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dc.contributor.authorDavies, L. J. M.
dc.contributor.authorHuynh, M. T.
dc.contributor.authorHopkins, A. M.
dc.contributor.authorSeymour, N.
dc.contributor.authorDriver, S. P.
dc.contributor.authorRobotham, A. G. R.
dc.contributor.authorBaldry, I. K.
dc.contributor.authorBland-hawthorn, J.
dc.contributor.authorBourne, N.
dc.contributor.authorBremer, M. N.
dc.contributor.authorBrown, M. J. I.
dc.contributor.authorBrough, S.
dc.contributor.authorCluver, M.
dc.contributor.authorGrootes, M. W.
dc.contributor.authorJarvis, M.
dc.contributor.authorLoveday, J.
dc.contributor.authorMoffet, A.
dc.contributor.authorOwers, M.
dc.contributor.authorPhillipps, S.
dc.contributor.authorSadler, E.
dc.contributor.authorWang, L.
dc.contributor.authorWilkins, S.
dc.contributor.authorWright, A.
dc.date.accessioned2017-01-20T17:30:08Z
dc.date.available2017-01-20T17:30:08Z
dc.date.issued2017-04
dc.identifier.citationDavies , L J M , Huynh , M T , Hopkins , A M , Seymour , N , Driver , S P , Robotham , A G R , Baldry , I K , Bland-hawthorn , J , Bourne , N , Bremer , M N , Brown , M J I , Brough , S , Cluver , M , Grootes , M W , Jarvis , M , Loveday , J , Moffet , A , Owers , M , Phillipps , S , Sadler , E , Wang , L , Wilkins , S & Wright , A 2017 , ' Galaxy And Mass Assembly : the 1.4 GHz SFR indicator, SFR-M ★ relation and predictions for ASKAP-GAMA ' , Monthly Notices of the Royal Astronomical Society , vol. 466 , no. 2 , pp. 2312-2324 . https://doi.org/10.1093/mnras/stw3080en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 248191658
dc.identifier.otherPURE UUID: 155233ed-f06c-4f1b-8e2b-1fc14ce668a0
dc.identifier.othercrossref: 10.1093/mnras/stw3080
dc.identifier.otherWOS: 000398284600078
dc.identifier.otherScopus: 85040247507
dc.identifier.urihttp://hdl.handle.net/10023/10139
dc.description.abstractWe present a robust calibration of the 1.4 GHz radio continuum star formation rate (SFR) using a combination of the Galaxy And Mass Assembly (GAMA) survey and the Faint Images of the Radio Sky at Twenty-cm (FIRST) survey. We identify individually detected 1.4 GHz GAMA–FIRST sources and use a late-type, non-active galactic nucleus, volume-limited sample from GAMA to produce stellar mass-selected samples. The latter are then combined to produce FIRST-stacked images. This extends the robust parametrization of the 1.4 GHz–SFR relation to faint luminosities. For both the individually detected galaxies and our stacked samples, we compare 1.4 GHz luminosity to SFRs derived from GAMA to determine a new 1.4 GHz luminosity-to-SFR relation with well-constrained slope and normalization. For the first time, we produce the radio SFR–M* relation over 2 decades in stellar mass, and find that our new calibration is robust, and produces a SFR–M* relation which is consistent with all other GAMA SFR methods. Finally, using our new 1.4 GHz luminosity-to-SFR calibration we make predictions for the number of star-forming GAMA sources which are likely to be detected in the upcoming Australian Square Kilometre Array Pathfinder surveys, Evolutionary Map of the Universe and Deep Investigation of Neutral Gas Origins.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2016, the Author(s). This work has been 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 mnras.oxfordjournals.org / https://doi.org/10.1093/mnras/stw3080en
dc.subjectGalaxies: star formationen
dc.subjectGalaxies: evolutionen
dc.subjectRadiation mechanisms: non-thermalen
dc.subjectRadiation continuum: galaxiesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleGalaxy And Mass Assembly : the 1.4 GHz SFR indicator, SFR-M★ relation and predictions for ASKAP-GAMAen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stw3080
dc.description.statusPeer revieweden


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