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dc.contributor.authorZhao, Gong-Bo
dc.contributor.authorSaito, Shun
dc.contributor.authorPercival, Will J.
dc.contributor.authorRoss, Ashley J.
dc.contributor.authorMontesano, Francesco
dc.contributor.authorViel, Matteo
dc.contributor.authorSchneider, Donald P.
dc.contributor.authorManera, Marc
dc.contributor.authorMiralda-Escudé, Jordi
dc.contributor.authorPalanque-Delabrouille, Nathalie
dc.contributor.authorRoss, Nicholas P.
dc.contributor.authorSamushia, Lado
dc.contributor.authorSánchez, Ariel G.
dc.contributor.authorSwanson, Molly E. C.
dc.contributor.authorThomas, Daniel
dc.contributor.authorTojeiro, Rita
dc.contributor.authorYèche, Christophe
dc.contributor.authorYork, Donald G.
dc.identifier.citationZhao , G-B , Saito , S , Percival , W J , Ross , A J , Montesano , F , Viel , M , Schneider , D P , Manera , M , Miralda-Escudé , J , Palanque-Delabrouille , N , Ross , N P , Samushia , L , Sánchez , A G , Swanson , M E C , Thomas , D , Tojeiro , R , Yèche , C & York , D G 2013 , ' The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey : weighing the neutrino mass using the galaxy power spectrum of the CMASS sample ' , Monthly Notices of the Royal Astronomical Society , vol. 436 , no. 3 , pp. 2038-2053 .
dc.identifier.otherPURE: 171418345
dc.identifier.otherPURE UUID: f3f05e56-f7ab-4bef-b60e-6c41e60d76e8
dc.identifier.otherBibCode: 2013MNRAS.436.2038Z
dc.identifier.otherScopus: 84888244893
dc.description.abstractWe measure the sum of the neutrino particle masses using the three-dimensional galaxy power spectrum of the Sloan Digital Sky Survey III (SDSS-III) Baryon Oscillation Spectroscopic Survey Data Release 9the constant MASS (CMASS) galaxy sample. Combined with the cosmic microwave background, supernova and additional baryonic acoustic oscillation data, we find upper 95 per cent confidence limits (CL) of the neutrino mass Σmν <0.340 eV within a flatΛ cold dark matter (ΛCDM) background, and Σmν <0.821 eV, assuming a more general background cosmological model. The number of neutrino species is measured to be Neff = 4.308 ± 0.794 and4.032^{+0.870}_{-0.894} for these two cases, respectively. We study and quantify the effect of several factors on the neutrino measurements, including the galaxy power spectrum bias model, the effect of redshift-space distortion, the cut-off scale of the power spectrum and the choice of additional data. The impact of neutrinos with unknown masses on other cosmological parameter measurements is investigated. The fractional matter density and the Hubble parameter are measured to be ΩM = 0.2796 ± 0.0097, H0 = 69.72^{+0.90}_{-0.91} kms-1 Mpc-1 (flat ΛCDM) and ΩM =0.2798^{+0.0132}_{-0.0136}, H_0=73.78^{+3.16}_{-3.17} kms-1 Mpc-1 (more general background model). Based on a Chevallier-Polarski-Linder parametrization of the equation-of-state w of dark energy, we find that w = -1 is consistent with observations,even allowing for neutrinos. Similarly, the curvature ΩK and the running of the spectral indexαs are both consistent with zero. The tensor-to-scalar ratio is constrained down to r <0.198 (95 per cent CL, flat ΛCDM) and r <0.440 (95 per cent CL, more general background model).
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2013 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:
dc.subjectCosmological parametersen
dc.subjectLarge-scale structure of Universeen
dc.subjectQB Astronomyen
dc.titleThe clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey : weighing the neutrino mass using the galaxy power spectrum of the CMASS sampleen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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