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dc.contributor.authorYan, Renbin
dc.contributor.authorBundy, Kevin
dc.contributor.authorLaw, David R.
dc.contributor.authorBershady, Matthew A.
dc.contributor.authorAndrews, Brett
dc.contributor.authorCherinka, Brian
dc.contributor.authorDiamond-Stanic, Aleksandar M.
dc.contributor.authorDrory, Niv
dc.contributor.authorMacDonald, Nicholas
dc.contributor.authorSánchez-Gallego, José R.
dc.contributor.authorThomas, Daniel
dc.contributor.authorWake, David A.
dc.contributor.authorWeijmans, Anne-Marie
dc.contributor.authorWestfall, Kyle B.
dc.contributor.authorZhang, Kai
dc.contributor.authorAragón-Salamanca, Alfonso
dc.contributor.authorBelfiore, Francesco
dc.contributor.authorBizyaev, Dmitry
dc.contributor.authorBlanc, Guillermo A.
dc.contributor.authorBlanton, Michael R.
dc.contributor.authorBrownstein, Joel
dc.contributor.authorCappellari, Michele
dc.contributor.authorD'Souza, Richard
dc.contributor.authorEmsellem, Eric
dc.contributor.authorFu, Hai
dc.contributor.authorGaulme, Patrick
dc.contributor.authorGraham, Mark T.
dc.contributor.authorGoddard, Daniel
dc.contributor.authorGunn, James E.
dc.contributor.authorHarding, Paul
dc.contributor.authorJones, Amy
dc.contributor.authorKinemuchi, Karen
dc.contributor.authorLi, Cheng
dc.contributor.authorLi, Hongyu
dc.contributor.authorMaiolino, Roberto
dc.contributor.authorMao, Shude
dc.contributor.authorMaraston, Claudia
dc.contributor.authorMasters, Karen
dc.contributor.authorMerrifield, Michael R.
dc.contributor.authorOravetz, Daniel
dc.contributor.authorPan, Kaike
dc.contributor.authorParejko, John K.
dc.contributor.authorSanchez, Sebastian F.
dc.contributor.authorSchlegel, David
dc.contributor.authorSimmons, Audrey
dc.contributor.authorThanjavur, Karun
dc.contributor.authorTinker, Jeremy
dc.contributor.authorTremonti, Christy
dc.contributor.authorvan den Bosch, Remco
dc.contributor.authorZheng, Zheng
dc.date.accessioned2016-09-12T11:30:18Z
dc.date.available2016-09-12T11:30:18Z
dc.date.issued2016-11-29
dc.identifier.citationYan , R , Bundy , K , Law , D R , Bershady , M A , Andrews , B , Cherinka , B , Diamond-Stanic , A M , Drory , N , MacDonald , N , Sánchez-Gallego , J R , Thomas , D , Wake , D A , Weijmans , A-M , Westfall , K B , Zhang , K , Aragón-Salamanca , A , Belfiore , F , Bizyaev , D , Blanc , G A , Blanton , M R , Brownstein , J , Cappellari , M , D'Souza , R , Emsellem , E , Fu , H , Gaulme , P , Graham , M T , Goddard , D , Gunn , J E , Harding , P , Jones , A , Kinemuchi , K , Li , C , Li , H , Maiolino , R , Mao , S , Maraston , C , Masters , K , Merrifield , M R , Oravetz , D , Pan , K , Parejko , J K , Sanchez , S F , Schlegel , D , Simmons , A , Thanjavur , K , Tinker , J , Tremonti , C , van den Bosch , R & Zheng , Z 2016 , ' SDSS-IV MaNGA IFS Galaxy Survey - survey design, execution, and initial data quality ' , Astrophysical Journal , vol. 152 , no. 6 , 197 . https://doi.org/10.3847/0004-6256/152/6/197en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 245028255
dc.identifier.otherPURE UUID: 228ed70e-2e0b-49af-85fd-ff080b071f91
dc.identifier.otherBibCode: 2016arXiv160708613Y
dc.identifier.otherScopus: 85009135158
dc.identifier.otherORCID: /0000-0002-5908-6852/work/40233475
dc.identifier.otherWOS: 000396039500001
dc.identifier.urihttp://hdl.handle.net/10023/9476
dc.description.abstractThe MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy (IFS) for 10K nearby galaxies at a spectral resolution of R~2000 from 3,622-10,354Å. The design of the survey is driven by a set of science requirements on the precision of estimates of the following properties: star formation rate surface density, gas metallicity, stellar population age, metallicity, and abundance ratio, and their gradients; stellar and gas kinematics; and enclosed gravitational mass as a function of radius. We describe how these science requirements set the depth of the observations and dictate sample selection. The majority of targeted galaxies are selected to ensure uniform spatial coverage in units of effective radius (Re) while maximizing spatial resolution. About 2/3 of the sample is covered out to 1.5Re (Primary sample), and 1/3 of the sample is covered to 2.5Re (Secondary sample). We describe the survey execution with details that would be useful in the design of similar future surveys. We also present statistics on the achieved data quality, specifically, the point spread function, sampling uniformity, spectral resolution, sky subtraction, and flux calibration. For our Primary sample, the median r-band signal-to-noise ratio is ~73 per 1.4Å pixel for spectra stacked between 1-1.5 Re. Measurements of various galaxy properties from the first year data show that we are meeting or exceeding the defined requirements for the majority of our science goals.
dc.format.extent32
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2016, American Astronomical Society. 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 iopscience.iop.org / https://dx.doi.org/10.3847/0004-6256/152/6/197en
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: generalen
dc.subjectSurveysen
dc.subjectTechniques: imaging spectroscopyen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleSDSS-IV MaNGA IFS Galaxy Survey - survey design, execution, and initial data qualityen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.3847/0004-6256/152/6/197
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2016arXiv160708613Yen


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