A very extended molecular web around NGC 1275
  We present the first detection of CO emission lines in the Halpha filaments
at distances as far as 50 kpc from the centre of the galaxy NGC 1275. This gas
is probably dense (>=10E3 cm-3). However, it is not possible to accurately
determine the density and the kinetic temperature of this relatively warm gas
(Tkin~20-500K) with the current data only. The amount of molecular gas in the
filaments is large 10E9 Msun (assuming a Galactic N(H2)/Ico ratio). This is 10%
of the total mass of molecular gas detected in this cD galaxy. This gas has
large-scale velocities comparable to those seen in Halpha. The origin of the
filaments is still unclear, but their formation is very likely linked to the
AGN positive feedback (Revaz et al., 2008) that regulates the cooling of the
surrounding X-ray-emitting gas as suggested by numerical simulations. We also
present high-resolution spectra of the galaxy core. The spatial characteristics
of the double-peaked profile suggest that the molecular web of filaments and
streamers penetrates down to radii of less than 2 kpc from the central AGN and
eventually feed the galaxy nucleus. The mass of gas inside the very central
region is ~10E^9 Msun, and is similar to the mass of molecular gas found in the
filaments.
