Current status of models with hot and cold dark matter

Mikheeva, E. V.; Lukash, V. N.; Arkhipova, N. A.; Malinovskii, A. M.

doi:10.1134/1.1353356

Cited by 2 publications

(5 citation statements)

References 35 publications

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“…The physical mechanisms of clusters formation promp the relation between cluster mass and temperature, T g ∞M 2/3 , confirmed by numerical simulations (e.g. Navarro et al 1995). The proportionality coefficient depends slightly on cosmological model (mainly, on the parameter Ω m ).…”

Section: Cluster Mass and Temperature Functions And The Evolution Testmentioning

confidence: 52%

“…The consistency with all these tests determines the model parameters (e.g. Bridle et al 1999, Mikheeva et al 2001.…”

Section: Cluster Mass and Temperature Functions And The Evolution Testmentioning

confidence: 99%

“…To test MDM models with a zero cosmological constant we follow the normalization procedure given by Arkhipova et al (1999), Mikheeva et al (2001). All models are normalized by σ 8 by the best fit present day cluster mass (Bahcall & Cen 1993;Bahcall et al 1997) and temperature (Henry & Arnaud 1991;Donahue & Voit 1999) functions.…”

Section: Mdm Models With Non-zero Tensor Modementioning

confidence: 99%

“…The consideration of the red spectra (n < 1) cannot reduce T /S substantially. E.g., in MDM models with fixed Ω ν = 0.2, h = 0.6, and n = 0.9, 1, 1.1: T /S = 0.6, 1.7, 3.6 respectively, which strongly suppresses the height of the first acoustic peak in ∆T /T spectrum (Mikheeva et al 2001).…”

Section: Mdm Models With Non-zero Tensor Modementioning

confidence: 99%

“…An importance of fundamental CGW has been emphasized by Starobinsky (1979), Rubakov et al (1982, Lukash & Mikheeva (2000). Theoretical predictions for cluster abundance in MDM models with CGW has been presented by Ma (1996) for the red spectra of density perturbations (n < 1), and by Mikheeva et al(2001) for both blue (n > 1) and red (n < 1) scalar perturbation spectra. Although ΛCDM models with Ω m ≤ 0.3 normalized by COBE 4-year data (Bunn & White 1997) are consistent with the cluster number density test, in order to archive an agreement with CMBA and cluster abundance data in MDM models it is necessary to take into account the CGW contribution in the derived value of ∆T /T at 10 0 angular scale.…”

Section: Introductionmentioning

confidence: 99%

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Abundance and evolution of galaxy clusters in cosmological models with massive neutrino

Arhipova

Kahniashvili

Lukash

2002

A&A

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Abstract. The time evolution of the number density of galaxy clusters and their mass and temperature functions are used to constrain cosmological parameters in the spatially flat dark matter models containing hot particles (massive neutrino) as well as cold and baryonic matter. We test the modified MDM (Λ = 0) models with cosmic gravitational waves and show that they neither pass the cluster evolution test nor reproduce the observed height of the first acoustic peak in ∆T /T spectrum, and therefore should be ruled out. The models with a non-zero cosmological constant are in better agreement with observations. We estimate the free cosmological parameters in ΛMDM with a negligible abundance of gravitational waves, and find that within the parameter ranges h ∈ (0.6, 0.7), n ∈ (0.9, 1.1), fν ≡ Ων /Ωm ∈ (0, 0.2), (i) the value of ΩΛ is strongly affected by a small fraction of hot dark matter: 0.45 < ΩΛ < 0.7 (1σ CL), and (ii) the redshift evolution of galaxy clusters alone reveals the following explicit relation between ΩΛ and fν : ΩΛ + 0.5fν = 0.65 ± 0.1. This degeneracy is also expected in LSS tests (with a smaller error). The present accuracy of observational data allows to bound the fraction of hot matter, fν ∈ (0, 0.2); the number of massive neutrino species remains undelimited, Nν = 1, 2, 3.

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Section: Cluster Mass and Temperature Functions And The Evolution Testmentioning

confidence: 52%

“…The consistency with all these tests determines the model parameters (e.g. Bridle et al 1999, Mikheeva et al 2001.…”

Section: Cluster Mass and Temperature Functions And The Evolution Testmentioning

confidence: 99%

Section: Mdm Models With Non-zero Tensor Modementioning

confidence: 99%

Section: Mdm Models With Non-zero Tensor Modementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Abundance and evolution of galaxy clusters in cosmological models with massive neutrino

Arhipova

Kahniashvili

Lukash

2002

A&A

Self Cite

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Astrophysics in 2001

Trimble¹,

Aschwanden²

2002

PUBL ASTRON SOC PAC

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ABSTRACT. During the year, astronomers provided explanations for solar topics ranging from the multiple personality disorder of neutrinos to cannibalism of CMEs (coronal mass ejections) and extrasolar topics including quivering stars, out-of-phase gaseous media, black holes of all sizes (too large, too small, and too medium), and the existence of the universe. Some of these explanations are probably probably true, though the authors are not betting large sums on any one. The data ought to remain true forever, though this requires a careful definition of "data" (think of the Martian canals).

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Current status of models with hot and cold dark matter

Cited by 2 publications

References 35 publications

Abundance and evolution of galaxy clusters in cosmological models with massive neutrino

Abundance and evolution of galaxy clusters in cosmological models with massive neutrino

Astrophysics in 2001

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