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dc.contributor.authorAlam, Shadab
dc.contributor.authorAta, Metin
dc.contributor.authorBailey, Stephen
dc.contributor.authorBeutler, Florian
dc.contributor.authorBizyaev, Dmitry
dc.contributor.authorBlazek, Jonathan A.
dc.contributor.authorBolton, Adam S.
dc.contributor.authorBrownstein, Joel R.
dc.contributor.authorBurden, Angela
dc.contributor.authorChuang, Chia-Hsun
dc.contributor.authorComparat, Johan
dc.contributor.authorCuesta, Antonio J.
dc.contributor.authorDawson, Kyle S.
dc.contributor.authorEisenstein, Daniel J.
dc.contributor.authorEscoffier, Stephanie
dc.contributor.authorGil-Marín, Héctor
dc.contributor.authorGrieb, Jan Niklas
dc.contributor.authorHand, Nick
dc.contributor.authorHo, Shirley
dc.contributor.authorKinemuchi, Karen
dc.contributor.authorKirkby, David
dc.contributor.authorKitaura, Francisco
dc.contributor.authorMalanushenko, Elena
dc.contributor.authorMalanushenko, Viktor
dc.contributor.authorMaraston, Claudia
dc.contributor.authorMcBride, Cameron K.
dc.contributor.authorNichol, Robert C.
dc.contributor.authorOlmstead, Matthew D.
dc.contributor.authorOravetz, Daniel
dc.contributor.authorPadmanabhan, Nikhil
dc.contributor.authorPalanque-Delabrouille, Nathalie
dc.contributor.authorPan, Kaike
dc.contributor.authorPellejero-Ibanez, Marcos
dc.contributor.authorPercival, Will J.
dc.contributor.authorPetitjean, Patrick
dc.contributor.authorPrada, Francisco
dc.contributor.authorPrice-Whelan, Adrian M.
dc.contributor.authorReid, Beth A.
dc.contributor.authorRodríguez-Torres, Sergio A.
dc.contributor.authorRoe, Natalie A.
dc.contributor.authorRoss, Ashley J.
dc.contributor.authorRoss, Nicholas P.
dc.contributor.authorRossi, Graziano
dc.contributor.authorRubiño-Martín, Jose Alberto
dc.contributor.authorSaito, Shun
dc.contributor.authorSalazar-Albornoz, Salvador
dc.contributor.authorSamushia, Lado
dc.contributor.authorSánchez, Ariel G.
dc.contributor.authorSatpathy, Siddharth
dc.contributor.authorSchlegel, David J.
dc.contributor.authorSchneider, Donald P.
dc.contributor.authorScóccola, Claudia G.
dc.contributor.authorSeo, Hee-Jong
dc.contributor.authorSheldon, Erin S.
dc.contributor.authorSimmons, Audrey
dc.contributor.authorSlosar, Anže
dc.contributor.authorStrauss, Michael A.
dc.contributor.authorSwanson, Molly E. C.
dc.contributor.authorThomas, Daniel
dc.contributor.authorTinker, Jeremy L.
dc.contributor.authorTojeiro, Rita
dc.contributor.authorVargas Magaña, Mariana
dc.contributor.authorVazquez, Jose Alberto
dc.contributor.authorVerde, Licia
dc.contributor.authorWake, David A.
dc.contributor.authorWang, Yuting
dc.contributor.authorWeinberg, David H.
dc.contributor.authorWhite, Martin
dc.contributor.authorWood-Vasey, W. Michael
dc.contributor.authorYèche, Christophe
dc.contributor.authorZehavi, Idit
dc.contributor.authorZhai, Zhongxu
dc.contributor.authorZhao, Gong-Bo
dc.identifier.citationAlam , S , Ata , M , Bailey , S , Beutler , F , Bizyaev , D , Blazek , J A , Bolton , A S , Brownstein , J R , Burden , A , Chuang , C-H , Comparat , J , Cuesta , A J , Dawson , K S , Eisenstein , D J , Escoffier , S , Gil-Marín , H , Grieb , J N , Hand , N , Ho , S , Kinemuchi , K , Kirkby , D , Kitaura , F , Malanushenko , E , Malanushenko , V , Maraston , C , McBride , C K , Nichol , R C , Olmstead , M D , Oravetz , D , Padmanabhan , N , Palanque-Delabrouille , N , Pan , K , Pellejero-Ibanez , M , Percival , W J , Petitjean , P , Prada , F , Price-Whelan , A M , Reid , B A , Rodríguez-Torres , S A , Roe , N A , Ross , A J , Ross , N P , Rossi , G , Rubiño-Martín , J A , Saito , S , Salazar-Albornoz , S , Samushia , L , Sánchez , A G , Satpathy , S , Schlegel , D J , Schneider , D P , Scóccola , C G , Seo , H-J , Sheldon , E S , Simmons , A , Slosar , A , Strauss , M A , Swanson , M E C , Thomas , D , Tinker , J L , Tojeiro , R , Vargas Magaña , M , Vazquez , J A , Verde , L , Wake , D A , Wang , Y , Weinberg , D H , White , M , Wood-Vasey , W M , Yèche , C , Zehavi , I , Zhai , Z & Zhao , G-B 2017 , ' The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey : cosmological analysis of the DR12 galaxy sample ' , Monthly Notices of the Royal Astronomical Society , vol. 470 , no. 3 , pp. 2617-2652 .
dc.identifier.otherPURE: 250036635
dc.identifier.otherPURE UUID: df3184f9-b0ba-4a59-ba6f-76a72e9f7587
dc.identifier.otherBibCode: 2016arXiv160703155A
dc.identifier.otherScopus: 85023742631
dc.identifier.otherWOS: 000406844800008
dc.descriptionRT acknowledges support from the Science and Technology Facilities Council via an Ernest Rutherford Fellowship (grant number ST/K004719/1).en
dc.description.abstractWe present cosmological results from the final galaxy clustering data set of the Baryon Oscillation Spectroscopic Survey, part of the Sloan Digital Sky Survey III. Our combined galaxy sample comprises 1.2 million massive galaxies over an effective area of 9329 deg2 and volume of 18.7 Gpc3, divided into three partially overlapping redshift slices centred at effective redshifts 0.38, 0.51, and 0.61. We measure the angular diameter distance DM and Hubble parameter H from the baryon acoustic oscillation (BAO) method, in combination with a cosmic microwave background prior on the sound horizon scale after applying reconstruction to reduce non-linear effects on the BAO feature. Using the anisotropic clustering of the pre-reconstruction density field, we measure the product DMH from the Alcock-Paczynski (AP) effect and the growth of structure, quantified by ƒσ8(z), from redshift-space distortions (RSD). We combine individual measurements presented in seven companion papers into a set of consensus values and likelihoods, obtaining constraints that are tighter and more robust than those from any one method; in particular, the AP measurement from sub-BAO scales sharpens constraints from post-reconstruction BAOs by breaking degeneracy between DM and H. Combined with Planck 2016 cosmic microwave background measurements, our distance scale measurements simultaneously imply curvature ΩK = 0.0003 ± 0.0026 and a dark energy equation of state parameter w = −1.01 ± 0.06, in strong affirmation of the spatially flat cold dark matter (CDM) model with a cosmological constant (ΛCDM). Our RSD measurements of ƒσ8, at 6 per cent precision, are similarly consistent with this model. When combined with supernova Ia data, we find H0 = 67.3 ± 1.0 km s−1 Mpc−1 even for our most general dark energy model, in tension with some direct measurements. Adding extra relativistic species as a degree of freedom loosens the constraint only slightly, to H0 = 67.8 ± 1.2 km s−1 Mpc−1. Assuming flat ΛCDM we find Ωm = 0.310 ± 0.005 and H0 = 67.6 ± 0.5 km s−1 Mpc−1, and we find a 95 per cent upper limit of 0.16 eV/c-2 on the neutrino mass sum.
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2017, the Author(s). 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
dc.subjectDistance scaleen
dc.subjectLarge-scale structure of Universeen
dc.subjectCosmology: observationsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleThe clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey : cosmological analysis of the DR12 galaxy sampleen
dc.typeJournal articleen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.description.statusPeer revieweden

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