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dc.contributor.authorWake, David A.
dc.contributor.authorBundy, Kevin
dc.contributor.authorDiamond-Stanic, Aleksandar M.
dc.contributor.authorYan, Renbin
dc.contributor.authorBlanton, Michael R.
dc.contributor.authorBershady, Matthew A.
dc.contributor.authorSánchez-Gallego, José R.
dc.contributor.authorDrory, Niv
dc.contributor.authorJones, Amy
dc.contributor.authorKauffmann, Guinevere
dc.contributor.authorLaw, David R.
dc.contributor.authorLi, Cheng
dc.contributor.authorMacDonald, Nicholas
dc.contributor.authorMasters, Karen
dc.contributor.authorThomas, Daniel
dc.contributor.authorTinker, Jeremy
dc.contributor.authorWeijmans, Anne-Marie
dc.contributor.authorBrownstein, Joel R.
dc.date.accessioned2017-08-11T11:30:30Z
dc.date.available2017-08-11T11:30:30Z
dc.date.issued2017-09
dc.identifier.citationWake , D A , Bundy , K , Diamond-Stanic , A M , Yan , R , Blanton , M R , Bershady , M A , Sánchez-Gallego , J R , Drory , N , Jones , A , Kauffmann , G , Law , D R , Li , C , MacDonald , N , Masters , K , Thomas , D , Tinker , J , Weijmans , A-M & Brownstein , J R 2017 , ' The SDSS-IV MaNGA sample : design, optimization, and usage considerations ' , Astronomical Journal , vol. 154 , no. 3 , 86 . https://doi.org/10.3847/1538-3881/aa7eccen
dc.identifier.issn0004-6256
dc.identifier.otherPURE: 250524405
dc.identifier.otherPURE UUID: 6bc7da6b-d10b-477d-b733-bc3805a99407
dc.identifier.otherBibCode: 2017arXiv170702989W
dc.identifier.otherScopus: 85029032343
dc.identifier.otherORCID: /0000-0002-5908-6852/work/40233460
dc.identifier.otherWOS: 000410574100004
dc.identifier.urihttps://hdl.handle.net/10023/11429
dc.description.abstractWe describe the sample design for the SDSS-IV MaNGA survey and present the final properties of the main samples along with important considerations for using these samples for science. Our target selection criteria were developed while simultaneously optimizing the size distribution of the MaNGA integral field units (IFUs), the IFU allocation strategy, and the target density to produce a survey defined in terms of maximizing S/N, spatial resolution, and sample size. Our selection strategy makes use of redshift limits that only depend oni-band absolute magnitude (Mi), or, for a small subset of our sample, Mi and color (NUV-i). Such a strategy ensures that all galaxies span the same range in angular size irrespective of luminosity and are therefore covered evenly by the adopted range of IFU sizes. We define three samples: the Primary and Secondary samples are selected to have a flat number density with respect to Mi and are targeted to have spectroscopic coverage to 1.5 and 2.5 effective radii (Re),respectively. The Color-Enhanced supplement increases the number of galaxies in the low-density regions of color-magnitude space by extending the redshift limits of the Primary sample in the appropriate color bins. The samples cover the stellar mass range 5 x 108 ≤ M⋆ ≤ 3 x 1011 M⊙ /h2 and are sampled at median physical resolutions of 1.37 kpc and 2.5 kpc for the Primary and Secondary samples respectively. We provide weights that will statistically correct for our luminosity and color-dependent selection function and IFU allocation strategy, thus correcting the observed sample to a volume limited sample.
dc.format.extent26
dc.language.isoeng
dc.relation.ispartofAstronomical Journalen
dc.rights© 2017, American Astronomical Society. 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 iopscience.iop.org / https://doi.org/10.3847/1538-3881/aa7eccen
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: generalen
dc.subjectGalaxies: statisticsen
dc.subjectSurveysen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe SDSS-IV MaNGA sample : design, optimization, and usage considerationsen
dc.typeJournal articleen
dc.contributor.sponsorThe Leverhulme Trusten
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.3847/1538-3881/aa7ecc
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2017arXiv170702989Wen
dc.identifier.grantnumberECF-2014-767en


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