Spatial correlation function of quasars and power spectrum of cosmological matter density perturbations

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dc.creatorNovosyadlyj, B.
dc.creatorChornij, Yu.
dc.date1999-01-28
dc.date.accessioned2026-07-07T02:30:14Z
dc.date.available2026-07-07T02:30:14Z
dc.descriptionWe examine the dependence of the spatial two-point correlation function of quasars $ξ_{qq}(r,z)$ at different redshifts on the initial power spectrum in flat cosmological models. Quasars and other elements of the large-scale structure of the universe are supposed to form in the peaks of the scalar Gaussian field of density fluctuations of appropriate scales. Quasars are considered as a manifestation of short-term active processes at the centers of these fluctuations. We propose a method for calculating the correlation function $ξ_{qq}(r,z)$ and show its amplitude and slope to depend on the shape of the initial power spectrum and the scale R of the fluctuations in which quasars are formed. We demonstrate that in the CDM models with the initial power spectrum slope $n=0.7\div1$ it is possible to explain, by choosing appropriate values of R, how the amplitudes and correlation radii of $ξ_{qq}(r,z)$ may either increase or decrease with increasing redshift z. In particular, the correlation radii of $ξ_{qq}(r,z)$ grow from $6-10h^{-1}$ Mpc when R grows from $0.45 h^{-1}$ to $1.3h^{-1}$ Mpc. The H+CDM model at realistic values of R fails to account for the observational data according to which the $ξ_{qq}(r,z)$ amplitude decreases with increasing $z$.
dc.description8 pages, 2 figures
dc.identifierhttps://arxiv.org/abs/astro-ph/9901393
dc.identifierhttp://arxiv.org/abs/astro-ph/9901393
dc.identifierKinematics Phys.Celest.Bodies 14 (1998) 56
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/13751
dc.subjectAstrophysics
dc.titleSpatial correlation function of quasars and power spectrum of cosmological matter density perturbations
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