Sloshing in its cD halo: MUSE kinematics of the central galaxy NGC 3311
  Early-type galaxies show a strong size evolution with redshift. This
evolution is explained by fast "in-situ" star formation at high-$z$ followed by
a late mass assembly mostly driven by minor mergers that deposit stars
primarily in the outer halo. We aim to identify structural components of the
Hydra I cD galaxy NGC 3311 to investigate the connection between the central
galaxy and the surrounding stellar halo. We map the line-of-sight velocity
distribution (LOSVD) using MUSE pointings covering NGC 3311 out to $25$ kpc.
Combining photometric and spectroscopic data, we model the LOSVD maps using a
finite mixture distribution, including four non-concentric, nearly isothermal
spheroids, with different line-of-sight systemic velocities $V$, velocity
dispersions $\sigma$, and higher order Gauss-Hermite moments $h_3$ and $h_4$.
The comparison of the correlations between $h_3$ and $h_4$ with $V/\sigma$ with
simulations indicates that NGC 3311 assembled mainly through dry mergers. The
$\sigma$ profile rises to $\simeq 400$ km s$^{\text -1}$ at 20 kpc indicating
that stars there were stripped from progenitors orbiting in the cluster core.
The finite mixture distribution modeling supports three inner components
related to the central galaxy and a fourth component with large effective
radius ($51$ kpc) and velocity dispersion ($327$ km s$^{\text{-1}}$) consistent
with a cD envelope. We find that the cD envelope is offset from the center of
NGC 3311 both spatially (8.6 kpc) and in velocity ($\Delta V = 204$
kms$^{-1}$), but coincide with the cluster core X-ray isophotes and the mean
velocity of galaxies. Also, the envelope contributes to the broad wings of the
LOSVD measured by large $h_4$ within 10 kpc. The cD envelope of NGC 3311 is
dynamically associated with the cluster core, which in Hydra I is in addition
displaced from the cluster center, presumably due to a recent subcluster
merger.
