AGNs and Their Host Galaxies in the Local Universe: Two Mass-independent Eddington Ratio Distribution Functions Characterize Black Hole Growth

Weigel, Anna K.; Schawinski, Kevin; Čaplar, Neven; Wong, O. I.; Treister, Ezequiel; Trakhtenbrot, Benny

doi:10.3847/1538-4357/aa803b

Cited by 42 publications

(63 citation statements)

References 254 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…As confirmed by previous studies (e.g. Aird et al 2012;Weigel et al 2017;Caplar et al 2018), such a trend is consistent with an anti-hierarchical growth of BHs, possibly linked to an intrinsically longer AGN duty cycle (Sect. 4.3).…”

Section: Extrapolating the Xlf Out To Z∼5supporting

confidence: 90%

“…Shedding light on these issues would be relevant for a number of studies focusing on the evolution of λ EDD distributions (e.g. Aird et al 2012;Bongiorno et al 2012;Weigel et al 2017;Caplar et al 2018;Bernhard et al 2018Bernhard et al , 2019Aird et al 2019;Grimmett et al 2019). We thus argue that testing this empirical prediction in the intrinsic Eddington-ratio space is essential to constrain the buildup of the M BH /M relation and standard prescriptions for BH accretion distributions.…”

Section: From Sbhar To Intrinsic Eddington Ratiomentioning

confidence: 93%

“…(ii) Secondly, we assume that the intrinsic λ EDD distribution of AGN follows a broken-powerlaw profile, as parameterised in a number of recent studies (e.g. Caplar et al 2015Caplar et al , 2018Weigel et al 2017;Bernhard et al 2018). This will be further motivated in Section 2.6.…”

Section: Prior Assumptionsmentioning

confidence: 99%

See 2 more Smart Citations

The Evolving AGN Duty Cycle in Galaxies Since z ∼ 3 as Encoded in the X-Ray Luminosity Function

Delvecchio

Daddi

Aird

et al. 2020

ApJ

Self Cite

View full text Add to dashboard Cite

We present a new modeling of the X-ray luminosity function (XLF) of Active Galactic Nuclei (AGN) out to z∼3, dissecting the contribution of main-sequence (MS) and starburst (SB) galaxies. For each galaxy population, we convolved the observed galaxy stellar mass (M ) function with a grid of Mindependent Eddington ratio (λ EDD ) distributions, normalised via empirical black hole accretion rate (BHAR) to star formation rate (SFR) relations. Our simple approach yields an excellent agreement with the observed XLF since z∼3. We find that the redshift evolution of the observed XLF can only be reproduced through an intrinsic flattening of the λ EDD distribution, and with a positive shift of the break λ * , consistent with an anti-hierarchical behavior. The AGN accretion history is predominantly made by massive (10 10 44.36 + 1.28·(1+z). We infer that the probability of finding highly-accreting (λ EDD > 10%) AGN significantly increases with redshift, from 0.4% (3.0%) at z=0.5 to 6.5% (15.3%) at z=3 for MS (SB) galaxies, implying a longer AGN duty cycle in the early Universe. Our results strongly favor a M -dependent ratio between BHAR and SFR, as BHAR/SFR ∝ M 0.73[+0.22,−0.29] , supporting a non-linear BH buildup relative to the host. Finally, this framework opens potential questions on super-Eddington BH accretion and different λ EDD prescriptions for understanding the cosmic BH mass assembly.

show abstract

Section: Extrapolating the Xlf Out To Z∼5supporting

confidence: 90%

Section: From Sbhar To Intrinsic Eddington Ratiomentioning

confidence: 93%

See 1 more Smart Citation

The Evolving AGN Duty Cycle in Galaxies Since z ∼ 3 as Encoded in the X-Ray Luminosity Function

Delvecchio

Daddi

Aird

et al. 2020

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…12. A small BH with a high Eddington ratio is therefore equivalent to a more massive BH with a smaller Eddington ratio, keeping in mind that high Eddington ratios are much less abundant then low or intermediate values (Habouzit et al 2017;Weigel et al 2017). The indicated freefall times yield the time that gas needs at least to fall back towards the centre once the AGN is off.…”

Section: Agn Luminositymentioning

confidence: 99%

Active galactic nucleus outflows in galaxy discs

Hartwig

Volonteri

Dashyan

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Galactic outflows, driven by active galactic nuclei (AGNs), play a crucial role in galaxy formation and in the self-regulated growth of supermassive black holes (BHs). AGN feedback couples to and affects gas, rather than stars, and in many, if not most, gasrich galaxies cold gas is rotationally supported and settles in a disc. We present a 2D analytical model for AGN-driven outflows in a gaseous disc and demonstrate the main improvements, compared to existing 1D solutions. We find significant differences for the outflow dynamics and wind efficiency. The outflow is energy-driven due to inefficient cooling up to a certain AGN luminosity (∼ 10 43 erg s −1 in our fiducial model), above which the outflow remains momentum-driven in the disc up to galactic scales. We reproduce results of 3D simulations that gas is preferentially ejected perpendicular to the disc and find that the fraction of ejected interstellar medium is lower than in 1D models. The recovery time of gas in the disc, defined as the freefall time from the radius to which the AGN pushes the ISM at most, is remarkably short, of the order 1 Myr. This indicates that AGN-driven winds cannot suppress BH growth for long. Without the inclusion of supernova feedback, we find a scaling of the BH mass with the halo velocity dispersion of M BH ∝ σ 4.8 .

show abstract

“…We note, however, that X-ray studies (e.g., Aird et al 2012), optical studies with well-characterized selection functions (e.g., Schulze & Wisotzki 2010), and phenomenological modeling (e.g., Weigel et al 2017) argue that the Eddington ratio distribution of quasars is more power-law-like. There appears to be a weak trend with mass in Figure 11, albeit with a large scatter.…”

Section: Correlation With Black Hole Massesmentioning

confidence: 99%

Quasar Accretion Disk Sizes from Continuum Reverberation Mapping from the Dark Energy Survey

Mudd¹,

Martini²,

Zu³

et al. 2018

ApJ

View full text Add to dashboard Cite

We present accretion disk size measurements for 15 luminous quasars at 0.7z1.9 derived from griz light curves from the Dark Energy Survey. We measure the disk sizes with continuum reverberation mapping using two methods, both of which are derived from the expectation that accretion disks have a radial temperature gradient and the continuum emission at a given radius is well described by a single blackbody. In the first method we measure the relative lags between the multiband light curves, which provides the relative time lag between shorter and longer wavelength variations. From this, we are only able to constrain upper limits on disk sizes, as many are consistent with no lag the 2σ level. The second method fits the model parameters for the canonical thin disk directly rather than solving for the individual time lags between the light curves. Our measurements demonstrate good agreement with the sizes predicted by this model for accretion rates between 0.3 and 1 times the Eddington rate. Given our large uncertainties, our measurements are also consistent with disk size measurements from gravitational microlensing studies of strongly lensed quasars, as well as other photometric reverberation mapping results, that find disk sizes that are a factor of a few (∼3) larger than predictions.

show abstract

AGNs and Their Host Galaxies in the Local Universe: Two Mass-independent Eddington Ratio Distribution Functions Characterize Black Hole Growth

Cited by 42 publications

References 254 publications

The Evolving AGN Duty Cycle in Galaxies Since z ∼ 3 as Encoded in the X-Ray Luminosity Function

The Evolving AGN Duty Cycle in Galaxies Since z ∼ 3 as Encoded in the X-Ray Luminosity Function

Active galactic nucleus outflows in galaxy discs

Quasar Accretion Disk Sizes from Continuum Reverberation Mapping from the Dark Energy Survey

Contact Info

Product

Resources

About