Explaining the energetic AGN outburst of MS 0735+7421 with massive slow jets

By conducting axisymmetrical hydrodynamical numerical simulations (2.5 dimensional code) we show that slow, massive, wide jets can reproduce the morphology of the huge X-ray deficient bubble pair in the cluster of galaxies MS 0735+7421. The total energy of the jets, composed of the energy in the bubble pair and in the shock wave, is constrained by observations conducted by McNamara et al. to be similar to 10(62) erg. We show that two opposite jets that are active for similar to 100 Myr, each with a launching half opening angle of alpha similar or equal to 70 degrees, an initial velocity of upsilon(j) similar to 0.1 c and a total mass loss rate of the two jets of (M)over dot(2j) similar to 100 M-circle dot yr(-1), can account for the observed morphology. Rapidly precessing narrow jets can be used instead of wide jets. In our model the cluster suffered from a cooling catastrophe similar to 100 Myr ago. Most of the mass that cooled, similar to 10(10) M-circle dot, was expelled back to the intracluster medium by the active galactic nuclei activity and is inside the bubbles now, similar to 10 per cent formed stars and similar to 10 per cent of the cold gas was accreted by the central black hole and was the source of the outburst energy. This type of activity is similar to that expected to occur in galaxy formation.