Dynamical friction of radio galaxies in galaxy clusters

Abstract

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 $t\sim 3–5$ Gyr.

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

References in corpus (4)

• Virial Scaling of Massive Dark Matter Halos: Why Clusters Prefer a High Normalization Cosmology
• An Observed Fundamental Plane Relation for Supermassive Black Holes
• Radio Sources in Galaxy Clusters: Radial Distribution, and 1.4 GHz and K-band Bivariate Luminosity Function
• The evolution of host mass and black hole mass in QSOs from the 2dF QSO Redshift Survey

Cited by in corpus (3)

• Intra Cluster Light properties in the CLASH-VLT cluster MACS J1206.2-0847
• J0454-0309: Evidence for a strong lensing fossil group falling into a poor galaxy cluster
• Implications of the mild gas motion found with Hitomi in the core of the Perseus cluster