Density profiles of dark matter halos in an improved secondary infall model
A. Del Popolo 1,2,
M. Gambera 1,3,
E. Recami 4,5,6 and
E. Spedicato 2
Received 1 December 1998 / Accepted 11 May 1999
In this paper we calculate the density profiles of virialized halos both in the case of structure evolving hierarchically from a scale-free Gaussian field having a power spectrum in a Universe and in the case of the CDM model, by using a modified version of Hoffman & Shaham's (1985) (hereafter HS) and Hoffman's (1988) model. We suppose that the initial density contrast profile around local maxima is given by the mean peak profile introduced by Bardeen et al. (1986) (hereafter BBKS), and is not just proportional to the two-point correlation function, as assumed by HS. We show that the density profiles, both for scale-free Universes and the CDM model, are not power-laws but have a logarithmic slope that increases from the inner halo to its outer parts. Both scale-free, for , and CDM density profiles are well approximated by Navarro et al. (1995, 1996, 1997) profile. The radius a, at which the slope , is a function of the mass of the halo and in the scale-free models also of the spectral index n.
Key words: cosmology: theory cosmology: large-scale structure of Universe galaxies: formation
Send offprint requests to: A. Del Popolo (firstname.lastname@example.org)
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© European Southern Observatory (ESO) 2000
Online publication: December 17, 1999