# Deep spectroscopy in nearby galaxy clusters: III Orbital structure of galaxies in Abell 85

## TL;DR

This study investigates the orbital structures of galaxies in Abell 85, revealing that galaxy orbits vary with distance from the center and stellar color, suggesting orbital shape influences galaxy color rather than accretion history.

## Contribution

It provides the first detailed analysis of galaxy orbital anisotropy in Abell 85 using Jeans modeling and compares galaxy dynamics with dark matter halo profiles.

## Key findings

- Galaxies near the center have isotropic orbits.
- Outer galaxies exhibit radial orbits.
- Blue and red galaxies show different orbital properties.

## Abstract

Galaxies in clusters are strongly affected by their environment. They evolve according to several physical mechanisms that are active in clusters. Their efficiency can strongly depend on the orbital configuration of the galaxies. Our aim is to analyse the orbits of the galaxies in the cluster Abell 85, based on the study of the galaxy velocity anisotropy parameter. We have solved the Jeans equation under the assumption that the galaxies in A85 are collisionless objects, within the spherically symmetric gravitational potential of the virialized cluster. The mass of the cluster was estimated with X-ray and caustic analyses. We find that the anisotropy profile of the full galaxy population in A85 is an increasing monotonic function of the distance from the cluster centre: on average, galaxies in the central region (r/r200 < 0.3) are on isotropic orbits, while galaxies in the outer regions are on radial orbits. We also find that the orbital properties of the galaxies strongly depend on their stellar colour. In particular, blue galaxies are on less radial orbits than red galaxies. The different families of cluster galaxies considered here have the pseudo phase-space density profiles Q(r) and Qr(r) consistent with the profiles expected in virialized dark matter halos in $N$-body simulations. This result suggests that the galaxies in A85 have reached dynamical equilibrium within the cluster potential. Our results indicate that the origin of the blue and red colour of the different galaxy populations is the different orbital shape rather than the accretion time.