Context : Extended filamentary H \alpha emission nebulae are a striking feature of nearby galaxy clusters but the formation mechanism of the filaments , and the processes which shape their morphology remain unclear .

Aims : We conduct an investigation into the formation , evolution and destruction of dense gas in the center of a simulated , Perseus-like , cluster under the influence of a spin-driven jet .
The jet is powered by the supermassive black hole located in the cluster ’ s brightest cluster galaxy .
We particularly study the role played by condensation of dense gas from the diffuse intracluster medium , and the impact of direct uplifting of existing dense gas by the jets , in determining the spatial distribution and kinematics of the dense gas .

Methods : We present a hydrodynamical simulation of an idealised Perseus-like cluster using the adaptive mesh refinement code ramses .
Our simulation includes a supermassive black hole ( SMBH ) that self-consistently tracks its spin evolution via its local accretion , and in turn drives a large-scale jet whose direction is based on the black hole ’ s spin evolution .
The simulation also includes a live dark matter ( DM ) halo , a SMBH free to move in the DM potential , star formation and stellar feedback .

Results : We show that the formation and destruction of dense gas is closely linked to the SMBH ’ s feedback cycle , and that its morphology is highly variable throughout the simulation .
While extended filamentary structures readily condense from the hot intra-cluster medium , they are easily shattered into an overly clumpy distribution of gas during their interaction with the jet driven outflows .
Condensation occurs predominantly onto infalling gas located 5 - 15 kpc from the center during quiescent phases of the central AGN , when the local ratio of the cooling time to free fall time falls below 20 , i.e .
when t _ { cool } / t _ { ff } < 20 .

Conclusions : We find evidence for both condensation and uplifting of dense gas , but caution that purely hydrodynamical simulations struggle to effectively regulate the cluster cooling cycle and produce overly clumpy distributions of dense gas morphologies , compared to observation .