Measuring Cosmological Parameters from the Evolution of Cluster X-Ray Temperatures

By J. Henry. 2000

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We have determined the cluster X-ray temperature function from two flux- and redshift-limited samples of clusters. The first sample is comprised of 25 clusters with average redshift 0.05. The local temperature function derived from it supersedes the one we published previously. Fourteen clusters with average redshift 0.38 comprise the second sample. We perform maximum likelihood fits of cluster evolution models to these data in order to constrain cosmological parameters. For an open model with zero cosmological constant we find that the density parameter is Ω0 = 0.49 ± 0.12, the rms mass density fluctuation averaged over 8 h-1 Mpc spheres is σ8 = 0.72 ± 0.10, and the effective index of the mass density fluctuation spectrum on cluster scales is n = -(1.72 ± 0.34), where all errors are symmetrized at 68% confidence. The corresponding results for the case where a cosmological constant produces a flat universe are 0.44 ± 0.12, 0.77 ± 0.15, and -(1.68 ± 0.38). These results agree with those determined from a variety of different independent methods, including supernovae, galaxy-galaxy correlations, fluctuations in the microwave background, gravitational lens statistics, and cluster peculiar velocities.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

Physical Implications of the X-ray Properties of Galaxy Groups and Clusters (2001, result): “In Figure 8 we show the observed temperature function from Henry (2000), after making the necessary volume correction to convert the results to our adopted cosmological model.”
COSMOLOGICAL CONSTRAINTS FROM THE SLOAN DIGITAL SKY SURVEY MaxBCG CLUSTER CATALOG (2009, background): “…at the ∆σ8 ≈ 0.05−0.10 level despite a spread in central values that range from σ8 ≈ 0.65 to σ8 ≈ 1.0 (Viana & Liddle 1996, 1999; Henry & Arnaud 1991; Henry 2000; Pierpaoli et al. 2001; Borgani et al. 2001; Seljak 2002; Viana et al. 2002; Schuecker et al. 2003; Allen et al. 2003; Bahcall…”
Measuring Ωm with the ROSAT Deep Cluster Survey (2001, background): “…sample by adding further 5 clusters at 0.50 ≤ z ≤ 0.83; for flat geometry, they constrained the density parameter to lie in the range Ωm ≃ 0.3±0.1 at the 1σ c.l. Henry (2000) combined the low–z data by Henry & Arnaud (1991) with ASCA temperatures for 15 EMSS clusters at 0.3 < z < 0.6, and…”
Sample Variance Considerations for Cluster Surveys (2002, background): “…rms of matter fluctuations and is thus a very sensitive probe of the power spectrum normalization and matter density in the universe (e.g., Evrard 1989; Frenk et al. 1990; Henry & Arnaud 1991; Lilje 1992; White et al. 1993; Eke et al. 1996; Viana & Liddle 1996; Henry 2000; Pierpaoli et al. 2001).”
The Evolution of X-Ray Clusters and the Entropy of the Intracluster Medium (2000, background): “…counts, luminosity functions and temperature distribu- tions indicate little apparent evolution in clusters back to redshifts as high as ∼ 0.7 (e.g., Henry 1997, 2000; Rosati et al. 1998; Schindler 1999), with the exception of very high luminosity objects or very high redshifts (Gioia et al.…”
Primordial non-Gaussianity from the large-scale structure (2010, background): “mitationofthis method is that, fora realisticamountof primordial NG, the non-Gaussian signal imprinted in cluster abundances is small compared to the systematics plaguing current and upcoming surveys [129, 130, 131]. Given the current uncertainties in the redshift evolution of clusters (one commonly”
The 400 Square Degree ROSAT PSPC Galaxy Cluster Survey: Catalog and Statistical Calibration (2006, unknown): “…used in the past for this purpose (e.g., Evrard 1989; White et al. 1993; Oukbir & Blanchard 1992; Viana & Liddle 1996, 1999; Eke et al. 1998; Henry 1997, 2000; Viana et al. 2003; Vikhlinin et al. 2003; Voevodkin & Vikhlinin 2004; Schuecker et al. 2003), primarily to constrain the…”
ERRATUM: “CHANDRA SAMPLE OF NEARBY RELAXED GALAXY CLUSTERS: MASS, GAS FRACTION, AND MASS–TEMPERATURE RELATION” (2006, ApJ, 640, 691) (2005, unknown): “We, however, caution against direct application of our normalizations to fitting the published cluster temperature functions (Markevitch 1998; Henry 2000; Ikebe et al. 2002) for several reasons.”
MACS: A Quest for the Most Massive Galaxy Clusters in the Universe (2000, background): “The abundance of clusters as a function of redshift is thus an important diagnostic of cosmological parameters, primarily the normalized present-day matter density of the universe, Ω0, and the amplitude of fluctuations in that matter, σ8 (e.g. Oukbir & Blanchard 1997; Eke et al. 1998; Henry 2000).”
A comparison of weak-lensing masses and X-ray properties of galaxy clusters (2007, background): “†E-mail: hoekstra@uvic.ca 1989; Eke et al. 1998; Henry 2000; Haiman, Mohr & Holder 2001; Levine, Schultz & White 2002; Allen et al. 2004).”
The mass profile of A1413 observed with XMM-Newton: Implications for the M-T relation (2002, background): “The magnitude of the effect is not large as compared to the typical difference of ∼50% (Henry 2000) in the normalisation derived by various groups using purely adiabatic simulations.”
Cosmological constraints from the local X-ray luminosity function of the most X-ray-luminous galaxy clusters (2002, result): “Our results are marginally consistent with the values of σ8 = 0.72±0.10 and Ωm = 0.49 ± 0.12 reported by Henry (2000) from an analysis combining the local temperature function of clusters with the properties of EMSS clusters within z < 0.6.”
Modified Entropy Models for the Intracluster Medium (2002, background): “…measure cosmological parameters such as M and 8 have relied heavily on the cluster mass-temperature relation to link cluster masses to observables like cluster temperature and luminosity (e.g., Henry 1997; Bahcall & Fan 1998; Eke et al. 1998a; Donahue & Voit 1999; Borgani et al. 1999; Henry 2000).”
The REFLEX galaxy cluster survey - VII. Omega(m) and sigma(8) from cluster abundance and large-scale clustering (2002, background): “…density come from, e.g., the abundance of galaxy clusters (e.g., Carlberg et al. 1996, Viana & Liddle 1996, Bahcall & Fan 1998, Eke et al. 1998, Henry 2000, Borgani et al. 2001, Reiprich & Böhringer 2002, hereafter RB02), and from the large-scale distribution of clusters (e.g. Collins et al.…”
Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes since z ~ 1.2 (2011, background): “The virial radius rvir is given by the following relation M = 4πr3vir 3 ρ0Δvir(z), (A.11) with Δvir(z) being the critical overdensity for virialisation at redshift z (Kitayama & Suto 1996; Nakamura & Suto 1997; Henry 2000).”
THE EVOLUTION OF X-RAY CLUSTERS OF GALAXIES (2002, methodology): “This result was extended to higher redshifts using cluster temperatures out to z ≃ 0.8 as measured with 26 ASCA and Beppo–SAX data (Donahue et al. 1999, Della Ceca et al. 2000, Henry 2000).”
Galaxy Clusters in Hubble Volume Simulations: Cosmological Constraints from Sky Survey Populations (2001, methodology): “This point is based on three hot (kT > 8 keV) and distant (z > 0.5) clusters covering a search area of 278 sq deg (Henry 2000), leading to a sky surface density 0.011 per sq deg at z > 0.5.”