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dc.contributor.authorTojeiro, R.
dc.contributor.authorPercival, W. J.
dc.contributor.authorBrinkmann, J.
dc.contributor.authorBrownstein, J. R.
dc.contributor.authorEisenstein, D. J.
dc.contributor.authorManera, M.
dc.contributor.authorMaraston, C.
dc.contributor.authorMcBride, C. K.
dc.contributor.authorMuna, D.
dc.contributor.authorReid, B.
dc.contributor.authorRoss, A. J.
dc.contributor.authorRoss, N. P.
dc.contributor.authorSamushia, L.
dc.contributor.authorPadmanabhan, N.
dc.contributor.authorSchneider, D. P.
dc.contributor.authorSkibba, R.
dc.contributor.authorSánchez, A. G.
dc.contributor.authorSwanson, M. E. C.
dc.contributor.authorThomas, D.
dc.contributor.authorTinker, J. L.
dc.contributor.authorVerde, L.
dc.contributor.authorWake, D. A.
dc.contributor.authorWeaver, B. A.
dc.contributor.authorZhao, G.-B.
dc.identifier.citationTojeiro , R , Percival , W J , Brinkmann , J , Brownstein , J R , Eisenstein , D J , Manera , M , Maraston , C , McBride , C K , Muna , D , Reid , B , Ross , A J , Ross , N P , Samushia , L , Padmanabhan , N , Schneider , D P , Skibba , R , Sánchez , A G , Swanson , M E C , Thomas , D , Tinker , J L , Verde , L , Wake , D A , Weaver , B A & Zhao , G-B 2012 , ' The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey : measuring structure growth using passive galaxies ' , Monthly Notices of the Royal Astronomical Society , vol. 424 , no. 3 , pp. 2339-2344 .
dc.identifier.otherPURE: 252559671
dc.identifier.otherPURE UUID: c2fdc2f2-bced-41d8-8f23-8e0605c63de4
dc.identifier.otherBibtex: urn:bafcca6ae6327f3a55c4bb5aadced830
dc.identifier.otherScopus: 84864518558
dc.description.abstractWe explore the benefits of using a passively evolving population of galaxies to measure the evolution of the rate of structure growth between z = 0.25 and 0.65 by combining data from the Sloan Digital Sky Survey (SDSS) I/II and SDSS-III surveys. The large-scale linear bias of a population of dynamically passive galaxies, which we select from both surveys, is easily modelled. Knowing the bias evolution breaks degeneracies inherent to other methodologies, and decreases the uncertainty in measurements of the rate of structure growth and the normalization of the galaxy power spectrum by up to a factor of 2. If we translate our measurements into a constraint on σ8(z = 0) assuming a concordance cosmological model and general relativity (GR), we find that using a bias model improves our uncertainty by a factor of nearly 1.5. Our results are consistent with a flat Λ cold dark matter model and with GR.
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2012 The Authors, Monthly Notices of the Royal Astronomical Society © 2012 RAS. This work has been made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at
dc.subjectCosmology: observationsen
dc.subjectDark energyen
dc.subjectLarge-scale structure of Universeen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleThe clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey : measuring structure growth using passive galaxiesen
dc.typeJournal articleen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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