Inquiring into the nature of the Abell 2667 Brightest Cluster Galaxy:
  physical properties from MUSE
  Based on HST and MUSE data, we probe the stellar and gas properties (i.e.
kinematics, stellar mass, star formation rate) of the radio-loud brightest
cluster galaxy (BCG) located at the centre of the X-ray luminous cool core
cluster Abell 2667 (z = 0.2343). The bi-dimensional modelling of the BCG
surface brightness profile reveals the presence of a complex system of
substructures extending all around the galaxy. Clumps of different size and
shape plunged into a more diffuse component constitute these substructures,
whose intense 'blue' optical colour hints to the presence of a young stellar
population. Our results depict the BCG as a massive (M_star ~ 1.38 x 10^11
M_sun) dispersion-supported spheroid (v_star < 150 km/s, sigma_0 ~ 216 km/s)
hosting an active supermassive black hole (M_SMBH ~ 3.8 x 10^9 M_sun) whose
optical features are typical of low ionisation nuclear emission line regions.
Although the velocity pattern of the stars in the BCG is irregular, the stellar
kinematics in the regions of the clumps show a positive velocity of ~ 100 km/s,
similarly to the gas component. An analysis of the mechanism giving rise to the
observed lines in the clumps through empirical diagnostic diagrams points out
that the emission is composite, suggesting the contribution from both star
formation and AGN. We conclude our analysis describing how scenarios of both
chaotic cold accretion and merging with a gas-rich disc galaxy can
efficaciously explain the phenomena the BCG is undergoing.
