Jet-induced star formation in 3C 285 and Minkowski Object
  How efficiently star formation proceeds in galaxies is still an open
question. Recent studies suggest that AGN can regulate the gas accretion and
thus slow down star formation (negative feedback). However, evidence of AGN
positive feedback has also been observed in a few radio galaxies (eg. Centaurus
A).
  Here we present CO observations of 3C 285 and Minkowski Object (MO), which
are examples of jet-induced star formation. A spot (named 09.6) aligned with
the 3C 285 radio jet, at a projected distance of ~70 kpc from the galaxy
centre, shows star formation, detected in optical emission. MO is located along
the jet of NGC 541 and also shows star formation. To know the distribution of
molecular gas along the jets is a way to study the physical processes at play
in the AGN interaction with the intergalactic medium.
  We observed CO lines in 3C 285, NGC 541, 09.6 and MO with the IRAM-30m
telescope. In the central galaxies, the spectra present a double-horn profile,
typical of a rotation pattern, from which we are able to estimate the molecular
gas density profile of the galaxy. The molecular gas appears to be in a compact
reservoir. In addition, no kinematic signature of a molecular outflow is
detected by the 30m-telescope.
  Interestingly, 09.6 and MO are not detected in CO. The cold gas mass upper
limits are consistent with a star formation induced by the compression of dense
ambient material by the jet. The depletion time scales are of the order of and
even smaller than what is found in 3C 285, NGC 541 and local spiral galaxies
(10^9 yr). The molecular gas surface density in 09.6 follows a
Schmidt-Kennicutt law if the emitting region is very compact, while MO is found
to have a much higher SFE (very short depletion time). Higher sensitivity and
spatial resolution are necessary to detect CO in the spots of star formation,
and map the emission in these jet-induced star forming regions.
