THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGY FROM GALAXY CLUSTERS DETECTED VIA THE SUNYAEV–ZEL'DOVICH EFFECT

By N. Sehgal, Hy Trac, V. Acquaviva, P. Ade, P. Aguirre, M. Amiri, J. Appel, L. Barrientos, E. Battistelli, J. Richard Bond and 59 more. 2010

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We present constraints on cosmological parameters based on a sample of Sunyaev–Zel'dovich-selected (SZ-selected) galaxy clusters detected in a millimeter-wave survey by the Atacama Cosmology Telescope. The cluster sample used in this analysis consists of nine optically confirmed high-mass clusters comprising the high-significance end of the total cluster sample identified in 455 deg2 of sky surveyed during 2008 at 148 GHz. We focus on the most massive systems to reduce the degeneracy between unknown cluster astrophysics and cosmology derived from SZ surveys. We describe the scaling relation between cluster mass and SZ signal with a four-parameter fit. Marginalizing over the values of the parameters in this fit with conservative priors gives σ8 = 0.851 ± 0.115 and w = −1.14 ± 0.35 for a spatially flat wCDM cosmological model with Wilkinson Microwave Anisotropy Probe (WMAP) seven-year priors on cosmological parameters. This gives a modest improvement in statistical uncertainty over WMAP seven-year constraints alone. Fixing the scaling relation between the cluster mass and SZ signal to a fiducial relation obtained from numerical simulations and calibrated by X-ray observations, we find σ8 = 0.821 ± 0.044 and w = −1.05 ± 0.20. These results are consistent with constraints from WMAP7 plus baryon acoustic oscillations plus Type Ia supernova which give σ8 = 0.802 ± 0.038 and w = −0.98 ± 0.053. A stacking analysis of the clusters in this sample compared to clusters simulated assuming the fiducial model also shows good agreement. These results suggest that, given the sample of clusters used here, both the astrophysics of massive clusters and the cosmological parameters derived from them are broadly consistent with current models.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/11d944935b24a00ab98081c3ddc32d794383f0a2

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Citations in the corpus

Observational probes of cosmic acceleration (2012, methodology): “In the simulation approach, one relies on numerical simulations to calibrate the observable–mass relation (e.g. Vanderlinde et al., 2010; Sehgal et al., 2011).”
COSMOLOGICAL CONSTRAINTS FROM SUNYAEV–ZEL'DOVICH-SELECTED CLUSTERS WITH X-RAY OBSERVATIONS IN THE FIRST 178 deg2 OF THE SOUTH POLE TELESCOPE SURVEY (2011, background): “However, even with only ∼10–20 clusters, the cosmological constraints from these surveys have been limited by the systematic uncertainty in the cluster mass calibration (Vanderlinde et al. 2010; Sehgal et al. 2011).”
The Atacama Cosmology Telescope: A Catalog of >4000 Sunyaev–Zel’dovich Galaxy Clusters (2020, background): “…the development of “blind” SZ surveys that constrain cosmological parameters by measuring the evolution of the cluster mass function (e.g., Vanderlinde et al. 2010; Sehgal et al. 2011; Hasselfield et al. 2013; Reichardt et al. 2013; Planck Collaboration et al. 2014a, 2016a; Bocquet et al. 2019).”
Weighing the giants – IV. Cosmology and neutrino mass (2014, background): “…Seljak 2002; Viana et al. 2002; Allen et al. 2003; Pierpaoli et al. 2003; Schuecker et al. 2003; Vikhlinin et al. 2003, 2009; Voevodkin & Vikhlinin 2004; Dahle 2006; Mantz et al. 2008, 2010a; Henry et al. 2009; Rozo et al. 2010; Sehgal et al. 2011; Benson et al. 2013; Planck Collaboration 2013d).”
The Atacama Cosmology Telescope: Sunyaev-Zel'dovich selected galaxy clusters at 148 GHz from three seasons of data (2013, methodology): “Of the nine clusters used in [98], our sample includes the five clusters at z > 0.”
ON THE CLUSTER PHYSICS OF SUNYAEV–ZEL'DOVICH AND X-RAY SURVEYS. I. THE INFLUENCE OF FEEDBACK, NON-THERMAL PRESSURE, AND CLUSTER SHAPES ON Y–M SCALING RELATIONS (2011, background): “Using a small sample of SZ-clusters, SPT (Vanderlinde et al. 2010) and ACT (Sehgal et al. 2011) determined some cosmological constraints, e.g., onσ8.”
Planck intermediate results: V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect (2012, unknown): “A131, page 11 of 24 A&A 550, A131 (2013) Our results, together with the SPT, and ACT results, have to be compared with other works that reported a di ﬀ erence between SZ and X-ray measurements.”
PROBING THE INFLATON: SMALL-SCALE POWER SPECTRUM CONSTRAINTS FROM MEASUREMENTS OF THE COSMIC MICROWAVE BACKGROUND ENERGY SPECTRUM (2012, background): “0.7 Mpc−1; Reid et al. 2010; Vikhlinin et al. 2009; Tinker et al. 2012; Sehgal et al. 2011), while the Lyman-α forest reaches slightly smaller scales (0.3 Mpc−1 . k .”
A MEASUREMENT OF GRAVITATIONAL LENSING OF THE MICROWAVE BACKGROUND USING SOUTH POLE TELESCOPE DATA (2012, background): “These include the measurement of the effects of reionization on the CMB at z ∼ 10 (e.g., Kogut et al. 2003; Komatsu et al. 2011; Zahn et al. 2011); the detection of the integrated Sachs-Wolfe effect from the onset of dark energy domination at z ∼ 1 (e.g., Fosalba et al. 2003; Padmanabhan et al. 2005”
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 SLOAN DIGITAL SKY SURVEY COADD: 275 deg2 OF DEEP SLOAN DIGITAL SKY SURVEY IMAGING ON STRIPE 82 (2011, background): “…sky that has been heavily studied, there are also many opportunities for multi-wavelength studies, from the x-ray (XMM: Mehrtens et al. 2012) to the microwave (SZ: Menanteau et al. 2010; Hand et al. 2011; Reese et al. 2012; Sehgal et al. 2011; Hasselfield et al. 2013) to radio (Hodge et al. 2013).”
Weighing the Giants - I. Weak-lensing masses for 51 massive galaxy clusters: project overview, data analysis methods and cluster images (2012, background): “This uncertainty in the absolute mass scaling is currently the dominant systematic uncertainty in the constraints on σ8 from cluster counts (Mantz et al. 2010a; Vikhlinin et al. 2009b; Rozo et al. 2010; Sehgal et al. 2011; Benson et al. 2013).”
THE ATACAMA COSMOLOGY TELESCOPE: ACT-CL J0102−4915 “EL GORDO,” A MASSIVE MERGING CLUSTER AT REDSHIFT 0.87 (2011, methodology): “5 pixel (yTCMB) of 490± 60µK as published in Sehgal et al. (2011).”
A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH TWO YEARS OF SOUTH POLE TELESCOPE OBSERVATIONS (2011, methodology): “We use local galaxy cluster abundances as measured by Vikhlinin et al. (2009), which directly and tightly constrain σ8 and are consistent with other structure probes (Rozo et al. 2010; Mantz et al. 2010; Vanderlinde et al. 2010; Sehgal et al. 2011).”