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dc.contributor.authorBelfiore, Francesco
dc.contributor.authorMaiolino, Roberto
dc.contributor.authorMaraston, Claudia
dc.contributor.authorEmsellem, Eric
dc.contributor.authorBershady, Matthew A.
dc.contributor.authorMasters, Karen L.
dc.contributor.authorBizyaev, Dmitry
dc.contributor.authorBoquien, Médéric
dc.contributor.authorBrownstein, Joel R.
dc.contributor.authorBundy, Kevin
dc.contributor.authorDiamond-Stanic, Aleksandar M.
dc.contributor.authorDrory, Niv
dc.contributor.authorHeckman, Timothy M.
dc.contributor.authorLaw, David R.
dc.contributor.authorMalanushenko, Olena
dc.contributor.authorOravetz, Audrey
dc.contributor.authorPan, Kaike
dc.contributor.authorRoman-Lopes, Alexandre
dc.contributor.authorThomas, Daniel
dc.contributor.authorWeijmans, Anne-Marie
dc.contributor.authorWestfall, Kyle B.
dc.contributor.authorYan, Renbin
dc.date.accessioned2017-06-14T16:30:12Z
dc.date.available2017-06-14T16:30:12Z
dc.date.issued2017-04
dc.identifier.citationBelfiore , F , Maiolino , R , Maraston , C , Emsellem , E , Bershady , M A , Masters , K L , Bizyaev , D , Boquien , M , Brownstein , J R , Bundy , K , Diamond-Stanic , A M , Drory , N , Heckman , T M , Law , D R , Malanushenko , O , Oravetz , A , Pan , K , Roman-Lopes , A , Thomas , D , Weijmans , A-M , Westfall , K B & Yan , R 2017 , ' SDSS IV MaNGA - the spatially resolved transition from star formation to quiescence ' , Monthly Notices of the Royal Astronomical Society , vol. 466 , no. 3 , pp. 2570-2589 . < https://www.repository.cam.ac.uk/handle/1810/262911 >en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 245780420
dc.identifier.otherPURE UUID: d13b600a-6a43-4d58-a900-e1d586f9cd54
dc.identifier.otherBibCode: 2016arXiv160901737B
dc.identifier.otherScopus: 85018331549
dc.identifier.otherORCID: /0000-0002-5908-6852/work/40233473
dc.identifier.urihttp://hdl.handle.net/10023/10996
dc.descriptionFB, RM and KM acknowledge funding from the United Kingdom Science and Technology Facilities Council (STFC). RM acknowledges support from the European Research Council (ERC) Advanced Grant 695671 ‘QUENCH’. AR-L acknowledges partial support from the DIULS regular project PR15143. MB was supported by NSF/AST-1517006. KB was supported by World Premier International Research Centre Initiative (WPI Initiative), MEXT, Japan and by JSPS KAKENHI Grant Number 15K17603. AW acknowledges support from a Leverhulme Early Career Fellowship. AD acknowledges support from The Grainger Foundation.en
dc.description.abstractUsing spatially resolved spectroscopy from SDSS-IV MaNGA we have demonstrated that low ionization emission-line regions (LIERs) in local galaxies result from photoionization by hot evolved stars, not active galactic nuclei, hence tracing galactic region hosting old stellar population where, despite the presence of ionized gas, star formation is no longer occurring. LIERs are ubiquitous in both quiescent galaxies and in the central regions of galaxies where star formation takes place at larger radii. We refer to these two classes of galaxies as extended LIER (eLIER) and central LIER (cLIER) galaxies, respectively. cLIERs are late-type galaxies primarily spread across the green valley, in the transition region between the star formation main sequence and quiescent galaxies. These galaxies display regular disc rotation in both stars and gas, although featuring a higher central stellar velocity dispersion than star-forming galaxies of the same mass. cLIERs are consistent with being slowly quenched inside-out; the transformation is associated with massive bulges, pointing towards the importance of bulge growth via secular evolution. eLIERs are morphologically early types and are indistinguishable from passive galaxies devoid of line emission in terms of their stellar populations, morphology and central stellar velocity dispersion. Ionized gas in eLIERs shows both disturbed and disc-like kinematics. When a large-scale flow/rotation is observed in the gas, it is often misaligned relative to the stellar component. These features indicate that eLIERs are passive galaxies harbouring a residual cold gas component, acquired mostly via external accretion. Importantly, quiescent galaxies devoid of line emission reside in denser environments and have significantly higher satellite fraction than eLIERs. Environmental effects thus represent the likely cause for the existence of line-less galaxies on the red sequence.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2016 the Authors. This work has been made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stw3211en
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: fundamental parametersen
dc.subjectGalaxies: ISMen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleSDSS IV MaNGA - the spatially resolved transition from star formation to quiescenceen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden
dc.identifier.urlhttps://www.repository.cam.ac.uk/handle/1810/262911en
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2016arXiv160901737Ben


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