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dc.contributor.authorParejko, John K.
dc.contributor.authorSunayama, Tomomi
dc.contributor.authorPadmanabhan, Nikhil
dc.contributor.authorWake, David A.
dc.contributor.authorBerlind, Andreas A.
dc.contributor.authorBizyaev, Dmitry
dc.contributor.authorBlanton, Michael
dc.contributor.authorBolton, Adam S.
dc.contributor.authorvan den Bosch, Frank
dc.contributor.authorBrinkmann, Jon
dc.contributor.authorBrownstein, Joel R.
dc.contributor.authorda Costa, Luiz Alberto Nicolaci
dc.contributor.authorEisenstein, Daniel J.
dc.contributor.authorGuo, Hong
dc.contributor.authorKazin, Eyal
dc.contributor.authorMaia, Marcio
dc.contributor.authorMalanushenko, Elena
dc.contributor.authorMaraston, Claudia
dc.contributor.authorMcBride, Cameron K.
dc.contributor.authorNichol, Robert C.
dc.contributor.authorOravetz, Daniel J.
dc.contributor.authorPan, Kaike
dc.contributor.authorPercival, Will J.
dc.contributor.authorPrada, Francisco
dc.contributor.authorRoss, Ashley J.
dc.contributor.authorRoss, Nicholas P.
dc.contributor.authorSchlegel, David J.
dc.contributor.authorSchneider, Don
dc.contributor.authorSimmons, Audrey E.
dc.contributor.authorSkibba, Ramin
dc.contributor.authorTinker, Jeremy
dc.contributor.authorTojeiro, Rita
dc.contributor.authorWeaver, Benjamin A.
dc.contributor.authorWetzel, Andrew
dc.contributor.authorWhite, Martin
dc.contributor.authorWeinberg, David H.
dc.contributor.authorThomas, Daniel
dc.contributor.authorZehavi, Idit
dc.contributor.authorZheng, Zheng
dc.date.accessioned2018-10-17T15:30:24Z
dc.date.available2018-10-17T15:30:24Z
dc.date.issued2013-02-11
dc.identifier.citationParejko , J K , Sunayama , T , Padmanabhan , N , Wake , D A , Berlind , A A , Bizyaev , D , Blanton , M , Bolton , A S , van den Bosch , F , Brinkmann , J , Brownstein , J R , da Costa , L A N , Eisenstein , D J , Guo , H , Kazin , E , Maia , M , Malanushenko , E , Maraston , C , McBride , C K , Nichol , R C , Oravetz , D J , Pan , K , Percival , W J , Prada , F , Ross , A J , Ross , N P , Schlegel , D J , Schneider , D , Simmons , A E , Skibba , R , Tinker , J , Tojeiro , R , Weaver , B A , Wetzel , A , White , M , Weinberg , D H , Thomas , D , Zehavi , I & Zheng , Z 2013 , ' The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey : the low-redshift sample ' , Monthly Notices of the Royal Astronomical Society , vol. 429 , no. 1 , pp. 98-112 . https://doi.org/10.1093/mnras/sts314en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 171421648
dc.identifier.otherPURE UUID: 6f81b30f-7791-4b7e-8c23-11cffc3244d0
dc.identifier.otherBibCode: 2013MNRAS.429...98P
dc.identifier.otherScopus: 84873901046
dc.identifier.urihttp://hdl.handle.net/10023/16267
dc.description.abstractWe report on the small-scale (0.5 <r <40 h-1 Mpc)clustering of 78 895 massive (M* ˜ 1011.3M⊙) galaxies at 0.2 <z <0.4 from the first twoyears of data from the Baryon Oscillation Spectroscopic Survey (BOSS),to be released as part of Sloan Digital Sky Survey (SDSS) Data Release 9(DR9). We describe the sample selection, basic properties of thegalaxies and caveats for working with the data. We calculate the real-and redshift-space two-point correlation functions of these galaxies,fit these measurements using halo occupation distribution (HOD)modelling within dark matter cosmological simulations, and estimate theerrors using mock catalogues. These galaxies lie in massive haloes, witha mean halo mass of 5.2 × 1013 h-1M⊙, a large-scale bias of ˜2.0 and a satellitefraction of 12 ± 2 per cent. Thus, these galaxies occupy haloeswith average masses in between those of the higher redshift BOSS CMASSsample and the original SDSS I/II luminous red galaxy sample.We report on the small-scale (0.5 < r < 40 h−1 Mpc) clustering of 78 895 massive (M* ∼ 1011.3 M⊙) galaxies at 0.2 < z < 0.4 from the first two years of data from the Baryon Oscillation Spectroscopic Survey (BOSS), to be released as part of Sloan Digital Sky Survey (SDSS) Data Release 9 (DR9). We describe the sample selection, basic properties of the galaxies and caveats for working with the data. We calculate the real- and redshift-space two-point correlation functions of these galaxies, fit these measurements using halo occupation distribution (HOD) modelling within dark matter cosmological simulations, and estimate the errors using mock catalogues. These galaxies lie in massive haloes, with a mean halo mass of 5.2 × 1013 h−1 M⊙, a large-scale bias of ∼2.0 and a satellite fraction of 12 ± 2 per cent. Thus, these galaxies occupy haloes with average masses in between those of the higher redshift BOSS CMASS sample and the original SDSS I/II luminous red galaxy sample.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://doi.org/10.1093/mnras/sts314en
dc.subjectLarge-scale structure of Universeen
dc.subjectGalaxies: haloesen
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: statisticsen
dc.subjectSurveysen
dc.subjectQB Astronomyen
dc.subject.lccQBen
dc.titleThe clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey : the low-redshift sampleen
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/sts314
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2013MNRAS.429...98Pen


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