WISDOM Project – III. Molecular gas measurement of the supermassive black hole mass in the barred lenticular galaxy NGC4429

Davis, Timothy A.; Bureau, Martin; Onishi, Kyoko; Voort, Freeke van de; Cappellari, Michele; Iguchi, Satoru; Liu, Lijie; North, Eve V.; Sarzi, Marc; Smith, Mark D.

doi:10.1093/mnras/stx2600

Cited by 60 publications

(107 citation statements)

References 71 publications

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“…The Cycle 2 and 4 data both show a centrally concentrated CO flux distribution (Figure 7), and the Cycle 4 imaging with a beam size corresponding to 17 pc partially resolves the CO(2−1) emission into large, cloud-like knots (Figure 8). Clumpy emission-line structure appears to be common for molecular gas disks in ETGs when observed at similar physical resolutions (Utomo et al 2015;Barth et al 2016a;Davis et al , 2018. We identify a central hole in CO surface brightness with a radius of ∼ 0.…”

Section: Emission Line Propertiessupporting

confidence: 58%

A Precision Measurement of the Mass of the Black Hole in NGC 3258 from High-resolution ALMA Observations of Its Circumnuclear Disk

Boizelle

Barth

Walsh

et al. 2019

ApJ

102

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We present ∼ 0. 10−resolution Atacama Large Millimeter/submillimeter Array (ALMA) CO(2−1) imaging of the arcsecond-scale (r ≈ 150 pc) dusty molecular disk in the giant elliptical galaxy NGC 3258. The data provide unprecedented resolution of cold gas disk kinematics within the dynamical sphere of influence of a supermassive black hole, revealing a quasi-Keplerian central increase in projected rotation speed rising from 280 km s −1 at the disk's outer edge to > 400 km s −1 near the disk center. We construct dynamical models for the rotating disk and fit beam-smeared model CO line profiles directly to the ALMA data cube. Our models incorporate both flat disks and tilted-ring disks that provide a better fit of the mildly warped structure in NGC 3258. We show that the exceptional angular resolution of the ALMA data makes it possible to infer the host galaxy's mass profile within r = 150 pc solely from the ALMA CO kinematics, without relying on optical or near-infrared imaging data to determine the stellar mass profile. Our model therefore circumvents any uncertainty in the black hole mass that would result from the substantial dust extinction in the galaxy's central region. The best model fit yields M BH = 2.249 × 10 9 M with a statistical model-fitting uncertainty of just 0.18%, and systematic uncertainties of 0.62% from various aspects of the model construction and 12% from uncertainty in the distance to NGC 3258. This observation demonstrates the full potential of ALMA for carrying out highly precise measurements of M BH in early-type galaxies containing circumnuclear gas disks.

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Section: Emission Line Propertiessupporting

confidence: 58%

A Precision Measurement of the Mass of the Black Hole in NGC 3258 from High-resolution ALMA Observations of Its Circumnuclear Disk

Boizelle

Barth

Walsh

et al. 2019

ApJ

102

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“…High-resolution observations of gas in the centers of Seyfert galaxies suggest nuclear bars may be intimately tied to AGN phenomena, closely linked to the feeding and growth of SMBHs (e.g., Onishi et al 2015;Barth et al 2016;Davis et al 2017Davis et al , 2018. Given the bar-like kinematic substructure from our Br α measurements, the radio core of NGC 253 near TH2 is an excellent target for high-resolution IR-radio gas spectroscopy.…”

Section: The Radio Core As the Galactic Centermentioning

confidence: 89%

Unveiling kinematic structure in the starburst heart of NGC 253

Cohen

Turner

Consiglio

2020

Monthly Notices of the Royal Astronomical Society

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We investigate the kinematics of ionized gas within the nuclear starburst of NGC 253 with observations of the Brackett α recombination line at 4.05 µm. The goal is to distinguish motions driven by star-formation feedback from gravitational motions induced by the central mass structure. Using NIRSPEC on Keck II, we obtained 30 spectra through a 0. 5 slit stepped across the central ∼5 ×25 (85 × 425 pc) region to produce a spectral cube. The Brα emission resolves into four nuclear sources: S1 at the infrared core (IRC), N1 at the radio core near nonthermal source TH2, and the fainter sources N2 and N3 in the northeast. The line profile is characterized by a primary component with ∆v primary ∼90-130 km s −1 (FWHM) on top of a broad blue wing with ∆v broad ∼300-350 km s −1 , and an additional redshifted narrow component in the west. The velocity field generated from our cube reveals several distinct patterns. A mean NE-SW velocity gradient of +10 km s −1 arcsec −1 along the major axis traces the solidbody rotation curve of the nuclear disk. At the radio core, isovelocity contours become S-shaped, indicating the presence of secondary nuclear bar of total extent ∼5 (90 pc). The symmetry of the bar places the galactic center near the radio peak TH2 of the galaxy rather than the IRC, and makes this the most likely location of a SMBH. A third kinematic substructure is formed by blueshifted gas on the southeast side of the IRC. This feature likely traces a ∼100-250 km s −1 starburst-driven outflow, linking the IRC to the galactic wind observed on kpc scales.

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“…Spatially resolving the Keplerian region allows the SMBH mass to be constrained to high accuracy (see e.g. Onishi et al 2017;Davis et al 2017Davis et al , 2018.…”

Section: Ngc 3557mentioning

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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WISDOM Project – III. Molecular gas measurement of the supermassive black hole mass in the barred lenticular galaxy NGC4429

Cited by 60 publications

References 71 publications

A Precision Measurement of the Mass of the Black Hole in NGC 3258 from High-resolution ALMA Observations of Its Circumnuclear Disk

A Precision Measurement of the Mass of the Black Hole in NGC 3258 from High-resolution ALMA Observations of Its Circumnuclear Disk

Unveiling kinematic structure in the starburst heart of NGC 253

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

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