MASS CALIBRATION AND COSMOLOGICAL ANALYSIS OF THE SPT-SZ GALAXY CLUSTER SAMPLE USING VELOCITY DISPERSION σv AND X-RAY YX MEASUREMENTS

We 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 deg(2) of the survey along with 63 velocity dispersion (sigma(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 sigma(v) and Y-X are consistent at the 0.6 sigma level, with the sigma(v) calibration preferring similar to 16% higher masses. We use the full SPTCL data set (SZ clusters+sigma(v)+Y-X) to measure sigma(8)(Omega(m)/0.27)(0.3) = 0.809 +/- 0.036 within a flat ACDM 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 Sigma m(upsilon) = 0.06 eV, we find the data sets to be consistent at the 1.0 sigma level for WMAP9 and 1.5 sigma for Planck+WP. Allowing for larger Sigma m(upsilon) 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 1.9 sigma higher than the Y-X calibration and 0.8 sigma higher than the sigma(v) calibration. Given the scale of these shifts (similar to 44% and similar to 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 Omega(m) = 0.299 +/- 0.009 and sigma(8) = 0.829 +/- 0.011. Within upsilon CDM model we find Sigma m(upsilon) = 0.148 +/- 0.081 eV. We present a consistency test of the cosmic growth rate using SPT clusters. Allowing both the growth index gamma and the dark energy equation-of-state parameter w to vary, we find gamma = 0.73 +/- 0.28 and w = -1.007 +/- 0.065, demonstrating that the expansion and the growth histories are consistent with ACDM universe (gamma = 0.55; w = -1).