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Contraction of Dark Matter Halos in Response to Condensation of Baryons
Published online by Cambridge University Press: 19 May 2006
Abstract
The cooling of baryons in the centers of dark matter halos leads to a
more concentrated dark matter distribution. This effect has
traditionally been calculated using the model of adiabatic
contraction, which assumes spherical symmetry, while in hierarchical
formation scenarios halos grow via multiple violent mergers. We
test the adiabatic contraction model in high-resolution cosmological
simulations and find that the dissipation of gas indeed increases
the density of dark matter and steepens its radial profile compared
to the case without cooling. Although the standard model
systematically overpredicts the increase of dark matter density, a
simple modification of the assumed invariant from M(r)r to
$M(\bar{r})r$, where $\bar{r}$
is the orbit-averaged particle
position, reproduces the simulated profiles within 10%.
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- Research Article
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- © EAS, EDP Sciences, 2006