Active Galactic Nucleus Feedback in an Elliptical Galaxy with the Most Updated AGN Physics. I. Low Angular Momentum Case

Yuan, Feng; Yoon, Doosoo; Li, Y.; Gan, Zhaoming; Ho, Luis C.; Guo, Fulai

doi:10.3847/1538-4357/aab8f8

Cited by 133 publications

(138 citation statements)

References 127 publications

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“…BH accretion has large variability (e.g. Sartori et al 2018;Yuan et al 2018) on the relevant BH-growth time scales (∼ 10 6−8 yr) that may hide any BH-galaxy connection within individual objects, making BHAR an ideal estimator for our study. The inclusion of X-ray undetected sources also enables us to analyze all sources in different CANDELS fields seamlessly with different X-ray depths (see Table 1).…”

Section: Black-hole Accretion Ratementioning

confidence: 99%

Does black hole growth depend fundamentally on host-galaxy compactness?

Yang

Brandt

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Possible connections between central black-hole (BH) growth and host-galaxy compactness have been found observationally, which may provide insight into BH-galaxy coevolution: compact galaxies might have large amounts of gas in their centers due to their high mass-to-size ratios, and simulations predict that high central gas density can boost BH accretion. However, it is not yet clear if BH growth is fundamentally related to the compactness of the host galaxy, due to observational degeneracies between compactness, stellar mass (M ), and star formation rate (SFR). To break these degeneracies, we carry out systematic partial-correlation studies to investigate the dependence of sample-averaged BH accretion rate (BHAR) on the compactness of host galaxies, represented by the surface-mass density, Σ e , or the projected central surfacemass density within 1 kpc, Σ 1 . We utilize 8842 galaxies with H < 24.5 in the five CANDELS fields at z = 0.5-3. We find that BHAR does not significantly depend on compactness when controlling for SFR or M among bulge-dominated galaxies and galaxies that are not dominated by bulges, respectively. However, when testing is confined to star-forming galaxies at z = 0.5-1.5, we find that the BHAR-Σ 1 relation is not simply a secondary manifestation of a primary BHAR-M relation, which may indicate a link between BH growth and the gas density within the central 1 kpc of galaxies.

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Section: Black-hole Accretion Ratementioning

confidence: 99%

Does black hole growth depend fundamentally on host-galaxy compactness?

Yang

Brandt

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…In this paper, we do not discuss the regime of higher accretion rate where various feedback processes would be important, e.g., radiation, winds and jets (e.g., Sazonov et al 2005;Ciotti & Ostriker 2001;Proga 2007;Yuan et al 2009;Ciotti et al 2009;Booth & Schaye 2009;Milosavljević et al 2009;Yuan & Li 2011;Novak et al 2011;Choi et al 2012Choi et al , 2014Costa et al 2014;Xie et al 2017;Yuan et al 2018;Yoon et al 2018;Bu & Yang 2019, and see Fabian 2012 references therein). We define the critical BH accretion rateṁ fb , above which a steady state no longer exists due to feedback but gas accretion occurs episodically.…”

Section: The Formation Of a Cold Accretion Diskmentioning

confidence: 99%

Transition of BH feeding from the quiescent regime into star-forming cold disc regime

Inayoshi

Ichikawa

Ostriker

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We study the properties of rotating accretion flows onto supermassive black holes (SMBHs) using axisymmetric two-dimensional hydrodynamical simulations with radiative cooling and BH feedback. The simulations resolve the accretion dynamics of gas outside from the BH influence radius through an inner accretion disk. For lower Bondi accretion rates in units of the Eddington rate (Ṁ B 10 −3Ṁ Edd ), the BH feeding is suppressed due to turbulent motion by several orders of magnitude from the Bondi rate with outflows to the Bondi radius nearly balancing inflows. Thus, the radiative luminosity results in as low as ∼ 10 −10 − 10 −7 L Edd , where L Edd is the Eddington luminosity. For higher rates ofṀ B > ∼ 10 −3Ṁ Edd , the optically-thin accreting gas cools via free-free emission and forms a geometrically-thin disk, which feeds the BH efficiently and increases the radiative luminosity to > ∼ 10 −3 L Edd . The transitional behavior of accreting BHs in galactic nuclei from radiatively inefficient phases to cold disk accretion naturally explains (1) the reason for the offset between the observed luminosities and theoretical predictions for nearby quiescent SMBHs, and (2) the conditions to fuel gas into the nuclear SMBH. In addition, the cold disk formed in galactic nuclei tends to be gravitationally unstable and leads to star formation when the Bondi rate is as high asṀ B > ∼ 10 −2 M yr −1 . This is a plausible explanation of the correlation observed between star formation rates and BH feeding rates in Seyfert galaxies.

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“…The cold gas reservoir in the central galaxy is an ideal place for the onset of the radiative cooling instability, which leads to active star formation. We calculate the star formation rate per unit volume by means of a recipe that reproduces quite well the standard Schmidt-Kennicutt empirical relation, as in our previous works (e.g., Novak et al 2011;Yuan et al 2018b),…”

Section: Star Formation and Stellar Feedbackmentioning

confidence: 99%

“…But their resolution has to be rather low, e.g., several kpc; it is thus difficult to study the details of AGN feedback. Another approach is to focus on the much smaller galaxy scale (Ciotti & Ostriker 1997Novak et al 2011Novak et al , 2012Gaspari et al 2013;Gan et al 2014;Hopkins et al 2016;Yuan et al 2018b;Yoon et al 2018;Li et al 2018). The advantage of this kind of model is that we can easily resolve the boundary of black hole accretion flow, i.e., the Bondi radius, which is typically several tens of pc.…”

Section: Introductionmentioning

confidence: 99%

On the Role of the Hot Feedback Mode in Active Galactic Nuclei Feedback in an Elliptical Galaxy

Yoon

Yuan

Ostriker

et al. 2019

ApJ

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Depending on the value of the accretion rate, black hole accretion is divided into cold and hot modes. The two modes have distinctly different physics and correspond to two feedback modes. Most previous feedback works either focus only on one mode, or the accretion physics is not always properly adopted. Here, by performing hydrodynamical numerical simulations of AGN feedback in an elliptical galaxy, we show that including both is important, and gives different results from including just one or the other. We specifically focus on the wind and radiation (but neglecting the jet) feedback in the hot mode, to explore whether this particular mode of feedback can play any important feedback role. For this aim, we have run two test models. In one model, we always adopt the cold mode no matter what value the accretion rate is; in another model, we turn off the AGN once it enters into the hot mode. We have calculated the AGN light curves, black hole growth, star formation, and AGN energy duty-cycle; and compared the results with the model in which the two modes are correctly included. Important differences are found. For example, if we were to adopt only the cold mode, the total mass of newly formed stars would become two orders of magnitude smaller, and the fraction of energy ejected within the high accretion regime (i.e., L BH > 2%L Edd ) would be too small to be consistent with observations. We have also investigated the respective roles of wind and radiation in the hot mode.

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Active Galactic Nucleus Feedback in an Elliptical Galaxy with the Most Updated AGN Physics. I. Low Angular Momentum Case

Cited by 133 publications

References 127 publications

Does black hole growth depend fundamentally on host-galaxy compactness?

Does black hole growth depend fundamentally on host-galaxy compactness?

Transition of BH feeding from the quiescent regime into star-forming cold disc regime

On the Role of the Hot Feedback Mode in Active Galactic Nuclei Feedback in an Elliptical Galaxy

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