2011MNRAS.416.2916O

Using observations from the Chandra and XMM–Newton X-ray observatories, we examine the interaction between the intragroup medium and central radio source in the nearby NGC 4261 galaxy group. We confirm the presence of cavities associated with the radio lobes and estimate their enthalpy to be ∼2.4 {x} 10⁵⁸ erg. The mechanical power output of the jets is ≥ 10⁴³ erg/s, at least a factor of 60 greater than the cooling luminosity in the region the lobes inhabit. We identify rims of compressed gas enclosing the lobes, but find no statistically significant temperature difference between them and their surroundings, suggesting that the lobe expansion velocity is approximately sonic (M ≤ 1.05). The apparent pressure of the radio lobes, based on the synchrotron minimum energy density argument, is a factor of 5 lower than that of the intragroup medium. Pressure balance could be achieved if the entrainment of thermal gas provided additional non-radiating particles in the lobe plasma, but the energy required to heat these particles would be ∼20 per cent of the mechanical energy output of the radio source. NGC 4261 has a relatively compact cool core, which should probably be categorized as a galactic corona. The corona is capable of fuelling the active nucleus for considerably longer than the inferred source lifetime, but can be only inefficiently heated by the active galactic nucleus (AGN) or conduction. The expansion of the radio lobes has affected the structure of the gas in the galaxy, compressing and moving the material of the corona without causing significant shock heating, and expelling gas from the immediate neighbourhood of the jets. We discuss the possible implications of this environment for the duration of the AGN outburst and consider mechanisms which might lead to the cessation of nuclear activity.