Tracing black hole and galaxy co-evolution in the Romulus simulations

Ricarte, Angelo; Tremmel, Michael; Natarajan, Priyamvada; Quinn, Thomas

doi:10.1093/mnras/stz2161

Cited by 54 publications

(48 citation statements)

References 132 publications

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“…Reproducing such high inflow rates from galactic scales down to the black hole accretion disk represents a significant challenge for models. Cold flows, major mergers, minor mergers, and secular processes are generically identified as AGN triggering mechanisms in cosmological and galaxy-scale simulations (e.g., Springel et al 2005;Li et al 2007;Bournaud et al 2011;Di Matteo et al 2012;Bellovary et al 2013;Anglés-Alcázar et al 2015;Pontzen et al 2017;Steinborn et al 2018;Ricarte et al 2019), but predicted inflow rates have been often limited by either resolution, subgrid ISM physics, idealized initial conditions, or uncertainties in black hole accretion parameterization. For the first time in a full cosmological context, we have shown that gas inflow rates of up to ∼10 M e yr −1 can indeed occur at subpc scales in a host halo with M vir ∼ 10 12.5 M e at z ∼ 2, sufficient to power a luminous QSO.…”

Section: Reproducing Luminous Qso Inflowsmentioning

confidence: 99%

“…Observations also appear inconclusive regarding the relative roles of galaxy mergers (e.g., Treister et al 2012;Hopkins et al 2014b;Kocevski et al 2015;Wylezalek et al 2016;Ricci et al 2017;Díaz-Santos et al 2018;Donley et al 2018) and secular processes (e.g., Kocevski et al 2012;Simmons et al 2012;Mechtley et al 2016;Villforth et al 2017;Smethurst et al 2019) driving black hole growth, with idealized and cosmological simulations sometimes producing contrasting results (e.g., Springel et al 2005;Li et al 2007;Bournaud et al 2011;Di Matteo et al 2012;Anglés-Alcázar et al 2015;Pontzen et al 2017;Steinborn et al 2018;Ricarte et al 2019;Sharma et al 2021). A massive satellite galaxy (M å ∼ 10 10 M e ) is approaching the central galaxy in its second passage toward finale coalescence at the time of the pre-QSO and full-QSO phases, located ∼20 kpc and ∼15 kpc away, respectively.…”

Section: Multiscale Torques and Agn Triggeringmentioning

confidence: 99%

“…Other studies suggest little or no connection between average SFR and black hole accretion (Harrison et al 2012;Mullaney et al 2012a;Stanley et al 2015) or link luminous AGN activity with a suppression of star formation (Page et al 2012), possibly only for galaxies above the star formation main sequence (Masoura et al 2018). Part of the discrepancy may originate from biases and selection effects (e.g., Trump et al 2015), but different characteristic timescales for star formation and AGN activity are likely crucial as well (Hickox et al 2014;Anglés-Alcázar et al 2015;Volonteri et al 2015;Ricarte et al 2019;Thomas et al 2019).…”

Section: The Sfr-agn Connectionmentioning

confidence: 99%

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Cosmological Simulations of Quasar Fueling to Subparsec Scales Using Lagrangian Hyper-refinement

Anglés-Alcázar

Quataert

Hopkins

et al. 2021

ApJ

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We present cosmological hydrodynamic simulations of a quasar-mass halo (M halo ≈ 10 12.5 M e 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 multiphase 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 subpc inflow rate (1) can reach ∼6 M e 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 e yr −1 on Myr timescales, and (3) is limited to short (∼2 Myr) active phases (0.01-0.1 M e 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 multiscale stellar non-axisymmetries dominate angular momentum transport over gas self-torquing and pressure gradients, with accretion weakly dependent on black hole mass. Subpc 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 coevolution.

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Section: Reproducing Luminous Qso Inflowsmentioning

confidence: 99%

Section: Multiscale Torques and Agn Triggeringmentioning

confidence: 99%

Section: The Sfr-agn Connectionmentioning

confidence: 99%

See 1 more Smart Citation

Cosmological Simulations of Quasar Fueling to Subparsec Scales Using Lagrangian Hyper-refinement

Anglés-Alcázar

Quataert

Hopkins

et al. 2021

ApJ

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“…Models of structure formation can reproduce the observed large-scale properties of quasars (e.g., their environment and clustering clustering) if their bright and short-lived active phases are most likely triggered by mergers (see Kauffmann and Haehnelt 2000;Alexander and Hickox 2012 and references therein). However, not all nuclear activity is triggered by galaxy collisions as SMBH growth can occur also through secular processes (Martin et al, 2018;Ricarte et al, 2019) with mergers triggering an initial rapid growth phase (McAlpine et al, 2018). In the last decade, quasar pairs at sub-Mpc (projected) separations have raised interest as these systems could possibly trace regions of systematic large-scale overdensities of galaxies (e.g., Hennawi et al 2006Hennawi et al , 2010Sandrinelli et al 2014;Eftekharzadeh et al 2017;Sandrinelli et al 2018b;Lusso et al 2018).…”

Section: Introductionmentioning

confidence: 99%

The quest for dual and binary supermassive black holes: A multi-messenger view

Rosa

Vignali

Bogdanović

et al. 2019

New Astronomy Reviews

203

123

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The quest for binary and dual supermassive black holes (SMBHs) at the dawn of the multi-messenger era is compelling. Detecting dual active galactic nuclei (AGN)-active SMBHs at projected separations larger than several parsecs-and binary AGN-probing the scale where SMBHs are bound in a Keplerian binary-is an observational challenge. The study of AGN pairs (either dual or binary) also represents an overarching theoretical problem in cosmology and astrophysics. The AGN triggering calls for detailed knowledge of the hydrodynamical conditions of gas in the imminent surroundings of the SMBHs and, at the same time, their duality calls for detailed knowledge on how galaxies assemble through major and minor mergers and grow fed by matter along the filaments of the cosmic web. This review describes the techniques used across the electromagnetic spectrum to detect dual and binary AGN candidates and proposes new avenues for their search. The current observational status is compared with the state-of-the-art numerical simulations and models for formation of dual and binary AGN. Binary SMBHs are among the loudest sources of gravitational waves (GWs) in the Universe. The search for a background of GWs at nHz frequencies from inspiralling SMBHs at low redshifts, and the direct detection of signals from their coalescence by the Laser Interferometer Space Antenna in the next decade, make this a theme of major interest for multi-messenger astrophysics. This review discusses the future facilities and observational strategies that are likely to significantly advance this fascinating field.

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“…Mullaney et al 2012) and simulations (e.g. Ricarte et al 2019;Thomas et al 2019) also exhibit no strong redshift evolution of the relation between star formation rate and BH accretion rate, and treat this as evidence for or a consequence of BH-galaxy coevolution.…”

Section: Bh Mass Density and Accretion Rate Densitymentioning

confidence: 99%

The ASTRID simulation: the evolution of Supermassive Black Holes

Ni,

Di Matteo,

Bird

et al. 2021

Preprint

Self Cite

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We present the evolution of black holes (BHs) and their relationship with their host galaxies in Astrid , a large-volume cosmological hydrodynamical simulation with box size 250 ℎ −1 Mpc containing 2 × 5500 3 particles evolved to 𝑧 = 3. Astrid statistically models BH gas accretion and AGN feedback to their environments, applies a power-law distribution for BH seed mass 𝑀 sd , uses a dynamical friction model for BH dynamics and executes a physical treatment of BH mergers. The BH population is broadly consistent with empirical constraints on the BH mass function, the bright end of the luminosity functions, and the time evolution of BH mass and accretion rate density. The BH mass and accretion exhibit a tight correlation with host stellar mass and star formation rate. We trace BHs seeded before 𝑧 > 10 down to 𝑧 = 3, finding that BHs carry virtually no imprint of the initial 𝑀 sd except those with the smallest 𝑀 sd , where less than 50% of them have doubled in mass. Gas accretion is the dominant channel for BH growth compared to BH mergers. With dynamical friction, Astrid predicts a significant delay for BH mergers after the first encounter of a BH pair, with a typical elapse time of about 200 Myrs. There are in total 4.5 × 10 5 BH mergers in Astrid at 𝑧 > 3, ∼ 10 3 of which have X-ray detectable EM counterparts: a bright kpc scale dual AGN with 𝐿 X > 10 43 erg s −1 . BHs with 𝑀 BH ∼ 10 7−8 𝑀 experience the most frequent mergers. Galaxies that host BH mergers are unbiased tracers of the overall 𝑀 BH − 𝑀 * relation. Massive (> 10 11 𝑀 ) galaxies have a high occupation number ( 10) of BHs, and hence host the majority of BH mergers.

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Tracing black hole and galaxy co-evolution in the Romulus simulations

Cited by 54 publications

References 132 publications

Cosmological Simulations of Quasar Fueling to Subparsec Scales Using Lagrangian Hyper-refinement

Cosmological Simulations of Quasar Fueling to Subparsec Scales Using Lagrangian Hyper-refinement

The quest for dual and binary supermassive black holes: A multi-messenger view

The ASTRID simulation: the evolution of Supermassive Black Holes

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