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dc.contributor.authorGuo, Hong
dc.contributor.authorZehavi, Idit
dc.contributor.authorZheng, Zheng
dc.contributor.authorWeinberg, David H.
dc.contributor.authorBerlind, Andreas A.
dc.contributor.authorBlanton, Michael
dc.contributor.authorChen, Yanmei
dc.contributor.authorEisenstein, Daniel J.
dc.contributor.authorHo, Shirley
dc.contributor.authorKazin, Eyal
dc.contributor.authorManera, Marc
dc.contributor.authorMaraston, Claudia
dc.contributor.authorMcBride, Cameron K.
dc.contributor.authorNuza, Sebastián E.
dc.contributor.authorPadmanabhan, Nikhil
dc.contributor.authorParejko, John K.
dc.contributor.authorPercival, Will J.
dc.contributor.authorRoss, Ashley J.
dc.contributor.authorRoss, Nicholas P.
dc.contributor.authorSamushia, Lado
dc.contributor.authorSánchez, Ariel G.
dc.contributor.authorSchlegel, David J.
dc.contributor.authorSchneider, Donald P.
dc.contributor.authorSkibba, Ramin A.
dc.contributor.authorSwanson, Molly E. C.
dc.contributor.authorTinker, Jeremy L.
dc.contributor.authorTojeiro, Rita
dc.contributor.authorWake, David A.
dc.contributor.authorWhite, Martin
dc.contributor.authorBahcall, Neta A.
dc.contributor.authorBizyaev, Dmitry
dc.contributor.authorBrewington, Howard
dc.contributor.authorBundy, Kevin
dc.contributor.authorda Costa, Luiz N. A.
dc.contributor.authorEbelke, Garrett
dc.contributor.authorMalanushenko, Elena
dc.contributor.authorMalanushenko, Viktor
dc.contributor.authorOravetz, Daniel
dc.contributor.authorRossi, Graziano
dc.contributor.authorSimmons, Audrey
dc.contributor.authorSnedden, Stephanie
dc.contributor.authorStreblyanska, Alina
dc.contributor.authorThomas, Daniel
dc.date.accessioned2018-10-17T14:30:13Z
dc.date.available2018-10-17T14:30:13Z
dc.date.issued2013-04-04
dc.identifier.citationGuo , H , Zehavi , I , Zheng , Z , Weinberg , D H , Berlind , A A , Blanton , M , Chen , Y , Eisenstein , D J , Ho , S , Kazin , E , Manera , M , Maraston , C , McBride , C K , Nuza , S E , Padmanabhan , N , Parejko , J K , Percival , W J , Ross , A J , Ross , N P , Samushia , L , Sánchez , A G , Schlegel , D J , Schneider , D P , Skibba , R A , Swanson , M E C , Tinker , J L , Tojeiro , R , Wake , D A , White , M , Bahcall , N A , Bizyaev , D , Brewington , H , Bundy , K , da Costa , L N A , Ebelke , G , Malanushenko , E , Malanushenko , V , Oravetz , D , Rossi , G , Simmons , A , Snedden , S , Streblyanska , A & Thomas , D 2013 , ' The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey : luminosity and color dependence and redshift evolution ' , Astrophysical Journal , vol. 767 , no. 2 , 122 . https://doi.org/10.1088/0004-637X/767/2/122en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 171421302
dc.identifier.otherPURE UUID: f495f86b-83ec-4433-a766-f39b0214105a
dc.identifier.otherBibCode: 2013ApJ...767..122G
dc.identifier.otherScopus: 84876104958
dc.identifier.urihttp://hdl.handle.net/10023/16262
dc.description.abstractWe measure the luminosity and color dependence and the redshift evolution of galaxy clustering in the Sloan Digital Sky Survey-III Baryon Oscillation Spectroscopic Survey Ninth Data Release. We focus on the projected two-point correlation function (2PCF) of subsets of its CMASS sample, which includes about 260,000 galaxies over ~3300 deg2 in the redshift range 0.43 < z < 0.7. To minimize the selection effect on galaxy clustering, we construct well-defined luminosity and color subsamples by carefully accounting for the CMASS galaxy selection cuts. The 2PCF of the whole CMASS sample, if approximated by a power-law, has a correlation length of r 0 = 7.93 ± 0.06 h –1 Mpc and an index of γ = 1.85 ± 0.01. Clear dependences on galaxy luminosity and color are found for the projected 2PCF in all redshift bins, with more luminous and redder galaxies generally exhibiting stronger clustering and steeper 2PCF. The color dependence is also clearly seen for galaxies within the red sequence, consistent with the behavior of SDSS-II main sample galaxies at lower redshifts. At a given luminosity (k + e corrected), no significant evolution of the projected 2PCFs with redshift is detected for red sequence galaxies. We also construct galaxy samples of fixed number density at different redshifts, using redshift-dependent magnitude thresholds. The clustering of these galaxies in the CMASS redshift range is found to be consistent with that predicted by passive evolution. Our measurements of the luminosity and color dependence and redshift evolution of galaxy clustering will allow for detailed modeling of the relation between galaxies and dark matter halos and new constraints on galaxy formation and evolution.
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2013. The American Astronomical Society. All rights reserved. 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/10.1088/0004-637X/767/2/122en
dc.subjectCosmology: observationsen
dc.subjectCosmology: theoryen
dc.subjectGalaxies: distances and redshiftsen
dc.subjectGalaxies: halosen
dc.subjectGalaxies: statisticsen
dc.subjectLarge-scale structure of Universeen
dc.subjectQB Astronomyen
dc.subject.lccQBen
dc.titleThe clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey : luminosity and color dependence and redshift evolutionen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/767/2/122
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2013ApJ...767..122Gen


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