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We analyse the environment of the supermassive black hole (SMBH) in thecentre of a massive elliptical galaxy NGC 1275 in the Perseus cluster, hostingthe radio source 3C 84. We focus on the young radio lobe observed inside theestimated Bondi accretion radius. We discuss the momentum balance between thejet associated with the lobe and the surrounding gas. The results are comparedwith the proper motion of the radio lobe obtained with the very long baselineinterferometry. We find that under assumption of a high-density environment >~100 cm^-3), the jet power must be comparable to the Eddington luminosity ---this is clearly inconsistent with the current moderate activity of 3C 84, whichindicates instead that the jet is expanding in a very low density region (<~1cm^-3), along the rotation axis of the accretion flow. The power required forthe jet to expand in the low-density environment is comparable to the pastaverage jet power estimated from the X-ray observations. We estimate theclassical Bondi accretion rate, assuming that (1) gas accretion is sphericallysymmetric, (2) accretion is associated with the jet environment, and (3) themedium surrounding the jet is representative of the properties of the dominantaccreting gas. We find that Bondi accretion is inconsistent with the estimatedjet power. This means that either accretion of the cold gas in the NGC 1275 ismore efficient than that of the hot gas, or the jets are powered by the SMBHspin.

The young radio lobe of 3C 84: inferred gas properties in the central 10 parsec