Here we present the analysis of multifrequency data gathered for the Fanaroff-Riley type-II ( FR II ) radio galaxy PKS B1358 - 113 , hosted in the brightest cluster galaxy in the center of Abell 1836 .
The galaxy harbors one of the most massive black holes known to date and our analysis of the acquired optical data reveals that this black hole is only weakly active , with a mass accretion rate \dot { M } _ { acc } \sim 2 \times 10 ^ { -4 } \dot { M } _ { Edd } \sim 0.02 M _ { \odot } yr ^ { -1 } .
Based on analysis of new Chandra and XMM- Newton X-ray observations and archival radio data , and assuming the well-established model for the evolution of FR II radio galaxies , we derive the preferred range for the jet kinetic luminosity L _ { j } \sim ( 1 - 6 ) \times 10 ^ { -3 } L _ { Edd } \sim ( 0.5 - 3 ) \times 10 ^ { 45 } erg s ^ { -1 } .
This is above the values implied by various scaling relations proposed for radio sources in galaxy clusters , being instead very close to the maximum jet power allowed for the given accretion rate .
We also constrain the radio source lifetime as \tau _ { j } \sim 40 - 70 Myrs , meaning the total amount of deposited jet energy E _ { tot } \sim ( 2 - 8 ) \times 10 ^ { 60 } ergs .
We argue that approximately half of this energy goes into shock-heating of the surrounding thermal gas , and the remaining 50 \% is deposited into the internal energy of the jet cavity .
The detailed analysis of the X-ray data provides indication for the presence of a bow-shock driven by the expanding radio lobes into the Abell 1836 cluster environment .
We derive the corresponding shock Mach number in the range \mathcal { M } _ { sh } \sim 2 - 4 , which is one of the highest claimed for clusters or groups of galaxies .
This , together with the recently growing evidence that powerful FR II radio galaxies may not be uncommon in the centers of clusters at higher redshifts , supports the idea that jet-induced shock heating may indeed play an important role in shaping the properties of clusters , galaxy groups , and galaxies in formation .
In this context , we speculate on a possible bias against detecting stronger jet-driven shocks in poorer environments , resulting from an inefficient electron heating at the shock front , combined with a relatively long electron-ion temperature equilibration timescale .