BH ∼ 10 9 M by z ∼ 6.…”

Section: Stellar Feedbackmentioning

confidence: 99%

Super-Eddington mass growth of intermediate-mass black holes embedded in dusty circumnuclear disks

Toyouchi,

Inayoshi,

Hosokawa

et al. 2020

Preprint

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We perform the first three-dimensional radiation hydrodynamical simulations that investigate the growth of intermediate-mass BHs (IMBHs) embedded in massive self-gravitating, dusty nuclear accretion disks. We explore the dependence of mass accretion efficiency on the gas metallicity Z and mass injection at super-Eddington accretion rates from the outer galactic disk Ṁin , and find that the central BH can be fed at rates exceeding the Eddington rate only when the dusty disk becomes sufficiently optically thick to ionizing radiation. In this case, mass outflows from the disk owing to photoevaporation is suppressed and thus a large fraction ( 40%) of the mass injection rate can feed the central BH. The conditions are expressed as Ṁin > 2.2 × 10 −1 M yr −1 (1 + Z/10 −2 Z ) −1 (c s /10 km s −1 ), where c s is the sound speed in the gaseous disk. With increasing numerical resolution, vigorous disk fragmentation reduces the disk surface density and dynamical heating by formed clumps makes the disk thickness higher. As a result, the photoevaorative mass-loss rate rises and thus the critical injection rate increases for fixed metallicity. This process enables super-Eddington growth of BHs until the BH mass reaches M BH ∼ 10 7−8 M , depending on the properties of the host dark-matter halo and metal-enrichment history. In the assembly of protogalaxies, seed BHs that form in overdense regions with a mass variance of 3-4σ at z ∼ 15 − 20 are able to undergo short periods of their rapid growth and transits into the Eddington-limited growth phase afterwards to be supermassive BHs observed at z > 6 − 7.

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Black hole -- galaxy scaling relations in FIRE: the importance of black hole location and mergers

Cited by 7 publications

References 122 publications

Cosmological simulations of quasar fueling to sub-parsec scales using Lagrangian hyper-refinement

Cosmological simulations of quasar fueling to sub-parsec scales using Lagrangian hyper-refinement

The CAMELS project: Cosmology and Astrophysics with MachinE Learning Simulations

Super-Eddington mass growth of intermediate-mass black holes embedded in dusty circumnuclear disks

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