COSMOLOGICAL CONSTRAINTS FROM SUNYAEV–ZEL'DOVICH-SELECTED CLUSTERS WITH X-RAY OBSERVATIONS IN THE FIRST 178 deg2 OF THE SOUTH POLE TELESCOPE SURVEY

By B. Benson, T. Haan, J. Dudley, C. Reichardt, K. Aird, K. Andersson, R. Armstrong, M. Ashby, M. Bautz, M. Bayliss and 70 more. 2011

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We use measurements from the South Pole Telescope (SPT) Sunyaev–Zel'dovich (SZ) cluster survey in combination with X-ray measurements to constrain cosmological parameters. We present a statistical method that fits for the scaling relations of the SZ and X-ray cluster observables with mass while jointly fitting for cosmology. The method is generalizable to multiple cluster observables, and self-consistently accounts for the effects of the cluster selection and uncertainties in cluster mass calibration on the derived cosmological constraints. We apply this method to a data set consisting of an SZ-selected catalog of 18 galaxy clusters at z > 0.3 from the first 178 deg2 of the 2500 deg2 SPT-SZ survey, with 14 clusters having X-ray observations from either Chandra or XMM-Newton. Assuming a spatially flat ΛCDM cosmological model, we find the SPT cluster sample constrains σ8(Ω m /0.25)0.30 = 0.785 ± 0.037. In combination with measurements of the cosmic microwave background (CMB) power spectrum from the SPT and the seven-year Wilkinson Microwave Anisotropy Probe data, the SPT cluster sample constrains σ8 = 0.795 ± 0.016 and Ω m = 0.255 ± 0.016, a factor of 1.5 improvement on each parameter over the CMB data alone. We consider several extensions beyond the ΛCDM model by including the following as free parameters: the dark energy equation of state (w), the sum of the neutrino masses (Σm ν), the effective number of relativistic species (N eff), and a primordial non-Gaussianity (f NL). We find that adding the SPT cluster data significantly improves the constraints on w and Σm ν beyond those found when using measurements of the CMB, supernovae, baryon acoustic oscillations, and the Hubble constant. Considering each extension independently, we best constrain w = −0.973 ± 0.063 and the sum of neutrino masses Σm ν < 0.28 eV at 95% confidence, a factor of 1.25 and 1.4 improvement, respectively, over the constraints without clusters. Assuming a ΛCDM model with a free N eff and Σm ν, we measure N eff = 3.91 ± 0.42 and constrain Σm ν < 0.63 eV at 95% confidence. We also use the SPT cluster sample to constrain f NL = −220 ± 317, consistent with zero primordial non-Gaussianity. Finally, we discuss the current systematic limitations due to the cluster mass calibration, and future improvements for the recently completed 2500 deg2 SPT-SZ survey. The survey has detected ∼500 clusters with a median redshift of ∼0.5 and a median mass of ∼2.3 × 1014 M ☉ h −1 and, when combined with an improved cluster mass calibration and existing external cosmological data sets will significantly improve constraints on w.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

Baryon impact on the halo mass function: Fitting formulae and implications for cluster cosmology (2015, background): “Catalogues from different cluster surveys have proven to be useful cosmological probes (e.g. Vikhlinin et al. 2009; Mantz et al. 2010; Rozo et al. 2010; Benson et al. 2013; Hasselfield et al. 2013; Planck Collaboration et al. 2015b; Bocquet et al. 2015; Mantz et al. 2015).”
Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts (2013, methodology): “Benson et al. (2013) used 18 galaxy clusters in the first 178 deg2 of the SPT survey to find σ8(Ωm/0.25)0.3 = 0.785 ± 0.037 for a spatially-flat model.”
Cosmology and astrophysics from relaxed galaxy clusters - II. Cosmological constraints (2014, background): “…et al. 2007; Kowalski et al. 2008; Mantz et al. 2008, 2010b; Dunkley et al. 2009; Vikhlinin et al. 2009; Rozo et al. 2010; Blake et al. 2011; Komatsu et al. 2011; Hinshaw et al. 2013; Suzuki et al. 2012; Anderson et al. 2014; Benson et al. 2013; Hasselfield et al. 2013; Planck Collaboration 2013a).”
The Atacama Cosmology Telescope: Sunyaev-Zel'dovich selected galaxy clusters at 148 GHz from three seasons of data (2013, methodology): “, 68, 84, 91, 103, 123] and constraints on cosmological parameters [11, 91, 98, 114].”
THE PSEUDO-EVOLUTION OF HALO MASS (2012, background): “…campaigns have been undertaken in the past (Vikhlinin et al. 2006; Böhringer et al. 2007; Mantz et al. 2010) and are also currently under way (e.g.Benson et al. 2013) to calibrate these scaling relations since they are necessary to obtain cosmological constraints from the observed abundance of…”
Weighing the giants – IV. Cosmology and neutrino mass (2014, methodology): “Even so, the constraints on w are impressive and competitive with the best other cosmological probes (below), as well as independent results from X-ray (Vikhlinin et al. 2009; see also Burenin & Vikhlinin 2012) and SZ-selected clusters (Benson et al. 2013).”
redMaPPer. I. ALGORITHM AND SDSS DR8 CATALOG (2013, background): “Over the past several years, galaxy clusters have been recognized as powerful cosmological probes (e.g., Henry et al. 2009; Vikhlinin et al. 2009; Mantz et al. 2010; Rozo et al. 2010; Clerc et al. 2012; Benson et al. 2013; Hasselfield et al. 2013).”
Robust weak-lensing mass calibration of Planck galaxy clusters (2014, background): “…in the absolute calibration of cluster masses is currently the most significant challenge facing cluster cosmology (WtG; see also Vikhlinin et al. 2009; Mantz et al. 2010a; Rozo et al. 2010; Sehgal et al. 2011; Benson et al. 2013; Allen et al. 2011; LSST Dark Energy Science Collaboration 2012).”
THE REDMAPPER GALAXY CLUSTER CATALOG FROM DES SCIENCE VERIFICATION DATA (2016, background): “…and are uniquely powerful cosmological probes (e.g., Henry et al. 2009; Vikhlinin et al. 2009; Mantz et al. 2010; Rozo et al. 2010; Clerc et al. 2012; Benson et al. 2013; Hasselfield et al. 2013; Planck Collaboration et al. 2014) (see also reviews in Allen et al. (2011); Weinberg et al. (2013)).”
COSMOLOGICAL CONSTRAINTS FROM GALAXY CLUSTERS IN THE 2500 SQUARE-DEGREE SPT-SZ SURVEY (2016, methodology): “SZ-Mass Scaling Relation Parameterization We use the same functional form for the SZ-mass scaling relation as previous SPT cluster cosmology analyses (V10; Benson et al. 2013, hereafter B13; Reichardt et al. 2013, hereafter R13; Bocquet et al. 2015).”