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dc.contributor.authorMartin, G.
dc.contributor.authorKaviraj, S.
dc.contributor.authorVolonteri, M.
dc.contributor.authorSimmons, B. D.
dc.contributor.authorDevriendt, J. E. G.
dc.contributor.authorLintott, C. J.
dc.contributor.authorSmethurst, R. J.
dc.contributor.authorDubois, Y.
dc.contributor.authorPichon, C.
dc.date.accessioned2018-06-06T17:08:44Z
dc.date.available2018-06-06T17:08:44Z
dc.date.issued2018-05-11
dc.identifier.citationMartin , G , Kaviraj , S , Volonteri , M , Simmons , B D , Devriendt , J E G , Lintott , C J , Smethurst , R J , Dubois , Y & Pichon , C 2018 , ' Normal black holes in bulge-less galaxies: the largely quiescent, merger-free growth of black holes over cosmic time ' , Monthly Notices of the Royal Astronomical Society , vol. 476 , no. 2 , sty324 , pp. 2801-2812 . https://doi.org/10.1093/mnras/sty324
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 13356042
dc.identifier.otherPURE UUID: 02b5ce26-6b1e-4b0b-8aa1-011e68f7531a
dc.identifier.otherArXiv: http://arxiv.org/abs/1801.09699v2
dc.identifier.otherScopus: 85048010159
dc.identifier.otherORCID: /0000-0002-5601-575X/work/77850192
dc.identifier.urihttp://hdl.handle.net/2299/20144
dc.description© 2018 The Author(s). Published by Oxford University Press on behalf of The Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. (http://creativecommons.org/licenses/by/4.0/).
dc.description.abstractUnderstanding the processes that drive the formation of black holes (BHs) is a key topic in observational cosmology. While the observed M BH-M Bulge correlation in bulge-dominated galaxies is thought to be produced by major mergers, the existence of an M BH-M* relation, across all galaxy morphological types, suggests that BHs may be largely built by secular processes. Recent evidence that bulge-less galaxies, which are unlikely to have had significant mergers, are offset from the M BH-M Bulge relation, but lie on the M BH-M* relation, has strengthened this hypothesis. Nevertheless, the small size and heterogeneity of current data sets, coupled with the difficulty in measuring precise BH masses, make it challenging to address this issue using empirical studies alone. Here, we use Horizon-AGN, a cosmological hydrodynamical simulation to probe the role of mergers in BH growth over cosmic time. We show that (1) as suggested by observations, simulated bulge-less galaxies lie offset from the main M BH-M Bulge relation, but on the M BH-M* relation, (2) the positions of galaxies on the M BH-M* relation are not affected by their merger histories, and (3) only ~35 per cent of the BH mass in today's massive galaxies is directly attributable to merging - the majority (~65 per cent) of BH growth, therefore, takes place gradually, via secular processes, over cosmic time.en
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.subjectGalaxies: evolution
dc.subjectGalaxies: interactions
dc.subjectGalaxies: supermassive black holes
dc.subjectMethods: numerical
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleNormal black holes in bulge-less galaxies: the largely quiescent, merger-free growth of black holes over cosmic timeen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionCentre of Data Innovation Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85048010159&partnerID=8YFLogxK
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2018-05-11
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/sty324
rioxxterms.licenseref.urihttp://creativecommons.org/licenses/by/4.0/
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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