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dc.contributor.authorScott, Nicholas
dc.contributor.authorvan de Sande, Jesse
dc.contributor.authorCroom, Scott M.
dc.contributor.authorGroves, Brent
dc.contributor.authorOwers, Matt S.
dc.contributor.authorPoetrodjojo, Henry
dc.contributor.authorD'Eugenio, Francesco
dc.contributor.authorMedling, Anne M.
dc.contributor.authorBarat, Dilyar
dc.contributor.authorBarone, Tania M.
dc.contributor.authorBland-Hawthorn, Joss
dc.contributor.authorBrough, Sarah
dc.contributor.authorBryant, Julia
dc.contributor.authorCortese, Luca
dc.contributor.authorFoster, Caroline
dc.contributor.authorGreen, Andrew W.
dc.contributor.authorOh, Sree
dc.contributor.authorColless, Matthew
dc.contributor.authorDrinkwater, Michael J.
dc.contributor.authorDriver, Simon P.
dc.contributor.authorGoodwin, Michael
dc.contributor.authorGunawardhana, Madusha L. P.
dc.contributor.authorFederrath, Christoph
dc.contributor.authorHarischandra, Lloyd
dc.contributor.authorJin, Yifei
dc.contributor.authorLawrence, J. S.
dc.contributor.authorLorente, Nuria P.
dc.contributor.authorMannering, Elizabeth
dc.contributor.authorO'Toole, Simon
dc.contributor.authorRichards, Samuel N.
dc.contributor.authorSanchez, Sebastian F.
dc.contributor.authorSchaefer, Adam L.
dc.contributor.authorSealey, Katrina
dc.contributor.authorSharp, Rob
dc.contributor.authorSweet, Sarah M.
dc.contributor.authorTaranu, Dan S.
dc.contributor.authorVaridel, Mathew
dc.date.accessioned2019-10-16T08:30:07Z
dc.date.available2019-10-16T08:30:07Z
dc.date.issued2018-12
dc.identifier.citationScott , N , van de Sande , J , Croom , S M , Groves , B , Owers , M S , Poetrodjojo , H , D'Eugenio , F , Medling , A M , Barat , D , Barone , T M , Bland-Hawthorn , J , Brough , S , Bryant , J , Cortese , L , Foster , C , Green , A W , Oh , S , Colless , M , Drinkwater , M J , Driver , S P , Goodwin , M , Gunawardhana , M L P , Federrath , C , Harischandra , L , Jin , Y , Lawrence , J S , Lorente , N P , Mannering , E , O'Toole , S , Richards , S N , Sanchez , S F , Schaefer , A L , Sealey , K , Sharp , R , Sweet , S M , Taranu , D S & Varidel , M 2018 , ' The SAMI Galaxy Survey : Data Release Two with absorption-line physics value-added products ' , Monthly Notices of the Royal Astronomical Society , vol. 481 , no. 2 , pp. 2299–2319 . https://doi.org/10.1093/mnras/sty2355en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 261905669
dc.identifier.otherPURE UUID: 34064031-4da6-41b6-815c-e3976c6c8cde
dc.identifier.otherArXiv: http://arxiv.org/abs/1808.03365v2
dc.identifier.otherScopus: 85058994697
dc.identifier.urihttp://hdl.handle.net/10023/18682
dc.descriptionThe data can be accessed via Australian Astronomical Optics' Data Central service (https://datacentral.org.au/)en
dc.description.abstractWe present the second major release of data from the Sydney – Australian Astronomical Observatory Multi-Object Integral Field Spectrograph (SAMI) Galaxy Survey. Data Release Two includes data for 1559 galaxies, about 50 per cent of the full survey. Galaxies included have a redshift range 0.004 < z < 0.113 and a large stellar mass range 7.5 < log (M⋆/M⊙) < 11.6. The core data for each galaxy consist of two primary spectral cubes covering the blue and red optical wavelength ranges. For each primary cube, we also provide three spatially binned spectral cubes and a set of standardized aperture spectra. For each core data product, we provide a set of value-added data products. This includes all emission line value-added products from Data Release One, expanded to the larger sample. In addition, we include stellar kinematic and stellar population value-added products derived from absorption line measurements. The data are provided online through Australian Astronomical Optics’ Data Central. We illustrate the potential of this release by presenting the distribution of ∼350000 stellar velocity dispersion measurements from individual spaxels as a function of R/Re, divided in four galaxy mass bins. In the highest stellar mass bin [log (M⋆/M⊙) > 11], the velocity dispersion strongly increases towards the centre, whereas below log (M⋆/M⊙) < 10 we find no evidence for a clear increase in the central velocity dispersion. This suggests a transition mass around log (M⋆/M⊙) ∼ 10 for galaxies with or without a dispersion-dominated bulge.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/sty2355en
dc.subjectGalaxies: abundancesen
dc.subjectGalaxies: generalen
dc.subjectGalaxies: kinematics and dynamicsen
dc.subjectGalaxies: star formationen
dc.subjectGalaxies: stellar contenten
dc.subjectastronomical data bases: surveysen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe SAMI Galaxy Survey : Data Release Two with absorption-line physics value-added productsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/sty2355
dc.description.statusPeer revieweden
dc.identifier.urlhttp://arxiv.org/abs/1808.03365en


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