Bocquet, S.Saro, A.Mohr, J. J.Aird, K. A.Ashby, MatthewBautz, M.Bayliss, MatthewBazin, G.Benson, B. A.Bleem, L. E.Brodwin, M.Carlstrom, J. E.Chang, C. L.Chiu, I.Cho, H. M.Clocchiatti, A.Crawford, T. M.Crites, A. T.Desai, S.de Haan, T.Dietrich, J. P.Dobbs, M. A.Foley, R. J.Forman, WilliamGangkofner, D.George, E. M.Gladders, M. D.Gonzalez, A. H.Halverson, N. W.Hennig, C.Hlavacek-Larrondo, J.Holder, G. P.Holzapfel, W. L.Hrubes, J. D.Jones, C.Keisler, R.Knox, L.Lee, A. T.Leitch, E. M.Liu, J.Lueker, M.Luong-Van, D.Marrone, D. P.McDonald, M.McMahon, J. J.Meyer, S. S.Mocanu, L.Murray, S. S.Padin, S.Pryke, C.Reichardt, C. L.Rest, ArminRuel, J.Ruhl, J. E.Saliwanchik, B. R.Sayre, J. T.Schaffer, K. K.Shirokoff, E.Spieler, H. G.Stalder, BrianStanford, S. A.Staniszewski, Z.Stark, AntonyStory, K.Stubbs, ChristopherVanderlinde, K.Vieira, J. D.Viklinin, AlexeyWilliamson, R.Zahn, O.Zenteno, A.2015-07-022015Bocquet, S., A. Saro, J. J. Mohr, K. A. Aird, M. L. N. Ashby, M. Bautz, M. Bayliss, et al. 2015. “Mass Calibration and Cosmological Analysis of the SPT-SZ Galaxy Cluster Sample Using Velocity Dispersion σ v and X-Ray Y X Measurements.” The Astrophysical Journal 799, no. 2: 214. doi:10.1088/0004-637x/799/2/2141538-4357http://nrs.harvard.edu/urn-3:HUL.InstRepos:16953382We present a velocity-dispersion-based mass calibration of the South Pole Telescope Sunyaev-Zel'dovich effect survey (SPT-SZ) galaxy cluster sample. Using a homogeneously selected sample of 100 cluster candidates from 720 deg2 of the survey along with 63 velocity dispersion (σ v ) and 16 X-ray Y X measurements of sample clusters, we simultaneously calibrate the mass-observable relation and constrain cosmological parameters. Our method accounts for cluster selection, cosmological sensitivity, and uncertainties in the mass calibrators. The calibrations using σ v and Y X are consistent at the 0.6σ level, with the σ v calibration preferring ~16% higher masses. We use the full SPTCL data set (SZ clusters+σ v +Y X) to measure σ8(Ωm/0.27)0.3 = 0.809 ± 0.036 within a flat ΛCDM model. The SPT cluster abundance is lower than preferred by either the WMAP9 or Planck+WMAP9 polarization (WP) data, but assuming that the sum of the neutrino masses is ∑m ν = 0.06 eV, we find the data sets to be consistent at the 1.0σ level for WMAP9 and 1.5σ for Planck+WP. Allowing for larger ∑m ν further reconciles the results. When we combine the SPTCL and Planck+WP data sets with information from baryon acoustic oscillations and Type Ia supernovae, the preferred cluster masses are 1.9σ higher than the Y X calibration and 0.8σ higher than the σ v calibration. Given the scale of these shifts (~44% and ~23% in mass, respectively), we execute a goodness-of-fit test; it reveals no tension, indicating that the best-fit model provides an adequate description of the data. Using the multi-probe data set, we measure Ωm = 0.299 ± 0.009 and σ8 = 0.829 ± 0.011. Within a νCDM model we find ∑m ν = 0.148 ± 0.081 eV. We present a consistency test of the cosmic growth rate using SPT clusters. Allowing both the growth index γ and the dark energy equation-of-state parameter w to vary, we find γ = 0.73 ± 0.28 and w = –1.007 ± 0.065, demonstrating that the expansion and the growth histories are consistent with a ΛCDM universe (γ = 0.55; w = –1).en-UScosmic background radiationcosmology: observationsgalaxies: clusters: individuallarge-scale structure of universeJournal Article2015-07-0210.1088/0004-637x/799/2/214