Mass Calibration and Cosmological Analysis of the SPT-SZ Galaxy Cluster Sample Using Velocity Dispersion σ v and X-Ray Y X Measurements
| Autor: | N. W. Halverson, C. L. Reichardt, L. M. Mocanu, Alfredo Zenteno, Julie Hlavacek-Larrondo, G. Bazin, T. M. Crawford, Christopher W. Stubbs, Daniel P. Marrone, Sebastian Bocquet, J. T. Sayre, K. K. Schaffer, J. D. Hrubes, Anthony H. Gonzalez, M. Lueker, A. Clocchiatti, Z. Staniszewski, Jonathan Ruel, Daniel M. Luong-Van, Michael D. Gladders, Bradford Benson, W. L. Holzapfel, K. Vanderlinde, Lindsey Bleem, Armin Rest, O. Zahn, Mike McDonald, Jeff McMahon, Lloyd Knox, Alexey Vikhlinin, B. Stalder, M. L. N. Ashby, Helmuth Spieler, T. de Haan, S. S. Meyer, S. S. Murray, Ryan Keisler, Aaron Lee, J. P. Dietrich, K. A. Aird, S. A. Stanford, M. Brodwin, K. T. Story, John E. Carlstrom, William R. Forman, R. Williamson, C. Pryke, Ryan J. Foley, Chihway Chang, A. T. Crites, Matthew B. Bayliss, G. P. Holder, J. D. Vieira, A. A. Stark, S. Padin, C. Hennig, E. M. Leitch, C. Jones, I-Non Chiu, S. Desai, H. M. Cho, Jiayi Liu, Erik Shirokoff, D. Gangkofner, Marshall W. Bautz, Benjamin Saliwanchik, J. E. Ruhl, Joseph J. Mohr, A. Saro, M. A. Dobbs, Elizabeth George |
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| Přispěvatelé: | Bocquet, S, Saro, A, Mohr, J J, Aird, K A, Ashby, M L N, Bautz, M, Bayliss, M, Bazin, 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, W R, Gangkofner, 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, A, Ruel, J, Ruhl, J E, Saliwanchik, B R, Sayre, J T, Schaffer, K K, Shirokoff, E, Spieler, H G, Stalder, B, Stanford, S A, Staniszewski, Z, Stark, A A, Story, K, Stubbs, C W, Vanderlinde, K, Vieira, J D, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A |
| Jazyk: | angličtina |
| Rok vydání: | 2015 |
| Předmět: |
Physics
galaxies: clusters: individual large-scale structure of universe clusters: individual [galaxies] Sigma Velocity dispersion Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics cosmic background radiation cosmology: observations Astrophysics - Cosmology and Nongalactic Astrophysics Omega symbols.namesake South Pole Telescope Space and Planetary Science Dark energy symbols Planck Neutrino Galaxy cluster observation [cosmology] |
| Zdroj: | Astrophysical Journal Artículos CONICYT CONICYT Chile instacron:CONICYT |
| Popis: | 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 (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 SP_(TCL) data set (SZ clusters+σ_v +Y_X) to measure σ_g(Ω_m/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 SPT_(CL) 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 Ω_m = 0.299 ± 0.009 and σ_g = 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). |
| Databáze: | OpenAIRE |
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