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Download (1MB) This is an Open Access document downloaded from ORCA, Cardiff University's institutional repository: http://orca.cf.ac.uk/136213/ This is the author’s version of a work that was submitted to / accepted for publication. Citation for final published version: Smith, Mark D., Bureau, Martin, Davis, Timothy A., Cappellari, Michele, Liu, Lijie, Onishi, Kyoko, Iguchi, Satoru, North, Eve V. and Sarzi, Marc 2021. WISDOM project - VI. Exploring the relation between supermassive black hole mass and galaxy rotation with molecular gas. Monthly Notices of the Royal Astronomical Society 500 , pp. 1933-1952. 10.1093/mnras/staa3274 file Publishers page: http://dx.doi.org/10.1093/mnras/staa3274 <http://dx.doi.org/10.1093/mnras/staa3274> Please note: Changes made as a result of publishing processes such as copy-editing, formatting and page numbers may not be reflected in this version. For the definitive version of this publication, please refer to the published source. You are advised to consult the publisher’s version if you wish to cite this paper. This version is being made available in accordance with publisher policies. See http://orca.cf.ac.uk/policies.html for usage policies. Copyright and moral rights for publications made available in ORCA are retained by the copyright holders. MNRAS 500, 1933–1952 (2021) doi:10.1093/mnras/staa3274 Advance Access publication 2020 October 22 WISDOM project – VI. Exploring the relation between supermassive black hole mass and galaxy rotation with molecular gas Mark D. Smith ,1‹ Martin Bureau,1,2 Timothy A. Davis ,3 Michele Cappellari ,1 Lijie Liu,1 Kyoko Onishi ,4,5,6 Satoru Iguchi ,5,6 Eve V. North 3 and Marc Sarzi7 1Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK 2Yonsei Frontier Lab and Department of Astronomy, Yonsei University, 50 Yonsei-ro, Seodaemun-gu, Seoul 03722, Republic of Korea 3School of Physics & Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, UK 4Research Center for Space and Cosmic Evolution, Ehime University, Matsuyama, Ehime 790-8577, Japan 5 Department of Astronomical Science, SOKENDAI (The Graduate University of Advanced Studies), Mitaka, Tokyo 181-8588, Japan 2021 11 January on guest by https://academic.oup.com/mnras/article/500/2/1933/5935252 from Downloaded 6National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Mitaka, Tokyo 181-8588, Japan 7Armagh Observatory and Planetarium, College Hill, Armagh BT61 DG, UK Accepted 2020 October 15. Received 2020 October 5; in original form 2020 February 11 ABSTRACT Empirical correlations between the masses of supermassive black holes (SMBHs) and properties of their host galaxies are well established. Among these is the correlation with the flat rotation velocity of each galaxy measured either at a large radius in its rotation curve or via a spatially integrated emission-line width. We propose here the use of the deprojected integrated CO emission-line width as an alternative tracer of this rotation velocity, which has already been shown useful for the Tully–Fisher (luminosity–rotation velocity) relation. We investigate the correlation between CO line widths and SMBH masses for two samples of galaxies with dynamical SMBH mass measurements, with spatially resolved and unresolved CO observations, respectively. The tightest correlation is found using the resolved sample of 25 galaxies as log(MBH/M ) 1 ⊙ = (7.5 0.1) (8.5 0.9)[log(W50/ sin i km s− ) 2.7], where MBH is the central SMBH mass, W50 is the full width at half- ± + ± − maximum of a double-horned emission-line profile, and i is the inclination of the CO disc. This relation has a total scatter of 0.6 dex, comparable to those of other SMBH mass correlations, and dominated by the intrinsic scatter of 0.5 dex. A tight correlation is also found between the deprojected CO line widths and the stellar velocity dispersions averaged within one effective radius. We apply our correlation to the COLD GASS sample to estimate the local SMBH mass function. Key words: galaxies: bulges – galaxies: general – galaxies: kinematics and dynamics – galaxies: nuclei – submillimetre: galax- ies. Peng 2007; Hirschmann et al. 2010; Jahnke & Maccio` 2011). The 1 INTRODUCTION relative importance of these mechanisms remains under dispute (e.g. Supermassive black holes (SMBHs) are found in the centres of almost Kormendy & Ho 2013; Simmons, Smethurst & Lintott 2017). all massive galaxies. They are now believed to play an instrumental The millimetre-Wave Interferometric Survey of Dark Object role in the evolution of their hosts, a conclusion drawn from the tight Masses (WISDOM) project aims to use the high angular resolutions correlations, spanning multiple orders of magnitude, between the achievable with the latest large millimetre/submillimetre interfer- SMBH masses and large-scale host properties (for reviews, see e.g. ometers to probe the environments around SMBHs. Principally, the Kormendy & Ho 2013;Graham2016). This is surprising given that, survey is measuring SMBH masses using molecular gas kinematics, in almost all galaxies following these correlations, the SMBH only as the interferometers can resolve spatial scales dominated by the dominates the gravitational potential on very small spatial scales SMBHs (Davis et al. 2013b, 2018a;Onishietal.2017; North et al. (100 pc), and it has a negligible gravitational influence on the 2019; Smith et al. 2019; Smith et al., in preparation). Other groups scales on which the host properties are measured. Nevertheless, have also used the same method to constrain SMBH masses (e.g. these tight correlations have been used to argue that each SMBH Onishi et al. 2015; Barth et al. 2016a,b; Boizelle et al. 2019;Nagai coevolves with its host, invoking mechanisms such as active galactic et al. 2019; Ruffa et al. 2019; Nguyen et al. 2020). In addition to nucleus (AGN) feedback (e.g. Bower et al. 2006;Crotonetal.2006; measuring SMBH masses, the same data can be used to investigate Vogelsberger et al. 2014), major merger-enhanced accretion (e.g. the physical state of the molecular gas and study giant molecular Sanders et al. 1988; Cattaneo, Haehnelt & Rees 1999; Di Matteo, clouds (Utomo et al. 2015; Liu et al. in preparation). In this paper, Springel & Hernquist 2005), and simple merger averaging (e.g. we use relatively low resolution CO observations to investigate a correlation between deprojected integrated CO line widths and SMBH masses, which we propose could be a useful estimator of ⋆ E-mail: [email protected] SMBH masses. C 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society 1934 M. D. Smith et al. 1.1 Dynamical signatures of SMBH–baryonic matter 1.2.1 CO Tully–Fisher relation correlations The TFR, relating the asymptotic velocity of a rotationally supported The tightest known correlations are those between the SMBH mass disc to its host galaxy’s absolute magnitude, is widely used to and properties of the host galaxy’s bulge – stellar velocity dispersion measure distances to extragalactic sources. For the last two decades, (σ ; e.g. Ferrarese & Merritt 2000;Gebhardtetal.2000), mass, since initial proposals by Dickey & Kazes (1992)andSofue(1992), ∗ or luminosity (Mbulge and Lbulge; e.g. Kormendy & Richstone 1995; millimetre-wave emission from CO molecules has been used as Magorrian et al. 1998; Marconi & Hunt 2003;Haring¨ & Rix 2004). an alternative to radio H I or optical H α emission to trace the These host quantities are measures of the stellar mass-dominated asymptotic rotation velocity (e.g. Ho 2007b; Davis et al. 2011, 2016; central potential of the bulge. Tiley et al. 2016, 2019;Topaletal.2018), including in early-type The MBH–σ relation has traditionally been viewed as the tightest galaxies (ETGs) where such rotationally supported CO discs are still ∗ correlation, with an intrinsic scatter of only 0.3 dex (e.g. Gebhardt reasonably common (e.g. Davis et al. 2013a). ≈ et al. 2000; Beifiori et al. 2012; Saglia et al. 2016). The velocity Although CO discs do not usually extend as far as neutral hydrogen dispersions used for these investigations are usually taken from discs, they have been found to extend to the flat part of the rotation 2021 11 January on guest by https://academic.oup.com/mnras/article/500/2/1933/5935252 from Downloaded spectra integrated within one effective radius (Re), although the curve in 70 per cent of CO-rich ETGs (Davis et al. 2013a), and effects of finite instrumental apertures can affect this scale. they appear≈ to extend in most LTGs (e.g. Leung et al. 2018;Levy Correlations also exist between the SMBH mass and other prop- et al. 2018). The potential at the radii probed by CO, however, is erties of the host galaxy. One of the simplest such properties is still dominated by the stellar component (Cappellari et al. 2013), and the total stellar mass (M ,tot;Davis,Graham&Cameron2018b). thus CO gas does not trace the same halo-dominated potential as H I. ∗ Although originally the total stellar mass (and the disc component in We discuss this in further detail in Section 1.3. late-type galaxies, LTGs) was thought not to correlate with SMBH Nevertheless, Davis, Graham & Combes (2019b) combined the mass (Kormendy & Gebhardt 2001; Kormendy, Bender & Cornell CO TFR of Tiley et al. (2019) with the MBH–M ,tot correlation of ∗ 12.2 2.1 2011), recent works have indicated there is a correlation, albeit Davis et al. (2018b) to yield a prediction of M V ± .For BH ∝ CO one weaker than MBH–σ (e.g. Beifiori et al. 2012;Lasker¨ et al. spiral galaxies, the disc–halo conspiracy enables the replacement of ∗ 2014; Savorgnan & Graham 2016;Mutlu-Pakdiletal.2018) with the CO line widths in the Tiley et al.
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