Mass Calibration and Cosmological Analysis of the SPT-SZ Galaxy Cluster Sample Using Velocity Dispersion $σ_v$ and X-ray $Y_\textrm{X}$ Measurements
Creators: name: Bocquet, S.
name: Saro, A.
name: Mohr, J. J.
name: Aird, K. A.
name: Ashby, M. L. N.
name: Bautz, M.
name: Bayliss, M.
name: Bazin, G.
name: Benson, B. A.
name: Bleem, L. E.
name: Brodwin, M.
name: Carlstrom, J. E.
name: Chang, C. L.
name: Chiu, I.
name: Cho, H. M.
name: Clocchiatti, A.
name: Crawford, T. M.
name: Crites, A. T.
name: Desai, S.
name: de Haan, T.
name: Dietrich, J. P.
name: Dobbs, M. A.
name: Foley, R. J.
name: Forman, W. R.
name: Gangkofner, D.
name: George, E. M.
name: Gladders, M. D.
name: Gonzalez, A. H.
name: Halverson, N. W.
name: Hennig, C.
name: Hlavacek-Larrondo, J.
name: Holder, G. P.
name: Holzapfel, W. L.
name: Hrubes, J. D.
name: Jones, C.
name: Keisler, R.
name: Knox, L.
name: Lee, A. T.
name: Leitch, E. M.
name: Liu, J.
name: Lueker, M.
name: Luong-Van, D.
name: Marrone, D. P.
name: McDonald, M.
name: McMahon, J. J.
name: Meyer, S. S.
name: Mocanu, L.
name: Murray, S. S.
name: Padin, S.
name: Pryke, C.
name: Reichardt, C. L.
name: Rest, A.
name: Ruel, J.
name: Ruhl, J. E.
name: Saliwanchik, B. R.
name: Sayre, J. T.
name: Schaffer, K. K.
name: Shirokoff, E.
name: Spieler, H. G.
name: Stalder, B.
name: Stanford, S. A.
name: Staniszewski, Z.
name: Stark, A. A.
name: Story, K.
name: Stubbs, C. W.
name: Vanderlinde, K.
name: Vieira, J. D.
name: Vikhlinin, A.
name: Williamson, R.
name: Zahn, O.
name: Zenteno, A.
Publisher: name: arXiv
Year: 2014
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: 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 deg2 of the survey along with 63 velocity dispersion ($σ_v$) and 16 X-ray Yx measurements of sample clusters, we simultaneously calibrate the mass-observable relation and constrain cosmological parameters. The calibrations using $σ_v$ and Yx are consistent at the $0.6σ$ level, with the $σ_v$ calibration preferring ~16% higher masses. We use the full cluster dataset to measure $σ_8(Ω_ m/0.27)^{0.3}=0.809\pm0.036$. The SPT cluster abundance is lower than preferred by either the WMAP9 or Planck+WMAP9 polarization (WP) data, but assuming the sum of the neutrino masses is $\sum m_ν=0.06$ eV, we find the datasets to be consistent at the 1.0$σ$ level for WMAP9 and 1.5$σ$ for Planck+WP. Allowing for larger $\sum m_ν$ further reconciles the results. When we combine the cluster and Planck+WP datasets with BAO and SNIa, the preferred cluster masses are $1.9σ$ higher than the Yx 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 dataset, we measure $Ω_ m=0.299\pm0.009$ and $σ_8=0.829\pm0.011$. Within a $ν$CDM model we find $\sum m_ν= 0.148\pm0.081$ eV. We present a consistency test of the cosmic growth rate. Allowing both the growth index $γ$ and the dark energy equation of state parameter $w$ to vary, we find $γ=0.73\pm0.28$ and $w=-1.007\pm0.065$, demonstrating that the expansion and the growth histories are consistent with a LCDM model ($γ=0.55; \,w=-1$).
description: Accepted by ApJ (v2 is accepted version); 17 pages, 6 figures