Mass calibration and cosmological analysis of the SPT-SZ galaxy cluster sample using velocity dispersion σνand X-ray YX measurements

S. Bocquet; A. Saro; J. J. Mohr; K. A. Aird; M. L N Ashby; M. Bautz; M. Bayliss; G. Bazin; B. A. Benson; L. E. Bleem; M. Brodwin; J. E. Carlstrom; C. L. Chang; I. Chiu; H. M. Cho; A. Clocchiatti; T. M. Crawford; A. T. Crites; S. Desai; T. De Haan; J. P. Dietrich; M. A. Dobbs; R. J. Foley; W. R. Forman; D. Gangkofner; E. M. George; M. D. Gladders; A. H. Gonzalez; N. W. Halverson; C. Hennig; J. Hlavacek-Larrondo; G. P. Holder; W. L. Holzapfel; J. D. Hrubes; C. Jones; R. Keisler; L. Knox; A. T. Lee; E. M. Leitch; J. Liu; M. Lueker; D. Luong-Van; D. P. Marrone; M. McDonald; J. J. McMahon; S. S. Meyer; L. Mocanu; S. S. Murray; S. Padin; C. Pryke; C. L. Reichardt; A. Rest; J. Ruel; J. E. Ruhl; B. R. Saliwanchik; J. T. Sayre; K. K. Schaffer; E. Shirokoff; H. G. Spieler; B. Stalder; S. A. Stanford; Z. Staniszewski; A. A. Stark; K. Story; C. W. Stubbs; K. Vanderlinde; J. D. Vieira; A. Vikhlinin; R. Williamson; O. Zahn; A. Zenteno

doi:10.1088/0004-637X/799/2/214

Mass calibration and cosmological analysis of the SPT-SZ galaxy cluster sample using velocity dispersion σ_νand X-ray Y_X measurements

S. Bocquet, A. Saro, J. J. Mohr, K. A. Aird, M. L N Ashby, M. Bautz, M. Bayliss, G. Bazin, B. A. Benson, L. E. Bleem, M. Brodwin, J. E. Carlstrom, C. L. Chang, I. Chiu, H. M. Cho, A. Clocchiatti, T. M. Crawford, A. T. Crites, S. Desai, T. De HaanJ. P. Dietrich, M. A. Dobbs, R. J. Foley, W. R. Forman, D. Gangkofner, E. M. George, M. D. Gladders, A. H. Gonzalez, N. W. Halverson, C. Hennig, J. Hlavacek-Larrondo, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, C. Jones, R. Keisler, L. Knox, A. T. Lee, E. M. Leitch, J. Liu, M. Lueker, D. Luong-Van, D. P. Marrone, M. McDonald, J. J. McMahon, S. S. Meyer, L. Mocanu, S. S. Murray, S. Padin, C. Pryke, C. L. Reichardt, A. Rest, J. Ruel, J. E. Ruhl, B. R. Saliwanchik, J. T. Sayre, K. K. Schaffer, E. Shirokoff, H. G. Spieler, B. Stalder, S. A. Stanford, Z. Staniszewski, A. A. Stark, K. Story, C. W. Stubbs, K. Vanderlinde, J. D. Vieira, A. Vikhlinin, R. Williamson, O. Zahn, A. Zenteno

Physics and Astronomy (Twin Cities)

Research output: Contribution to journal › Article › peer-review

122 Scopus citations

Abstract

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_ν) and 16 X-ray Y_X measurements of sample clusters, we simultaneously calibrate themass-observable relation and constrain cosmological parameters. Ourmethod accounts for cluster selection, cosmological sensitivity, and uncertainties in the mass calibrators. The calibrations using σ_νand Y_X are consistent at the 0.6σ level, with the σ_ν calibration preferring ∼16% higher masses. We use the full SPTCL data set (SZ clusters+σ_ν+Y_X) to measure σ₈ (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 Σ 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 Σm_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_νcalibration. 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 σ₈ = 0.829 ± 0.011. Within a νCDM model we find Σm_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).

Original language	English (US)
Article number	214
Journal	Astrophysical Journal
Volume	799
Issue number	2
DOIs	https://doi.org/10.1088/0004-637X/799/2/214
State	Published - Feb 1 2015

Bibliographical note

Publisher Copyright:
© 2015. The American Astronomical Society. All rights reserved.

Keywords

Cosmic background radiation
Cosmology: observations
Galaxies: clusters: individual
Large-scale structure of universe

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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., ... Zenteno, A. (2015). Mass calibration and cosmological analysis of the SPT-SZ galaxy cluster sample using velocity dispersion σ_νand X-ray Y_X measurements. Astrophysical Journal, 799(2), Article 214. https://doi.org/10.1088/0004-637X/799/2/214

Bocquet, S, Saro, A, Mohr, JJ, Aird, KA, Ashby, MLN, Bautz, M, Bayliss, M, Bazin, G, Benson, BA, Bleem, LE, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, De Haan, T, Dietrich, JP, Dobbs, MA, Foley, RJ, Forman, WR, Gangkofner, D, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hennig, C, Hlavacek-Larrondo, J, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, L, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O & Zenteno, A 2015, 'Mass calibration and cosmological analysis of the SPT-SZ galaxy cluster sample using velocity dispersion σ_νand X-ray Y_X measurements', Astrophysical Journal, vol. 799, no. 2, 214. https://doi.org/10.1088/0004-637X/799/2/214

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title = "Mass calibration and cosmological analysis of the SPT-SZ galaxy cluster sample using velocity dispersion σνand X-ray YX measurements",

abstract = "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 (σν) and 16 X-ray YX measurements of sample clusters, we simultaneously calibrate themass-observable relation and constrain cosmological parameters. Ourmethod accounts for cluster selection, cosmological sensitivity, and uncertainties in the mass calibrators. The calibrations using σνand YX are consistent at the 0.6σ level, with the σν calibration preferring ∼16% higher masses. We use the full SPTCL data set (SZ clusters+σν+YX) 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 Σ mν = 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 Σmν 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 YX calibration and 0.8σ higher than the σνcalibration. 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 Σmν = 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).",

keywords = "Cosmic background radiation, Cosmology: observations, Galaxies: clusters: individual, Large-scale structure of universe",

author = "S. Bocquet and A. Saro and Mohr, {J. J.} and Aird, {K. A.} and Ashby, {M. L N} and M. Bautz and M. Bayliss and G. Bazin and Benson, {B. A.} and Bleem, {L. E.} and M. Brodwin and Carlstrom, {J. E.} and Chang, {C. L.} and I. Chiu and Cho, {H. M.} and A. Clocchiatti and Crawford, {T. M.} and Crites, {A. T.} and S. Desai and {De Haan}, T. and Dietrich, {J. P.} and Dobbs, {M. A.} and Foley, {R. J.} and Forman, {W. R.} and D. Gangkofner and George, {E. M.} and Gladders, {M. D.} and Gonzalez, {A. H.} and Halverson, {N. W.} and C. Hennig and J. Hlavacek-Larrondo and Holder, {G. P.} and Holzapfel, {W. L.} and Hrubes, {J. D.} and C. Jones and R. Keisler and L. Knox and Lee, {A. T.} and Leitch, {E. M.} and J. Liu and M. Lueker and D. Luong-Van and Marrone, {D. P.} and M. McDonald and McMahon, {J. J.} and Meyer, {S. S.} and L. Mocanu and Murray, {S. S.} and S. Padin and C. Pryke and Reichardt, {C. L.} and A. Rest and J. Ruel and Ruhl, {J. E.} and Saliwanchik, {B. R.} and Sayre, {J. T.} and Schaffer, {K. K.} and E. Shirokoff and Spieler, {H. G.} and B. Stalder and Stanford, {S. A.} and Z. Staniszewski and Stark, {A. A.} and K. Story and Stubbs, {C. W.} and K. Vanderlinde and Vieira, {J. D.} and A. Vikhlinin and R. Williamson and O. Zahn and A. Zenteno",

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TY - JOUR

T1 - Mass calibration and cosmological analysis of the SPT-SZ galaxy cluster sample using velocity dispersion σνand X-ray YX measurements

AU - Bocquet, S.

AU - Saro, A.

AU - Mohr, J. J.

AU - Aird, K. A.

AU - Ashby, M. L N

AU - Bautz, M.

AU - Bayliss, M.

AU - Bazin, G.

AU - Benson, B. A.

AU - Bleem, L. E.

AU - Brodwin, M.

AU - Carlstrom, J. E.

AU - Chang, C. L.

AU - Chiu, I.

AU - Cho, H. M.

AU - Clocchiatti, A.

AU - Crawford, T. M.

AU - Crites, A. T.

AU - Desai, S.

AU - De Haan, T.

AU - Dietrich, J. P.

AU - Dobbs, M. A.

AU - Foley, R. J.

AU - Forman, W. R.

AU - Gangkofner, D.

AU - George, E. M.

AU - Gladders, M. D.

AU - Gonzalez, A. H.

AU - Halverson, N. W.

AU - Hennig, C.

AU - Hlavacek-Larrondo, J.

AU - Holder, G. P.

AU - Holzapfel, W. L.

AU - Hrubes, J. D.

AU - Jones, C.

AU - Keisler, R.

AU - Knox, L.

AU - Lee, A. T.

AU - Leitch, E. M.

AU - Liu, J.

AU - Lueker, M.

AU - Luong-Van, D.

AU - Marrone, D. P.

AU - McDonald, M.

AU - McMahon, J. J.

AU - Meyer, S. S.

AU - Mocanu, L.

AU - Murray, S. S.

AU - Padin, S.

AU - Pryke, C.

AU - Reichardt, C. L.

AU - Rest, A.

AU - Ruel, J.

AU - Ruhl, J. E.

AU - Saliwanchik, B. R.

AU - Sayre, J. T.

AU - Schaffer, K. K.

AU - Shirokoff, E.

AU - Spieler, H. G.

AU - Stalder, B.

AU - Stanford, S. A.

AU - Staniszewski, Z.

AU - Stark, A. A.

AU - Story, K.

AU - Stubbs, C. W.

AU - Vanderlinde, K.

AU - Vieira, J. D.

AU - Vikhlinin, A.

AU - Williamson, R.

AU - Zahn, O.

AU - Zenteno, A.

PY - 2015/2/1

Y1 - 2015/2/1

N2 - 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 (σν) and 16 X-ray YX measurements of sample clusters, we simultaneously calibrate themass-observable relation and constrain cosmological parameters. Ourmethod accounts for cluster selection, cosmological sensitivity, and uncertainties in the mass calibrators. The calibrations using σνand YX are consistent at the 0.6σ level, with the σν calibration preferring ∼16% higher masses. We use the full SPTCL data set (SZ clusters+σν+YX) 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 Σ mν = 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 Σmν 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 YX calibration and 0.8σ higher than the σνcalibration. 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 Σmν = 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).

AB - 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 (σν) and 16 X-ray YX measurements of sample clusters, we simultaneously calibrate themass-observable relation and constrain cosmological parameters. Ourmethod accounts for cluster selection, cosmological sensitivity, and uncertainties in the mass calibrators. The calibrations using σνand YX are consistent at the 0.6σ level, with the σν calibration preferring ∼16% higher masses. We use the full SPTCL data set (SZ clusters+σν+YX) 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 Σ mν = 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 Σmν 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 YX calibration and 0.8σ higher than the σνcalibration. 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 Σmν = 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).

KW - Cosmic background radiation

KW - Cosmology: observations

KW - Galaxies: clusters: individual

KW - Large-scale structure of universe

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JO - Astrophysical Journal

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