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 } \simeq 1.38 \times 10 ^ { 11 } ~ { } \text { M } _ { \odot } ) dispersion-supported spheroid ( \Delta \text { v } _ { \star } \leq 150 km s ^ { -1 } , \sigma _ { 0 } \sim 216 km s ^ { -1 } ) hosting an active supermassive black hole ( M _ { SMBH } \simeq 3.8 \times 10 ^ { 9 } ~ { } \text { M } _ { \odot } ) 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 \sim 100 km s ^ { -1 } , 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 .