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WISDOM project - V. Resolving molecular gas in Keplerian rotation around the supermassive black hole in NGC0383

North, Eve V., Davis, Timothy A., Bureau, Martin, Cappellari, Michele, Iguchi, Satoru, Liu, Lijie, Onishi, Kyoko, Sarzi, Marc, Smith, Mark D. and Williams, Thomas G. 2019. WISDOM project - V. Resolving molecular gas in Keplerian rotation around the supermassive black hole in NGC0383. Monthly Notices of the Royal Astronomical Society , -. 10.1093/mnras/stz2598

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Abstract

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-milimeter Array (ALMA) cycle 4 and 5 observations of the 12CO(2–1) emission line with a spatial resolution of 58 × 32 pc2 (0 ′′ . .′′ 18 × 0 ′′ . .′′ 1). 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), 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 a 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⊙, F160W in the centre to 2.4 ± 0.3 M⊙/L ⊙,F160W /L⊙,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 (≈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.

Item Type: Article
Date Type: Published Online
Status: In Press
Schools: Physics and Astronomy
ISSN: 0035-8711
Date of First Compliant Deposit: 13 September 2019
Date of Acceptance: 4 September 2019
Last Modified: 18 Oct 2019 05:49
URI: http://orca.cf.ac.uk/id/eprint/125446

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