Molecular accretion in the core of the galaxy cluster 2A 0335+096
  We present adaptive optics-assisted K-band integral field spectroscopy of the
central cluster galaxy in 2A 0335+096 (z=0.0349). The H2 v=1-0 S(1) emission is
concentrated in two peaks within 600 pc of the nucleus and fainter but
kinematically-active emission extends towards the nucleus. The H2 is in a
rotating structure which aligns with, and appears to have been accreted from, a
stream of H-alpha emission extending over 14 kpc towards a companion galaxy.
The projected rotation axis aligns with the 5 GHz radio lobes.
  This H2 traces the known 1.2E9 Msun CO-emitting reservoir; limits on the
Br-gamma emission confirm that the H2 emission is not excited by star
formation, which occurs at a rate of less than 1 Msun/yr in this gas. If its
accretion onto the black hole can be regulated whilst star formation remains
suppressed, the reservoir could last for at least 1 Gyr; the simultaneous
accretion of just ~ 5 per cent of the gas could drive a series of AGN outbursts
which offset X-ray cooling in the cluster core for the full 1 Gyr.
Alternatively, if the regulation is ineffective and the bulk of the H2 accretes
within a few orbital periods (25-100 Myr), the resulting 1E62 erg outburst
would be among the most powerful cluster AGN outbursts known. In either case,
these observations further support cold feedback scenarios for AGN heating.
