CHANDRA CLUSTER COSMOLOGY PROJECT III: COSMOLOGICAL PARAMETER CONSTRAINTS

By A. Vikhlinin, Andrey V. Kravtsov, R. Burenin, H. Ebeling, W. Forman, A. Hornstrup, C. Jones, S. Murray, D. Nagai, H. Quintana and 1 more. 2008

823 citations recorded by the source corpus.

Chandra observations of large samples of galaxy clusters detected in X-rays by ROSAT provide a new, robust determination of the cluster mass functions at low and high redshifts. Statistical and systematic errors are now sufficiently small, and the redshift leverage sufficiently large for the mass function evolution to be used as a useful growth of a structure-based dark energy probe. In this paper, we present cosmological parameter constraints obtained from Chandra observations of 37 clusters with 〈z〉 = 0.55 derived from 400 deg2 ROSAT serendipitous survey and 49 brightest z ≈ 0.05 clusters detected in the All-Sky Survey. Evolution of the mass function between these redshifts requires ΩΛ > 0 with a ∼5σ significance, and constrains the dark energy equation-of-state parameter to w0 = −1.14 ± 0.21, assuming a constant w and a flat universe. Cluster information also significantly improves constraints when combined with other methods. Fitting our cluster data jointly with the latest supernovae, Wilkinson Microwave Anisotropy Probe, and baryonic acoustic oscillation measurements, we obtain w0 = −0.991 ± 0.045 (stat) ±0.039 (sys), a factor of 1.5 reduction in statistical uncertainties, and nearly a factor of 2 improvement in systematics compared with constraints that can be obtained without clusters. The joint analysis of these four data sets puts a conservative upper limit on the masses of light neutrinos ∑mν < 0.33 eV at 95% CL. We also present updated measurements of ΩMh and σ8 from the low-redshift cluster mass function.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGY FROM GALAXY CLUSTERS DETECTED VIA THE SUNYAEV–ZEL'DOVICH EFFECT (2010, positive): “These results are also consistent with analyses from X-ray cluster samples giving σ8(Ωm/0.25)0.47 = 0.813 ± 0.013 (stat) ±0.024 (sys) and w = −1.14 ± 0.21 (Vikhlinin et al. 2009), Ωm = 0.23 ± 0.04, σ8 = 0.82 ± 0.05, and w = −1.01 ± 0.20 for a wCDM model (Mantz et al. 2010), and Ωm = 0.30+0.03−0.02,…”
MASS FUNCTION PREDICTIONS BEYOND ΛCDM (2010, background): “2010; Abbott et al. 2005; Vikhlinin et al. 2009; Kosowsky 2003; Staniszewski et al. 2009; Bartlett et al. 2008; Fang & Haiman 2008).”
Observational probes of cosmic acceleration (2012, methodology): “…Suzuki et al., 2012), by dark energy constraints from the evolution of X-ray or optically selected clusters (Henry et al., 2009; Mantz et al., 2010; Vikhlinin et al., 2009; Rozo et al., 2010), by improved measurements of the Hubble constant (Riess et al., 2009, 2011; Freedman et al., 2012), and by…”
Detailed cluster lensing profiles at large radii and the impact on cluster weak lensing studies (2011, background): “Indeed, recent cosmological constraints from X-ray analysis of clusters has mainly been limited by various astrophysical uncertainties (e.g., Vikhlinin et al. 2009; Mantz et al. 2010).”
Cosmological parameters from the comparison of peculiar velocities with predictions from the 2M++ density field (2014, methodology): “Constraints can also be obtained from the number counts and mass of galaxy clusters as measured through X-ray surface brightness (Vikhlinin et al. 2009) and measurements of the Sunyaev-Zeldovich (SZ) effect (Planck Collaboration et al. 2013a, Reichardt et al. 2013).”
Stellar Mass—Halo Mass Relation and Star Formation Efficiency in High-Mass Halos (2014, methodology): “The total masses, M500, were derived using robust, lowscatter mass proxy YX (Kravtsov et al. 2006) derived from the Chandra observations, as desribed in Vikhlinin et al. (2009a), except for Abell 1991, MKW 4, RXJ 1159+5531.”
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).”
Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts (2013, methodology): “(A.1)), taken from Arnaud et al. (2010), is not measurable; neither is it measurable for the best-fit Chandra YX–MHE500 relation published in Vikhlinin et al. (2009a).”
A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND DAMPING TAIL FROM THE 2500-SQUARE-DEGREE SPT-SZ SURVEY (2012, result): “Comparing to X-ray measurements of cluster abundance, we rescale the σ8 constraint from Vikhlinin et al. (2009) to the SPT+WMAP7 value of ΩM to find σ8 = 0.813 ± 0.027, which is again consistent with our measured values.”
THE COYOTE UNIVERSE. II. COSMOLOGICAL MODELS AND PRECISION EMULATION OF THE NONLINEAR MATTER POWER SPECTRUM (2009, background): “…a constant equation of state for the dark energy to w = −1 with roughly 10% accuracy (for very recent results from supernovae see, e.g., Kowalski et al. 2008; for weak lensing see, e.g., Kilbinger et al. 2009; and for the latest constraints from clusters of galaxies, see Vikhlinin et al. 2009).”
JOINT ANALYSIS OF CLUSTER OBSERVATIONS. II. CHANDRA/XMM-NEWTON X-RAY AND WEAK LENSING SCALING RELATIONS FOR A SAMPLE OF 50 RICH CLUSTERS OF GALAXIES (2012, methodology): “In numerical simulation studies, this pressure-like quantity has been shown be a much better mass proxy and has been successfully deployed in measurements of cosmological parameters including the dark energy equation of state (Vikhlinin et al. 2009a, 2009b).”
Weighing the Giants – III. Methods and measurements of accurate galaxy cluster weak-lensing masses (2012, methodology): “Weak lensing follow-up of clusters can be used,an to some extent has already been used, to set the absolute calibrations for the mass-observable relations employed in current X-ray and optical cluster count surveys (e.g. Mantz et al. 2008, 2010a; Vikhlinin et al. 2009b; Rozo et al. 2010).”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL PARAMETER RESULTS (2012, background): “Among 49 z < 0.1 clusters with detailed Chandra observations (Vikhlinin et al. 2009a), 29 are large enough to be resolved by WMAP and are outside the KQ75y7 sky mask.”
Simulating the Universe with MICE: The abundance of massive clusters (2009, background): “…matter density), the normalization of the matter power spectrum and the expansion history of the universe, characterized by the dark energy density and its equation of state (e.g. see Mantz et al. 2008; Cunha 2009; Henry et al. 2009; Rozo et al. 2009; Vikhlinin et al. 2009, and references therein).”
Cosmic Discordance: Are Planck CMB and CFHTLenS weak lensing measurements out of tune? (2014, methodology): “They use local H0, baryon acoustic oscillations and local X-ray cluster abundance measurements (Vikhlinin et al. (2009), shown as the red band in Fig.”
GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV–ZEL’DOVICH EFFECT IN THE FIRST 720 SQUARE DEGREES OF THE SOUTH POLE TELESCOPE SURVEY (2012, methodology): “X-ray scaling relations Following Vikhlinin et al. (2009b) and B11, we use YX as an X-ray proxy for cluster mass, M500.”
IMPACT OF CLUSTER PHYSICS ON THE SUNYAEV–ZEL'DOVICH POWER SPECTRUM (2010, methodology): “…some tension between the value of σ8 implied by the measured amplitude of the tSZ power spectrum at ℓ = 3000 and those derived from WMAP observations of the primary CMB power spectrum (Dunkley et al. 2009; Komatsu et al. 2010), or from cluster abundances (Vikhlinin et al. 2009; Mantz et al. 2010).”