Constraining cosmological models with cluster power spectra

Retzlaff, J.; Borgani, S.; Gottlöber, Stefan; Klypin, Anatoly; Müller, V.

doi:10.1016/s1384-1076(98)00034-7

Cited by 51 publications

(98 citation statements)

References 64 publications

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“…A similar conclusion has been obtained by Luo & Vishniac (1993) by the comparison of the one-dimensional power spectrum found for the Broadhurst et al (1990) pencil beam survey with the theoretical spectrum calculated on the basis of the standard theory. SigniÐcant di †erences between cluster power spectra and spectra based on various variants of CDM models have been noticed by Retzla † et al (1998) and Tadros et al (1998) ; similar di †erences have been found also in the case of the power spectrum based on the twodimensional distribution of APM galaxies by Peacock (1997) and&Baugh (1998). The reconstruction Gaztan8 aga of the primordial density Ðeld by Kashlinsky (1998) also prefers a low-density parameter and shows the difficulty of Ðtting data with CDM models and constant bias parameter.…”

Section: Models With L Ow-density Parametersupporting

confidence: 56%

“…However, recent evidence (Broadhurst et al 1990 ;Landy et al 1996 ;Einasto et al 1997c ;Retzla † et al 1998 ;Tadros et al 1998) indicates that the power spectra of galaxies and clusters of galaxies have a spike or peak on scales around l \ 120 h~1 Mpc or wavenumber k \ 2n/l \ 0.05 h Mpc~1 (we designate the Hubble constant as 100 h km s~1 Mpc~1). This scale corresponds to the step size of the superclustervoid network (Einasto et al 1994a(Einasto et al , 1997a.…”

Section: Introductionmentioning

confidence: 98%

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Steps toward the Power Spectrum of Matter. III. The Primordial Spectrum

Einasto

Tago

et al. 1999

ApJ

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We compare the observed power spectrum of matter found in our earlier papers with analytical power spectra. We extrapolate the observed power spectra on small scales to Ðnd the linear power spectrum of matter. We consider spatially Ñat cold and mixed dark matter models with the cosmological constant as well as open models. We Ðx the Hubble constant and the baryon density in the middle of the allowed range and vary the density parameter and the cosmological constant. We determine the primordial power spectrum of matter using the power spectrum of matter and the transfer functions of analytical models. We take two di †erent spectra suggested by observations : one with a sharp maximum at 120 h~1 Mpc and a second one with a broader maximum, as found for regions with rich and medium-rich superclusters of galaxies, respectively. For both models, the primordial power spectra have a break in amplitude ; in the case of the spectrum with a sharp maximum the break is sharp. We conclude that a scale-free primordial power spectrum is excluded if presently available data on the distribution of clusters and galaxies represent the true mass distribution of the universe.

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Section: Models With L Ow-density Parametersupporting

confidence: 56%

Section: Introductionmentioning

confidence: 98%

Steps toward the Power Spectrum of Matter. III. The Primordial Spectrum

Einasto

Tago

et al. 1999

ApJ

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“…The power spectrum of matter distribution in the present universe has been measured from the spatial distribution of galaxies and galaxy clusters, and found to be generally well reproduced by the CDM power spectrum (Peacock & West 1992;Einasto et al 1993;Jing & Valadarnini 1993;Einasto et al 1997;Retzlaff et al 1998;Tadros et al 1998;Miller & Batuski 2001). An important feature of the power spectra is a turnover, where the scale is closely linked to the horizon scale at matterradiation equality.…”

Section: Comparison With Other Measurementsmentioning

confidence: 89%

A new measurement of the X-ray temperature function of clusters of galaxies

Ikebe

Reiprich

Böhringer

et al. 2002

A&A

190

296

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Abstract. We present a newly measured X-ray temperature function of galaxy clusters using a complete flux-limited sample of 61 clusters. The sample is constructed with the total survey area of 8.14 steradians and the flux limit of 1.99 × 10 −11 ergs s −1 cm −2 in the 0.1-2.4 keV band. X-ray temperatures and fluxes of the sample clusters were accurately measured with ASCA and ROSAT data. The derived temperature function covers an unprecedentedly wide temperature range of 1.4-11 keV. By fitting these data with theoretically predicted temperature functions given by the Press-Schechter formalism together with a recent formation approximation and the CDM power spectrum, we obtained tight and individual constraints on Ωm,0 and σ8. We also employed the Formation-Epoch model in which the distribution in the formation epoch of clusters as well as the temperature evolution are taken into account, showing significantly different results. Systematics caused by the uncertainty in the mass-temperature relation are studied and found to be as large as the statistical errors.

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“…Baugh & Efstathiou (1993 and Gaztañaga & Baugh (1998) determined the three-dimensional power spectrum from the projected distribution of the APM galaxies; the Abell cluster power spectrum was derived by Einasto et al (1997a) and Retzlaff et al (1998), Tadros et al (1998) calculated the power spectrum for the APM clusters. All these studies found the peak or turnover of the power spectrum near a wavelength of λ 0 = 120-130 h −1 Mpc or a wavenumber k 0 = 2π/λ 0 = 0.05 h Mpc −1 .…”

Section: Introductionmentioning

confidence: 99%

The supercluster-void network V.

Saar

Einasto

Toomet

et al. 2002

A&A

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Abstract.We analyze the distribution of Abell clusters of galaxies to study the regularity of the supercluster-void network. We apply a new method, the regularity periodogram, that is sensitive to the geometry of the location of clusters, and measure the regularity of the network. We find that the supercluster-void network resembles a cubic lattice over the entire volume considered (out to the distance of 350 h −1 Mpc). The distribution of clusters in rich superclusters is not isotropic: it is periodic along a cubic lattice approximately aligned with the supergalactic coordinates S GX, S GY, S GZ. This large-scale inhomogeneity does not contradict recent CMB data, but its theoretical explanation remains a challenge.

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Constraining cosmological models with cluster power spectra

Cited by 51 publications

References 64 publications

Steps toward the Power Spectrum of Matter. III. The Primordial Spectrum

Steps toward the Power Spectrum of Matter. III. The Primordial Spectrum

A new measurement of the X-ray temperature function of clusters of galaxies

The supercluster-void network V.

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