The origin of spin in galaxies: clues from simulations of atomic cooling haloes

Prieto, J.; Jiménez, Raúl; Haiman, Zoltán; González, Roberto

doi:10.1093/mnras/stv1234

Cited by 22 publications

(44 citation statements)

References 45 publications

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“…Conversely the tidal field strength is low t1 = 0.2 in regions with thin converging filaments which bring in cold material fast and lead to the formation of the most massive black hole in a spheroidal dominated host. Tidal torque theory has been shown by Gonzalez et al (2016) to explain the initial spin of galaxies in hydrodynamic simulations at high redshifts, and Prieto et al (2015) have found that halos with fewer filaments tend to have larger spin. This is in agreement with the examples we have presented here, where the disc galaxies tend to lie in regions with two main filaments, and the low angular momentum galaxies that host black holes lie at the centers of a more symmetric arrangement of multiple filaments.…”

Section: The Origin Of the Fastest Black Hole Growth: Tidal Field Strmentioning

confidence: 93%

The origin of the most massive black holes at high-z: BlueTides and the next quasar frontier

Matteo

Croft

Feng

et al. 2017

Monthly Notices of the Royal Astronomical Society

114

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The growth of the most massive black holes in the early universe, consistent with the detection of highly luminous quasars at z > 6 implies sustained, critical accretion of material to grow and power them. Given a black hole seed scenario, it is still uncertain which conditions in the early Universe allow the fastest black hole growth. Large scale hydrodynamical cosmological simulations of structure formation allow us to explore the conditions conducive to the growth of the earliest supermassive black holes. We use the cosmological hydrodynamic simulation BlueTides, which incorporates a variety of baryon physics in a (400h −1 Mpc) 3 volume with 0.7 trillion particles to follow the earliest phases of black hole critical growth. At z = 8 the most massive black holes (a handful) approach masses of 10 8 M with the most massive (with M BH = 4 × 10 8 M ) being found in an extremely compact spheroid-dominated host galaxy. Examining the large-scale environment of hosts, we find that the initial tidal field is more important than overdensity in setting the conditions for early BH growth. In regions of low tidal fields gas accretes 'cold' onto the black hole and falls along thin, radial filaments straight into the center forming the most compact galaxies and most massive black holes at earliest times. Regions of high tidal fields instead induce larger coherent angular momenta and influence the formation of the first population of massive compact disks. The extreme early growth depends on the early interplay of high gas densities and the tidal field that shapes the mode of accretion. Mergers play a minor role in the formation of the first generation, rare massive BHs.

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Section: The Origin Of the Fastest Black Hole Growth: Tidal Field Strmentioning

confidence: 93%

The origin of the most massive black holes at high-z: BlueTides and the next quasar frontier

Matteo

Croft

Feng

et al. 2017

Monthly Notices of the Royal Astronomical Society

114

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“…Pichon et al 2011;Prieto et al 2015;Danovich et al 2015) is a robust motivation to study the MT process at different scales in the first galaxies. In the following, we analyze the MT process on kpc ( 0.1R vir ) scales.…”

Section: Mass Transport In the Discmentioning

confidence: 99%

How AGN and SN Feedback Affect Mass Transport and Black Hole Growth in High-redshift Galaxies

Prieto

Escala

Volonteri

et al. 2017

ApJ

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By using cosmological hydrodynamical simulations we study the effect of supernova (SN) and active galactic nuclei (AGN) feedback on the mass transport of gas on to galactic nuclei and the black hole (BH) growth down to redshift z ∼ 6. We study the BH growth in relation with the mass transport processes associated with gravity and pressure torques, and how they are modified by feedback. Cosmological gas funelled through cold flows reaches the galactic outer region close to free-fall. Then torques associated to pressure triggered by gas turbulent motions produced in the circum-galactic medium by shocks and explosions from SNe are the main source of mass transport beyond the central ∼ 100 pc. Due to high concentrations of mass in the central galactic region, gravitational torques tend to be more important at high redshift. The combined effect of almost free-falling material and both gravity and pressure torques produces a mass accretion rate of order ∼ 1 M /yr at ∼ pc scales. In the absence of SN feedback, AGN feedback alone does not affect significantly either star formation or BH growth until the BH reaches a sufficiently high mass of ∼ 10 6 M to self-regulate. SN feedback alone, instead, decreases both stellar and BH growth. Finally, SN and AGN feedback in tandem efficiently quench the BH growth, while star formation remains at the levels set by SN feedback alone due to the small final BH mass, ∼ few 10 5 M . SNe create a more rarefied and hot environment where energy injection from the central AGN can accelerate the gas further.

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“…In this picture Pichon et al 2011;Stewart et al 2011bStewart et al , 2013Codis et al 2012Codis et al , 2015Danovich et al 2012Danovich et al , 2015Prieto et al 2015;Tillson et al 2015), the particularly high angular momentum of cold flow gas is related to its coherent, filamentary origin, coupled with the specific geometry of the cosmic web in the environment of a given galaxy. These filamentary cold flows deliver significant angular momentum to galaxy halos, with the cold gas orbiting for ∼1−2 dynamical times before spiraling into the central galaxy.…”

Section: Introductionmentioning

confidence: 99%

High Angular Momentum Halo Gas: A Feedback and Code-independent Prediction of LCDM

Stewart

Maller

Oñorbe

et al. 2017

ApJ

110

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We investigate angular momentum acquisition in Milky Way-sized galaxies by comparing five high resolution zoom-in simulations, each implementing identical cosmological initial conditions but utilizing different hydrodynamic codes: Enzo, Art, Ramses, Arepo, and Gizmo-PSPH. Each code implements a distinct set of feedback and star formation prescriptions. We find that while many galaxy and halo properties vary between the different codes (and feedback prescriptions), there is qualitative agreement on the process of angular momentum acquisition in the galaxy's halo. In all simulations, cold filamentary gas accretion to the halo results in ∼4 times more specific angular momentum in cold halo gas (λ cold 0.1) than in the dark matter halo. At z>1, this inflow takes the form of inspiraling cold streams that are co-directional in the halo of the galaxy and are fueled, aligned, and kinematically connected to filamentary gas infall along the cosmic web. Due to the qualitative agreement among disparate simulations, we conclude that the buildup of high angular momentum halo gas and the presence of these inspiraling cold streams are robust predictions of Lambda Cold Dark Matter galaxy formation, though the detailed morphology of these streams is significantly less certain. A growing body of observational evidence suggests that this process is borne out in the real universe.

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The origin of spin in galaxies: clues from simulations of atomic cooling haloes

Cited by 22 publications

References 45 publications

The origin of the most massive black holes at high-z: BlueTides and the next quasar frontier

The origin of the most massive black holes at high-z: BlueTides and the next quasar frontier

How AGN and SN Feedback Affect Mass Transport and Black Hole Growth in High-redshift Galaxies

High Angular Momentum Halo Gas: A Feedback and Code-independent Prediction of LCDM

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