WISDOM Project – II. Molecular gas measurement of the supermassive black hole mass in NGC 4697

Davis, Timothy A.; Bureau, Martin; Onishi, Kyoko; Cappellari, Michele; Iguchi, Satoru; Sarzi, M.

doi:10.1093/mnras/stw3217

Cited by 80 publications

(114 citation statements)

References 74 publications

(110 reference statements)

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“…Even outside our own galaxy, when the nuclear gas disk is well resolved and gas velocity profile carefully mapped, the mass estimate from gas kinematics is entirely consistent with stellar dynamics mass estimates (Davis et al 2017;Boizelle et al 2019). However, in galaxies where there is not a wellresolved disk, there are theoretical reasons to believe that, in sub-Eddington systems, inside the Bondi radius the gas does not lie on Keplerian or near-Keplerian orbits (Narayan & Yi 1994;Neumayer et al 2007;Chan & Krolik 2017;Imanishi et al 2018).…”

Section: Introductionsupporting

confidence: 79%

Impact of Accretion Flow Dynamics on Gas-dynamical Black Hole Mass Estimates

Jeter

Broderick

McNamara

2019

ApJ

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At low redshift, the majority of supermassive black hole (SMBH) mass estimates are obtained from modeling stellar kinematics or ionized gas dynamics in the vicinity of the galaxy nucleus. For large early type galaxies, stellar kinematics models predict higher masses than gas-dynamical models. In the case of M87, this discrepancy is larger than 2 σ. Critical to gas-dynamical modeling is the assumed underlying dynamical state of the gas: that it lies on circular Keplerian orbits, potentially with some additional turbulent pressure support. This is inconsistent with models of the gas flow about low-accretion-rate SMBHs and at odds with observations of the Galactic Center.We present a simple model for non-Keplerian gas disks and explore their implications for SMBH mass measurements. We show that a larger central black hole with gas experiencing small amounts of sub-Keplerian motion can produce velocity curves similar to models that just contain circular Keplerian motions and a lower black hole mass. However, these non-Keplerian models are distinguishable from low-mass Keplerian models primarily through measurements of the velocity dispersion, wherein non-Keplerian models produce higher and narrower peak dispersions. Away from the galaxy center, but still within the circumnuclear gas disk, non-Keplerian models also become distinguishable from Keplerian models via a shift in the velocity curve. The velocity model presented in this paper is capable of resolving the discrepancy between the ionized gas dynamics and stellar kinematics mass estimates, and is applicable to gas-dynamical mass estimates of SMBHs in general.

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Section: Introductionsupporting

confidence: 79%

Impact of Accretion Flow Dynamics on Gas-dynamical Black Hole Mass Estimates

Jeter

Broderick

McNamara

2019

ApJ

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“…This, in principle, would indicate dynamically very cold gas (e.g. Davis et al 2017), but such a low σ gas value is not well constrained by the channel width of the IC 1531 datacube (20 km s −1 ). In fact, in interferometric line observations with moderate S/N, the smallest velocity dispersion that is possible to measure is approximately 2 √ 2ln2 times smaller than the channel width, or ≈ 9 km s −1 in this case (≈3 times the best-fit value reported in Table 2) .…”

Section: Gas Disc Stabilitymentioning

confidence: 99%

The AGN fuelling/feedback cycle in nearby radio galaxies – II. Kinematics of the molecular gas

Ruffa

Davis

Prandoni

et al. 2019

Monthly Notices of the Royal Astronomical Society

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This is the second paper of a series exploring the multi-component (stars, warm and cold gas and radio jets) properties of a sample of eleven nearby low excitation radio galaxies (LERGs), with the aim of better understanding the AGN fuelling/feedback cycle in these objects. Here we present a study of the molecular gas kinematics of six sample galaxies detected in 12 CO(2-1) with ALMA. In all cases, our modelling suggests that the bulk of the gas in the observed (sub-)kpc CO discs is in ordered rotation. Nevertheless, low-level distortions are ubiquitous, indicating that the molecular gas is not fully relaxed into the host galaxy potential. The majority of the discs, however, are only marginally resolved, preventing us from drawing strong conclusions. NGC 3557 and NGC 3100 are special cases. The features observed in the CO velocity curve of NGC 3557 allow us to estimate a super-massive black hole (SMBH) mass of (7.10 ± 0.02) × 10 8 M , in agreement with expectations from the M SMBH − σ * relation. The rotation pattern of NGC 3100 shows distortions that appear to be consistent with the presence of both a position angle and inclination warp. Non-negligible radial motions are also found in the plane of the CO disc, likely consistent with streaming motions associated with the spiral pattern found in the inner regions of the disc. The dominant radial motions are likely to be inflows, supporting a scenario in which the cold gas is contributing to the fuelling of the AGN.M SMBH is the mass of the central super-massive black hole, m p is the mass of the proton, ε is the accretion efficiency, c is the speed of light and σ T is the cross-section for Thomson scattering.

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“…The method we use to estimate the SMBH mass is described in detail in Davis et al (2017) and was used in the previous WISDOM papers, but we summarise the specifics for modelling NGC 0383 in this section. We make use of the publicly available Kinematic Molecular Simulation (KinMS) 3 mm-wave observation simulation tool of Davis et al (2013a) to create models of the data cube.…”

Section: Dynamical Modellingmentioning

confidence: 99%

“…The first use of this method with Carbon Monoxide (CO) was by Davis et al (2013b). SMBH mass measurements in fast-rotator early-type galaxies (Onishi et al 2017;Davis et al 2017Davis et al , 2018, galaxies with ir-regular gas distributions (Smith et al 2019), and in the first late-type galaxy with the dense molecular gas tracers HCN and HCO + (Onishi et al 2015) have been successful. Barth et al (2016a,b) and Boizelle et al (2019) also used CO to constrain the SMBH mass in the early-type galaxy NGC 1332 and NGC 3258.…”

Section: Introductionmentioning

confidence: 99%

WISDOM project – V. Resolving molecular gas in Keplerian rotation around the supermassive black hole in NGC 0383

North

Davis

Bureau

et al. 2019

Monthly Notices of the Royal Astronomical Society

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As part of the mm-Wave Interferometric Survey of Dark Object Masses (WISDOM), we present a measurement of the mass of the supermassive black hole (SMBH) in the nearby early-type galaxy NGC 0383 (radio source 3C 031). This measurement is based on Atacama Large Millimeter/sub-millimeter Array (ALMA) cycle 4 and 5 observations of the 12CO(2–1) emission line with a spatial resolution of 58 × 32 pc2 (0.18 arcsec × 0.1 arcsec). This resolution, combined with a channel width of 10 km s−1, allows us to well resolve the radius of the black hole sphere of influence (measured as RSOI = 316 pc = 0.98 arcsec), where we detect a clear Keplerian increase of the rotation velocities. NGC 0383 has a kinematically relaxed, smooth nuclear molecular gas disc with weak ring/spiral features. We forward model the ALMA data cube with the Kinematic Molecular Simulation (KinMS) tool and a Bayesian Markov Chain Monte Carlo method to measure an SMBH mass of (4.2 ± 0.7) × 109 M⊙, a F160W-band stellar mass-to-light ratio that varies from 2.8 ± 0.6 M⊙/L$_{\odot ,\, \mathrm{F160W}}$ in the centre to 2.4 ± 0.3 M⊙$/\rm L_{\odot ,\, \mathrm{F160W}}$ at the outer edge of the disc and a molecular gas velocity dispersion of 8.3 ± 2.1 km s−1(all 3σ uncertainties). We also detect unresolved continuum emission across the full bandwidth, consistent with synchrotron emission from an active galactic nucleus. This work demonstrates that low-J CO emission can resolve gas very close to the SMBH ($\approx 140\, 000$ Schwarzschild radii) and hence that the molecular gas method is highly complimentary to megamaser observations, as it can probe the same emitting material.

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WISDOM Project – II. Molecular gas measurement of the supermassive black hole mass in NGC 4697

Cited by 80 publications

References 74 publications

Impact of Accretion Flow Dynamics on Gas-dynamical Black Hole Mass Estimates

Impact of Accretion Flow Dynamics on Gas-dynamical Black Hole Mass Estimates

The AGN fuelling/feedback cycle in nearby radio galaxies – II. Kinematics of the molecular gas

WISDOM project – V. Resolving molecular gas in Keplerian rotation around the supermassive black hole in NGC 0383

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