Dynamical friction of radio galaxies in galaxy clusters

Details Dynamical friction of radio galaxies in galaxy clusters Dynamical friction of radio galaxies in galaxy clusters

2008-04-22

arxiv.org/abs/0804.3468v1

Astronomy and Astrophysics

Astrophysics

4 pages, 2 figures, MNRAS (Letters) in press

Scientific paper

10.1111/j.1745-3933.2008.00483.x

The distribution of luminous radio galaxies in galaxy clusters has been observed to be concentrated in the inner region. We consider the role of dynamical friction of massive galaxies ($M\sim 10^{12.5}$ M$_{\odot}$), assuming them to be hosts of luminous radio galaxies, and show that beginning with a Navarro-Frenk-White density profile of a cluster of mass $M_{cl}\sim 10^{15}$ M$_{\odot}$ of concentration $c\sim 5$ and collapsing at $z\sim 1$, the density profile of radio galaxies evolve to a profile of concentration $c \sim 25$, as observed, in a time scale of $t\sim 3\hbox{--}5$ Gyr.

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