Spherical collapse and mass function of rich clusters in models with curvature and cosmological constant

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dc.creatorKulinich, Yu.
dc.creatorNovosyadlyj, B.
dc.date2003-02-18
dc.date2003-03-04
dc.date.accessioned2026-07-07T02:07:38Z
dc.date.available2026-07-07T02:07:38Z
dc.descriptionWe have analyzed the dependences of the threshold value of amplitude of linear density fluctuation collapsed at the current epoch, $δ_c$, and its overdensity after virialization, $Δ_c$, on matter density content, 3D curvature parameter and cosmological constant. Though the range for the threshold values of perturbation amplitude is quite narrow - $1.55\le δ_c\le 1.75$ in the region of parameters $-0.4\leΩ_k\le0.4$, $0\leΩ_Λ\le 1$, $0.1\leΩ_m\le 1$, the difference in the concentrations of rich clusters of galaxies (calculated within the Press-Schechter formalism framework) with real and with canonical values of $δ_c$ reaches, and for some models exceeds, 30%. The range of changes for the overdensity after virialization, $Δ_c$, is considerably wider for the same region of parameters: $60\leΔ_c\le180$. It results into difference up to $\sim40$% between the X-ray temperatures of gas, as calculated for these values and for the canonical value of $Δ_c=178$. Also we have found analytical approximations of the dependences $δ_c(Ω_m,Ω_Λ)$ and $Δ_c(Ω_m,Ω_Λ)$ with their accuracies for above mentioned region of parameters being no worse than 0.2% and 1.7% respectively.
dc.description17 pages, 8 figures, LaTeX (Accepted for publication by Journal of Physical Studies, 2003, No1)
dc.identifierhttps://arxiv.org/abs/astro-ph/0302358
dc.identifierhttp://arxiv.org/abs/astro-ph/0302358
dc.identifierJ.Phys.Stud. 7 (2003) 234-246
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/5762
dc.subjectAstrophysics
dc.titleSpherical collapse and mass function of rich clusters in models with curvature and cosmological constant
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