Orateur
M.
Shogo Masaki
(Nagoya University)
Description
We study the matter distribution in and around dark halos in the standard $\Lambda$ cold dark matter ($\Lambda$CDM) universe.
We use the outputs of high resolution $N$-body simulations to compute the mean surface density profile around galactic size dark matter halos.
The result is compared with the observed surface density profile from the lensing magnification measurement of quasars in Sloan Digital Sky Survey (SDSS) recently reported by Menard et al. (2010).
We show that the $\Lambda$CDM simulations reproduce the observed surface density profile remarkably well over a wide range of radial distance of $10 - 10^{4} h^{-1}$kpc.
The mean surface density profile at small separation lengths is consistent with
the theoretical prediction that dark halos have a universal Navarro-Frenk-White
density profile.
The observed single power-law of $\Sigma \propto R^{-0.8}$ over the distance range is explained by a simple analytic model based on a halo approach.
%The time evolution of the mean surface density profile is studied to make predictions for future observations.
We also study the distribution of dark matter in the outer part of the halos
by measuring the mass enclosed within $\alpha R_{\rm virial}$, as a function of $\alpha$.
Our simulations suggest that more than a half of total matter is contained in
about 10\% volume associated with galactic halos.
Assuming the SDSS galaxies are hosted by dark halos with mass $2\times 10^{12} - 10^{14}M_{\odot}$, the total mass around the halos amounts
to 30 percent of the total mass in the local universe.
Author
M.
Shogo Masaki
(Nagoya University)
Co-auteurs
Prof.
Masataka Fukugita
(IPMU, University of Tokyo)
Prof.
Naoki Yoshida
(IPMU, University of Tokyo)
