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dc.contributor.authorLi, Cheng
dc.contributor.authorWang, Enci
dc.contributor.authorLin, Lin
dc.contributor.authorBershady, Matthew A.
dc.contributor.authorBundy, Kevin
dc.contributor.authorTremonti, Christy A.
dc.contributor.authorXiao, Ting
dc.contributor.authorYan, Renbin
dc.contributor.authorBizyaev, Dmitry
dc.contributor.authorBlanton, Michael
dc.contributor.authorCales, Sabrina
dc.contributor.authorCherinka, Brian
dc.contributor.authorCheung, Edmond
dc.contributor.authorDrory, Niv
dc.contributor.authorEmsellem, Eric
dc.contributor.authorFu, Hai
dc.contributor.authorGelfand, Joseph
dc.contributor.authorLaw, David R.
dc.contributor.authorLin, Lihwai
dc.contributor.authorMacDonald, Nick
dc.contributor.authorMaraston, Claudia
dc.contributor.authorMasters, Karen L.
dc.contributor.authorMerrifield, Michael R.
dc.contributor.authorPan, Kaike
dc.contributor.authorSanchez, S. F.
dc.contributor.authorSchneider, Donald P.
dc.contributor.authorThomas, Daniel
dc.contributor.authorWake, David
dc.contributor.authorWang, Lixin
dc.contributor.authorWeijmans, Anne-Marie
dc.contributor.authorWilkinson, David
dc.contributor.authorYoachim, Peter
dc.contributor.authorZhang, Kai
dc.contributor.authorZheng, Tiantian
dc.date.accessioned2015-03-04T15:31:06Z
dc.date.available2015-03-04T15:31:06Z
dc.date.issued2015-05-11
dc.identifier.citationLi , C , Wang , E , Lin , L , Bershady , M A , Bundy , K , Tremonti , C A , Xiao , T , Yan , R , Bizyaev , D , Blanton , M , Cales , S , Cherinka , B , Cheung , E , Drory , N , Emsellem , E , Fu , H , Gelfand , J , Law , D R , Lin , L , MacDonald , N , Maraston , C , Masters , K L , Merrifield , M R , Pan , K , Sanchez , S F , Schneider , D P , Thomas , D , Wake , D , Wang , L , Weijmans , A-M , Wilkinson , D , Yoachim , P , Zhang , K & Zheng , T 2015 , ' P-MaNGA : gradients in recent star formation histories as diagnostics for galaxy growth and death ' , Astrophysical Journal , vol. 804 , no. 2 . https://doi.org/10.1088/0004-637X/804/2/125en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 172304931
dc.identifier.otherPURE UUID: d0406f7a-29cd-4db3-9ca2-7b1bd8c3e2e0
dc.identifier.otherBibCode: 2015arXiv150207040L
dc.identifier.otherScopus: 84929992642
dc.identifier.otherORCID: /0000-0002-5908-6852/work/40233462
dc.identifier.otherWOS: 000354905000047
dc.identifier.urihttp://hdl.handle.net/10023/6178
dc.descriptionC.L. acknowledges the support of the 100 Talents Program of Chinese Academy of Sciences (CAS). This work is supported by NSFC (11173045, 11233005, 11325314, 11320101002), by the Strategic Priority Research Program "The Emergence of Cosmological Structures" of CAS (grant No. XDB09000000), and by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. We have made use of data from HyperLeda for our work. Funding for SDSS-III and SDSS-IV has been provided by the Alfred P. Sloan Foundation and Participating Institutions. Additional funding for SDSS-III comes from the National Science Foundation and the U.S. Department of Energy Office of Science.en
dc.description.abstractWe present an analysis of the data produced by the MaNGA prototype run (P-MaNGA), aiming to test how the radial gradients in recent star formation histories, as indicated by the 4000AA-break (D4000), Hdelta absorption (EW(Hd_A)) and Halpha emission (EW(Ha)) indices, can be useful for understanding disk growth and star formation cessation in local galaxies. We classify 12 galaxies observed on two P-MaNGA plates as either centrally quiescent (CQ) or centrally star-forming (CSF), according to whether D4000 measured in the central spaxel of each datacube exceeds 1.6. For each galaxy we generate both 2D maps and radial profiles of D4000, EW(Hd_A) and EW(Ha). We find that CSF galaxies generally show very weak or no radial variation in these diagnostics. In contrast, CQ galaxies present significant radial gradients, in the sense that D4000 decreases, while both EW(Hd_A) and EW(Ha) increase from the galactic center outward. The outer regions of the galaxies show greater scatter on diagrams relating the three parameters than their central parts. In particular, the clear separation between centrally-measured quiescent and star-forming galaxies in these diagnostic planes is largely filled in by the outer parts of galaxies whose global colors place them in the green valley, supporting the idea that the green valley represents a transition between blue-cloud and red-sequence phases, at least in our small sample. These results are consistent with a picture in which the cessation of star formation propagates from the center of a galaxy outwards as it moves to the red sequence.
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2015. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at http://dx.doi.org/10.1088/0004-637X/804/2/125en
dc.subjectAstrophysics - Astrophysics of Galaxiesen
dc.subjectAstrophysics - Cosmology and Nongalactic Astrophysicsen
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: formationen
dc.subjectGalaxies: generalen
dc.subjectGalaxies: stellar contenten
dc.subjectMethods: observationalen
dc.subjectSurveysen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleP-MaNGA : gradients in recent star formation histories as diagnostics for galaxy growth and deathen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/804/2/125
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2015arXiv150207040Len


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