The ASTRID simulation: the evolution of supermassive black holes

Ni, Yueying; Matteo, Tiziana Di; Bird, Simeon; Croft, Rupert A. C.; Feng, Yu; Chen, Nianyi; Tremmel, Michael; DeGraf, Colin; Li, Yin

doi:10.1093/mnras/stac351

Cited by 78 publications

(59 citation statements)

References 101 publications

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“…Using the TNG model, Weinberger et al (2018) studied the growth rates of black holes and showed for M BH > 10 9.5 M mergers with other black holes dominated their growth at z < 1. Sim-ulations that do not use repositioning, such as Ni et al (2022), show subdominant growth from mergers at all redshifts.…”

Section: Bcg Black Holementioning

confidence: 99%

There and back again: understanding the critical properties of backsplash galaxies

Borrow¹,

Vogelsberger²,

O’Neil³

et al. 2022

Preprint

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Backsplash galaxies are galaxies that once resided inside a cluster, and have migrated back oustide as they move towards the apocenter of their orbit. The kinematic properties of these galaxies are well understood, thanks to the significant study of backsplashers in dark matter-only simulations, but their intrinsic properties are not well constrained due to modelling uncertainties in sub-grid physics, ram pressure stripping, dynamical friction, and tidal forces. In this paper, we use the Illustris-TNG-300-1 simulation, with a baryonic resolution of M b ≈ 1.1 × 10 7 M , to study backsplash galaxies around 1302 isolated galaxy clusters with mass 10 13.0 < M 200,mean /M < 10 15.5 . We employ a decision tree classifier to extract features of galaxies that make them likely to be backsplash galaxies, compared to nearby field galaxies, and find that backsplash galaxies have low gas fractions, high mass-to-light ratios, large stellar sizes, and low black hole occupation fractions. We investigate in detail the origins of these large sizes, and hypothesise their origins are linked to the tidal environments in the cluster. We show that the black hole recentering scheme employed in many cosmological simulations leads to the loss of black holes from galaxies accreted into clusters, and suggest improvements to these models. Generally, we find that backsplash galaxies are a useful population to test and understand numerical galaxy formation models.

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Section: Bcg Black Holementioning

confidence: 99%

There and back again: understanding the critical properties of backsplash galaxies

Borrow¹,

Vogelsberger²,

O’Neil³

et al. 2022

Preprint

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“…Our work was motivated by our previous analysis of wandering IMBHs in the Illustris TNG50 simulation (Weller et al 2022), for which we had to resort to stellar clusters as proxies to investigate IMBHs, due to the lack of BHs in the appropriate mass range. In the cosmological simulation ASTRID (Ni et al 2022;Bird et al 2022), BHs in the mass range of IMBHs are self-consistently modeled, easing our way to investigate their orbital and radiative properties in massive galaxies at 𝑧 ∼ 3. We caution the reader that these galaxies are more gas-rich than local ones.…”

Section: Discussionmentioning

confidence: 99%

“…ASTRID implements a variety of sub-grid models for physics governing the formation of galaxies and SMBHs and their associated supernova and AGN feedback, inhomogeneous hydrogen, helium reionization, and the effect of massive neutrinos. Here we briefly summarize the physical models used in the simulation and refer the readers to the introductory paper Ni et al (2022); Bird et al (2022) for more detailed descriptions.…”

Section: Astrid -The Cosmological Simulationmentioning

confidence: 99%

“…With the halo-based BH seeding algorithm applied in ASTRID , the population of wandering BHs are mostly brought by the galaxy mergers through the hierarchical structure formation. The mean occupation number of the BHs grows with their host galaxy mass (see Ni et al 2022). To study the population of wandering BHs in massive galaxies at 𝑧 ∼ 3, we selected three examples of massive halos at this redshift.…”

Section: Galaxy Selectionmentioning

confidence: 99%

“…Other proposed methods for IMBH formation include runaway mergers in globular star clusters, hyper-Eddington accretion onto stellar-mass BHs, supra-exponential accretion on seed BHs, and direct collapse of hypermassive quasi-stars (see, e.g., Governato et al 1994;Volonteri et al 2003;Holley-Bockelmann et al 2008;Fragione & Kocsis 2018;Greene et al 2020;Pacucci & Loeb 2020 and references therein). dering IMBHs in massive 𝑧 ∼ 3 galaxies using the cosmological simulation ASTRID (Bird et al 2022;Ni et al 2022;Chen et al 2022b).…”

Section: Introductionmentioning

confidence: 99%

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Orbital and Radiative Properties of Wandering Intermediate-Mass Black Holes in the ASTRID Simulation

Weller¹,

Pacucci²,

Ni³

et al. 2022

Preprint

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Intermediate-Mass Black Holes (IMBHs), defined as having a mass in the range 10 3 M to 10 6 M , are commonly found at the center of dwarf galaxies. Simulations and observations convincingly show that a sizable population of IMBHs could wander offcenter in local galaxies. We use the cosmological simulation ASTRID to study the orbital and radiative properties of wandering IMBHs in massive galaxies at 𝑧 ∼ 3. We find that this population of undetected black holes has large orbital inclinations (60 • ± 22 • ) with respect to the principal plane of the host. The eccentricity of their orbits is also significant (0.6 ± 0.2) and decreases with time. Wandering IMBHs undergo spikes of accretion activity around the pericenter of their orbits, with rates 10 −3 − 10 −5 times the Eddington rate and a median accretion duty cycle of ∼ 12%. Their typical spectral energy distribution peaks in the infrared at ∼ 11 𝜇m rest frame. The studied IMBHs reach 2 − 10 keV X-ray luminosities > 10 37 erg s −1 for ∼ 10% of the time. This luminosity corresponds to fluxes > 10 −15 erg s −1 cm −2 within 10 Mpc. Two out of the 28 IMBHs studied (∼ 7%) have brief X-ray luminosity spikes > 10 41 erg s −1 , in the hyper-luminous X-ray sources (HLXs) regime. These findings suggest that HLXs are a small subset of the general wandering IMBH population, which is characterized by luminosities 10 3 − 10 4 times fainter. Dedicated surveys with current and future observatories are needed to assess the demographics of this missing population of black holes.

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Dynamical friction of a massive black hole in a turbulent gaseous medium

Lescaudron¹,

Dubois²,

Beckmann³

et al. 2023

A&A

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The orbital decay of massive black holes in galaxies in the aftermath of mergers is at the heart of whether massive black holes successfully pair and merge, leading to emission of low-frequency gravitational waves. The role of dynamical friction sourced from the gas distribution has been uncertain because many analytical and numerical studies have either focussed on a homogeneous medium or have not reached resolutions below the scales relevant to the problem, namely the Bondi-Hoyle-Lyttleton radius. We performed numerical simulations of a massive black hole moving in a turbulent medium in order to study dynamical friction from turbulent gas. We find that the black hole slows down to the sound speed, rather than the turbulent speed, and that the orbital decay is well captured if the Bondi-Hoyle-Lyttleton radius is resolved with at least five resolution elements. We find that the larger the turbulent eddies, the larger the scatter in dynamical friction magnitude, because of the stochastic nature of the problem, and also because of the larger over- and under-densities encountered by the black hole along its trajectory. Compared to the classic solution in a homogeneous medium, the magnitude of the force depends more weakly on the Mach number, and dynamical friction is overall more efficient for high Mach numbers, but less efficient towards and at the transonic regime.

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The ASTRID simulation: the evolution of supermassive black holes

Cited by 78 publications

References 101 publications

There and back again: understanding the critical properties of backsplash galaxies

There and back again: understanding the critical properties of backsplash galaxies

Orbital and Radiative Properties of Wandering Intermediate-Mass Black Holes in the ASTRID Simulation

Dynamical friction of a massive black hole in a turbulent gaseous medium

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