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dc.contributor.authorDavis, T.~A.
dc.contributor.authorBureau, M.
dc.contributor.authorOnishi, K.
dc.contributor.authorvan de Voort, F.
dc.contributor.authorCappellari, M.
dc.contributor.authorIguchi, S.
dc.contributor.authorLiu, L.
dc.contributor.authorNorth, E.~V.
dc.contributor.authorSarzi, M.
dc.contributor.authorSmith, M.~D.
dc.date.accessioned2018-09-12T15:20:43Z
dc.date.available2018-09-12T15:20:43Z
dc.date.issued2018-01-21
dc.identifier.citationDavis , T A , Bureau , M , Onishi , K , van de Voort , F , Cappellari , M , Iguchi , S , Liu , L , North , E V , Sarzi , M & Smith , M D 2018 , ' WISDOM Project - III. Molecular gas measurement of the supermassive black hole mass in the barred lenticular galaxy NGC4429 ' , Monthly Notices of the Royal Astronomical Society , vol. 473 , no. 3 , pp. 3818-3834 . https://doi.org/10.1093/mnras/stx2600
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 13356793
dc.identifier.otherPURE UUID: 12938aff-6162-4bca-8efb-78a34cc3a22b
dc.identifier.otherBibtex: urn:c67471bf01b78ea5a96e71ff163b2527
dc.identifier.otherScopus: 85045998360
dc.identifier.urihttps://arxiv.org/abs/1710.01488
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
dc.description.abstractAs part of the mm-Wave Interferometric Survey of Dark Object Masses project we present an estimate of the mass of the supermassive black hole (SMBH) in the nearby fast-rotating early-type galaxy NGC4429, that is barred and has a boxy/peanut-shaped bulge. This estimate is based on Atacama Large Millimeter/submillimeter Array (ALMA) cycle-2 observations of the 12CO(3-2) emission line with a linear resolution of ≈13 pc (0.18 arcsec × 0.14 arcsec). NGC4429 has a relaxed, flocculent nuclear disc of molecular gas that is truncated at small radii, likely due to the combined effects of gas stability and tidal shear. The warm/dense 12CO(3-2) emitting gas is confined to the inner parts of this disc, likely again because the gas becomes more stable at larger radii, preventing star formation. The gas disc has a low velocity dispersion of 2.2+ -0.65 0.68 km s -1. Despite the inner truncation of the gas disc, we are able to model the kinematics of the gas and estimate a mass of (1.5 ± 0.1+ -0.35 0.15 ) × 108 M ⊙ for the SMBH in NGC4429 (where the quoted uncertainties reflect the random and systematic uncertainties, respectively), consistent with a previous upper limit set using ionized gas kinematics. We confirm that the V-band mass-to-light ratio changes by ≈30 per cent within the inner 400 pc of NGC4429, as suggested by other authors. This SMBH mass measurement based on molecular gas kinematics, the sixth presented in the literature, once again demonstrates the power of ALMA to constrain SMBH masses.en
dc.format.extent17
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectCD
dc.subjectGalaxies: elliptical and lenticular
dc.subjectGalaxies: individual:NGC4429
dc.subjectGalaxies: ISM
dc.subjectGalaxies: kinematics and dynamics
dc.subjectGalaxies: nuclei
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleWISDOM Project - III. Molecular gas measurement of the supermassive black hole mass in the barred lenticular galaxy NGC4429en
dc.contributor.institutionSchool of Engineering and Technology
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85045998360&partnerID=8YFLogxK
dc.identifier.urlhttps://arxiv.org/abs/1710.01488
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stx2600
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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