Evidence for evolution of the luminosity function of clusters of galaxies

Edge, Alastair; Stewart, G. C.; Fabian, A. C.; Arnaud, K. A.

doi:10.1063/1.40391

Cited by 185 publications

(279 citation statements)

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“…Second, our Q ϭ 1 0 low-redshift temperature function has the same shape as in HA and the normalization, although still within the HA errors, is systematically a factor ∼2 lower. It is in good agreement with Edge et al (1990). This change results from the use here of a more robust estimator of the temperature function as well as the correction of a numerical error in HA.…”

Section: Observational Resultssupporting

confidence: 75%

“…There have been many papers that have constrained cosmological parameters using X-ray temperature measurements of clusters (Henry & Arnaud 1991, hereafter HA;Lilje 1992;Oukbir & Blanchard 1992;Hanami 1993;White, Efstathiou, & Frenk 1993a;Bartlett & Silk 1993;Viana & Liddle 1996, hereafter VL;Eke, Cole, & Frenk 1996;Kitayama & Suto 1996, hereafter KS;Oukbir & Blanchard 1997, hereafter OB97). Nearly all of this work has used the low-redshift samples of HA and/or Edge et al (1990). The final result is that there is a degeneracy between j 8 and Q 0 ; the amplitude of the mass density fluctuations is tightly constrained for any given Q 0 , but neither is constrained separately.…”

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confidence: 97%

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A Measurement of the Density Parameter Derived from the Evolution of Cluster X-Ray Temperatures

Henry¹

1997

The Astrophysical Journal

172

175

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We have, for the first time, determined the cluster X-ray temperature function at a redshift other than zero. The observed evolution of the temperatures is mild to a redshift of one-third. The normalization of the luminositytemperature relation is 0.92 ‫ע‬ 0.07 of the low-redshift relation (1 j error), assuming that its shape is the same. Such behavior occurs when clusters form with constant central entropy. The evolution of the temperature function implies that Q 0 is 0.50 ‫ע‬ 0.14 assuming an open universe, or 0.55 ‫ע‬ 0.17 assuming that a cosmological constant produces a flat universe (1 j symmetrized errors)

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Section: Observational Resultssupporting

confidence: 75%

mentioning

confidence: 97%

A Measurement of the Density Parameter Derived from the Evolution of Cluster X-Ray Temperatures

Henry¹

1997

The Astrophysical Journal

172

175

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“…As these authors point out, there is considerable uncertainty in the number density of clusters above 6 keV at redshift zero. A consistent value of ∼ 30 × 10 −8 (h −1 Mpc) −3 is obtained from both the samples of Edge et al (1990) and HA91. Integrating the ROSAT Brightest Cluster Sample (BCS) (Ebeling et al 1997) best-fitting Schechter function for the EMSS passband (0.3−3.5 keV) from infinity to the luminosity corresponding to 6 keV (1.25 × 10 37 h −2 W) suggests a number density of clusters of ∼ 40×10 −8 (h −1 Mpc) −3 .…”

Section: Comparison With Other Studiesmentioning

confidence: 66%

“…EMSS (Henry et al 1992;Gioia & Luppino 1994), ASCA (e.g. Donahue 1996;Mushotzky & Scharf 1997;Henry 1997) and ROSAT (Ebeling et al 1997, Burke et al 1997, Rosati et al 1998) measurements of the X-ray emitting intracluster plasma now complement the low-redshift studies carried out by Edge et al (1990) and David et al (1993). In addition, the CNOC survey provides galaxy velocity dispersions for a well-defined sample of high-redshift clusters (Carlberg et al 1996) and further information on mass distributions is coming from weak gravitational lensing measurements (e.g.…”

Section: Introductionmentioning

confidence: 99%

Measuring Omega0 using cluster evolution

Eke

Cole

Frenk

et al. 1998

Monthly Notices RAS

248

272

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The evolution of the abundance of galaxy clusters depends sensitively on the value of the cosmological density parameter, Ω 0 . Recent ASCA data are used to quantify this evolution as measured by the cluster X-ray temperature function. A χ 2 minimisation fit to the cumulative temperature function, as well as a maximum likelihood estimate (which requires additional assumptions about cluster luminosities), lead to the estimate Ω 0 ≈ 0.45 ± 0.2 (1-σ statistical error). Various systematic uncertainties are considered, none of which enhance significantly the probability that Ω 0 = 1. These conclusions hold for models with or without a cosmological constant, i.e. with Λ 0 = 0 or 1 − Ω 0 . The statistical uncertainties are at least as large as any of the individual systematic errors that have been considered here, suggesting that additional temperature measurements of distant clusters will allow an improvement in this estimate. An alternative method that uses the highest redshift clusters to place an upper limit on Ω 0 is also presented and tentatively applied, with the result that Ω 0 = 1 can be ruled out at the 98 per cent confidence level. Whilst this method does not require a well-defined statistical sample of distant clusters, there are still modelling uncertainties that preclude a firmer conclusion at this time.

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“…Starting from the X-ray flux limited sample by Edge et al (1990), we considered all the clusters with a temperature T ≥ 8 keV, a redshift z < 0.1, and declination δ > −40 • (to be observed by the VLA). Among the resulting nine clusters (Ophiuchus, Coma, A2319, A754, A2142, A401, A644, A2065, A2255) we skipped Coma and A2255 because they were already analyzed in other RM projects (Feretti et al 1995;Govoni et al 2006;Bonafede et al 2010), and A754 because of its complex X-ray morphology.…”

Section: Vla Observations and Data Reductionmentioning

confidence: 99%

Rotation measures of radio sources in hot galaxy clusters

Govoni

Dolag

Murgia

et al. 2010

A&A

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Aims. The goal of this work is to investigate the Faraday rotation measure (RM) of radio galaxies in hot galaxy clusters in order to establish a possible connection between the magnetic field strength and the gas temperature of the intracluster medium. Methods. We performed Very Large Array observations at 3.6 cm and 6 cm of two radio galaxies located in A401 and Ophiuchus, a radio galaxy in A2142, and a radio galaxy located in the background of A2065. All these galaxy clusters are characterized by high temperatures. Results. We obtained detailed RM images at an angular resolution of 3 for most of the observed radio galaxies. The RM images are patchy and reveal fine substructures of a few kpc in size. Under the assumption that the radio galaxies themselves have no effect on the measured RMs, these structures indicate that the intracluster magnetic fields fluctuate down to such small scales. These new data are compared with RM information present in the literature for cooler galaxy clusters. For a fixed projected distance from the cluster center, clusters with higher temperature show a higher dispersion of the RM distributions (σ RM ), mostly because of the higher gas density in these clusters. Although the previously known relation between the clusters X-ray surface brightness (S X ) at the radio galaxy location and σ RM is confirmed, a possible connection between the σ RM − S X relation and the cluster temperature, if present, is very weak. Therefore, in view of the current data, it is impossible to establish a strict link between the magnetic field strength and the gas temperature of the intracluster medium.

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Evidence for evolution of the luminosity function of clusters of galaxies

Cited by 185 publications

References 0 publications

A Measurement of the Density Parameter Derived from the Evolution of Cluster X-Ray Temperatures

A Measurement of the Density Parameter Derived from the Evolution of Cluster X-Ray Temperatures

Measuring Omega0 using cluster evolution

Rotation measures of radio sources in hot galaxy clusters

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