Fast and energetic AGN-driven outflows in simulated dwarf galaxies

Koudmani, Sophie; Sijacki, Debora; Bourne, Martin A.; Smith, Matthew C.

doi:10.1093/mnras/stz097

Cited by 69 publications

(59 citation statements)

References 97 publications

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“…Complementary approaches are becoming possible with the implementation of super-Lagrangian refinement techniques in other cosmological simulations codes. Curtis & Sijacki (2015, 2016b implemented a dynamic refinement scheme in the moving-mesh code AREPO (Springel 2010) to increase the resolution dynamically around the black hole, which has been used to improve black hole feedback implementations in cosmological simulations (Curtis & Sijacki 2016a) and idealized simulations of galaxies (Koudmani et al 2019) and clusters (Bourne & Sijacki 2017). Beckmann et al (2019) presented a new refinement scheme to resolve the black hole radius of influence in RAMSES (Teyssier 2002) and studied the growth of black hole seeds in isolated cooling halos.…”

Section: Comparison To Previous Methodologiesmentioning

confidence: 99%

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: Comparison To Previous Methodologiesmentioning

confidence: 99%

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

Anglés-Alcázar

Quataert

Hopkins

et al. 2021

ApJ

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“…with reduced or null SFR) with an AGN show a clear decoupling in the rotation of stars and gas. However, the relationship of gas kinematics to BH feedback is not clear for all galaxies (see also: Koudmani et al 2019). In particular, Ilha et al (2019) find that the typical decoupling between stars and gas for AGN defined galaxies is consistent with an inactive control sample.…”

Section: Introductionmentioning

confidence: 95%

Decoupling the rotation of stars and gas – II. The link between black hole activity and simulated IFU kinematics in IllustrisTNG

Duckworth

Starkenburg

Genel

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study the relationship between supermassive black hole (BH) feedback, BH luminosity, and the kinematics of stars and gas for galaxies in IllustrisTNG. We use galaxies with mock MaNGA observations to identify kinematic misalignment at z = 0 (difference in rotation of stars and gas), for which we follow the evolutionary history of BH activity and gas properties over the last 8 Gyr. Misaligned low-mass galaxies ($\mathrm{\mathit{ M}_{stel} \lt 10^{10.2}\, \mathrm{M}_{\odot }}$) typically have boosted BH luminosity and BH growth, and have had more energy injected by BHs into the gas over the last 8 Gyr in comparison to low-mass aligned galaxies. These properties likely lead to outflows and gas removal, in agreement with active low mass galaxies in observations. Splitting on BH luminosity at z = 0 produces consistent distributions of kinematic misalignment at z = 0; however, splitting on the maximum BH luminosity over the last 8 Gyr produces statistically significant different distributions. While instantaneous correlation at z = 0 is difficult due to misalignment persisting on longer time-scales, the relationship between BH activity and misalignment is clear. High-mass quenched galaxies ($\mathrm{\mathit{ M}_{stel} \gt 10^{10.2}\, \mathrm{M}_{\odot }}$) with misalignment typically have similar BH luminosities, show lower gas fractions, and have typically lower gas phase metallicity over the last 8 Gyr in comparison to the high mass aligned.

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“…While this coupling efficiency is likely to be 1 to 10 per cent for SN (Dubois & Teyssier 2008), it remains largely unquantified for AGN in dwarfs (although recent studies indicate that the presence of an AGN has a positive impact on the efficiency of feedback in dwarfs, see e.g. Koudmani et al (2019)). We ignore coupling efficiencies in our analysis here.…”

Section: Agn Vs Sn Energetics: the Plausibility Of Agn Feedbackmentioning

confidence: 99%

AGN in dwarf galaxies: frequency, triggering processes and the plausibility of AGN feedback

Kaviraj

Martin

Silk

2019

Monthly Notices of the Royal Astronomical Society: Letters

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While AGN are considered to be key drivers of the evolution of massive galaxies, their potentially significant role in the dwarf-galaxy regime (M * < 10 9 M ⊙ ) remains largely unexplored. We combine optical and infrared data, from the Hyper Suprime-Cam (HSC) and the Wide-field Infrared Explorer (WISE) respectively, to explore the properties of ∼800 AGN in dwarfs at low redshift (z < 0.3). Infrared-selected AGN fractions are ∼10 -30 per cent in dwarfs, which, for reasonable duty cycles, indicates a high BH-occupation fraction. Visual inspection of the deep HSC images indicates that the merger fraction in dwarf AGN (∼6 per cent) shows no excess compared to a control sample of non-AGN, suggesting that the AGN-triggering processes are secular in nature. Energetic arguments indicate that, in both dwarfs and massive galaxies, bolometric AGN luminosities (L AGN ) are significantly greater than supernova luminosities (L SN ). L AGN /L SN is, in fact, higher in dwarfs, with predictions from simulations suggesting that this ratio only increases with redshift. Together with the potentially high BH-occupation fraction, this suggests that, if AGN feedback is an important driver of massive-galaxy evolution, the same is likely to be true in the dwarf regime, contrary to our classical thinking.

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Fast and energetic AGN-driven outflows in simulated dwarf galaxies

Cited by 69 publications

References 97 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

Decoupling the rotation of stars and gas – II. The link between black hole activity and simulated IFU kinematics in IllustrisTNG

AGN in dwarf galaxies: frequency, triggering processes and the plausibility of AGN feedback

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