Black hole obscuration and duty-cycles mediated by AGN feedback in high-redshift galaxies

Trebitsch, Maxime; Volonteri, Marta; Dubois, Yohan

doi:10.1093/mnras/stz1280

Cited by 46 publications

(55 citation statements)

References 83 publications

(108 reference statements)

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“…This is mostly caused by the circumnuclear gas at r < 100 pc from the PBH. This result is consistent with recent numerical results reported by Trebitsch et al (2019), in which cosmological radiative hydrodynamic simulations of galaxy formation are used to study the nuclear obscuration.…”

Section: Discussion: Origin Of Obscured Agnssupporting

confidence: 92%

Mass Accretion toward Black Holes in the Final Phase of Galaxy Mergers

Kawaguchi

Yutani

Wada

2020

ApJ

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We studied the final phases of galactic mergers, focusing on interactions between supermassive black holes (SMBHs) and the interstellar medium in a central sub-kpc region, using an N-body/hydrodynamics code. This numerical experiment aims to understand the fate of the gas supplied by mergers of two or more galaxies with SMBHs, whose masses are 10 7 M . We observed that the mass accretion rate to one SMBH exceeds the Eddington accretion rate when the distance between two black holes (BHs) rapidly decreases. However, this rapid accretion phase does not last for more than 10 7 yrs, and it drops to ∼ 10% of the Eddington rate in the quasisteady accretion phase. The rapid accretion is caused by the angular momentum transfer from the gas to the stellar component, and the moderate accretion in the quasi-steady phase is caused by turbulent viscosity and gravitational torque in the disk. The second merger event enhances the mass accretion to the BHs; however, this phase takes place on a similar timescale to the first merger event. We also found that the AGN feedback and the mass accretion to BHs can coexist in the central region of merged galaxies, if the amount of feedback energy is given as (2×10 −4 −2×10 −3 )Ṁ c 2 , whereṀ is the accretion rate to r = 1 pc. The accretion rate is suppressed by ∼ 1/50 in the quasi-steady accretion phase for 0.02Ṁ c 2 . The fraction of the gas that finally falls to each BH is approximately 5-7% of the supplied total gas mass (10 8 M ), and 15-20% of the gas forms a circumnuclear gas inside 100 pc. This remnant gas heavily obscures the luminous phase of the active galactic nuclei (AGN) during merger events, and the moderate AGN feedback does not alter this property.

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Section: Discussion: Origin Of Obscured Agnssupporting

confidence: 92%

Mass Accretion toward Black Holes in the Final Phase of Galaxy Mergers

Kawaguchi

Yutani

Wada

2020

ApJ

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“…Looking at the major branches of the halos, the AGN duty cycle τagn is log(τagn) ∼ 0.64 (0.18) for the progenitors of halos with M h ≈ 10 13.5 (10 11.5 ) M in the intrinsic case, since the major branch of higher-mass halos enters the Eddington-limited accretion phase at earlier times (Piana et al 2021). When obscuration effects are applied, these numbers go down by a factor of 4 (12) for halos with M h ≈ 10 13.5 (10 11.5 ) M , as expected by the mass dependence of the obscured fraction of AGN, and in qualitative agreement with the results found in Trebitsch et al (2019). Finally, the variance of τagn within each mass bin is directly linked to the specific variations in the mass assembly history (especially for halos with final masses M h < ∼ 10 12.3 M ).…”

Section: Fractional Lifetime For Agn Domination Of Uv Luminositysupporting

confidence: 85%

The impact of black hole feedback on the UV luminosity and stellar mass assembly of high-redshift galaxies

Piana,

Dayal,

Choudhury

2021

Preprint

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We employ the Delphi semi-analytical model to study the impact of black hole growth on high-redshift galaxies, both in terms of the observed UV luminosity and of the star formation rate. To do this, firstly, we assess the contribution of AGN to the total galaxy UV luminosity as a function of stellar mass and redshift. We estimate, together with their duty cycle, the observed fraction of AGN-dominated galaxies and find that they outnumber stellar-dominated galaxies at M UV < ∼ − 24 mag and z ≈ 5 − 6. Secondly, we study the evolution of the AGN and stellar luminosity functions (LFs), finding that it is driven both by changes in their characteristic luminosities M * (i.e. evolution of the intrinsic brightness of galaxies) and in their normalisations φ * (i.e. evolution of the number densities of galaxies), depending on the luminosity range considered. Finally, we follow the mass assembly history for three different halo mass bins, finding that the magnitude of AGN-driven outflows depends on the host halo mass. We show that AGN feedback is most effective when the energy emitted by the accreting black hole is approximately 1% of the halo binding energy, and that this condition is met in galaxies in halos with M h ∼ 10 11.75 M at z = 4. In such cases, AGN feedback can drive outflows that are up to 100 times more energetic than SN-driven outflows, and the star formation rate is a factor of three lower than for galaxies of the same mass without black hole activity.

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“…While many of them focused on the relative impact of stellar feedback (e.g. Pallottini et al 2017a;Trebitsch et al 2018;Ma et al 2018;Katz et al 2017Katz et al , 2019, the chemical composition (Maio & Tescari 2015;Arata et al 2020), and the role of active galactic nuclei (Trebitsch et al 2019;Lupi et al 2019), other studies tried to more accurately describe how the FIR emission is affected by different gas conditions, (e.g. Vallini et al 2013;Olsen et al 2015), also considering the impact of the cosmic microwave background and the metallicity on the powered emission (Vallini et al 2015;Olsen et al 2017), internal structure of molecular clouds Decataldo et al in prep), the importance of the radiation field (Vallini et al 2017;Pallottini et al 2019;Arata et al 2019), and possible bias in the comparison between theory and simulations (Kohandel et al 2019;Lupi et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Predicting FIR lines from simulated galaxies

Lupi

Pallottini

Ferrara

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Far-infrared (FIR) emission lines are a powerful tool to investigate the properties of the interstellar medium, especially in high-redshift galaxies, where ALMA observations have provided unprecedented information. Interpreting such data with state-of-the-art cosmological simulations post-processed with cloudy, has provided insights on the internal structure and gas dynamics of these systems. However, no detailed investigation of the consistency and uncertainties of this kind of analysis has been performed to date. Here, we compare different approaches to estimate FIR line emission from state-of-the-art cosmological simulations, either with cloudy or with on-the-fly non-equilibrium chemistry. We find that [C ii]158μ predictions are robust to the model variations we explored. [O i] emission lines, that typically trace colder and denser gas relative to [C ii]158μ, are instead model dependent, as these lines are strongly affected by the thermodynamic state of the gas and non-equilibrium photoionization effects. For the same reasons, [O i] lines represent an excellent tool to constrain emission models, hence future observations targeting these lines will be crucial.

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Black hole obscuration and duty-cycles mediated by AGN feedback in high-redshift galaxies

Cited by 46 publications

References 83 publications

Mass Accretion toward Black Holes in the Final Phase of Galaxy Mergers

Mass Accretion toward Black Holes in the Final Phase of Galaxy Mergers

The impact of black hole feedback on the UV luminosity and stellar mass assembly of high-redshift galaxies

Predicting FIR lines from simulated galaxies

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