Molecular gas filamentary structures in galaxy clusters
  Recent molecular line observations with ALMA and NOEMA in several Brightest
Cluster Galaxies (BCG) have revealed the large-scale filamentary structure at
the center of cool core clusters. These filaments extend over 20-100kpc, they
are tightly correlated with ionized gas (H$\alpha$, [NII]) emission, and have
characteristic shapes: either radial and straight, or also showing a U-turn,
like a horse-shoe structure.
  The kinematics is quite regular and laminar, and the derived infall time is
much longer than the free-fall time. The filaments extend up to the radius
where the cooling time becomes larger than the infall time. Filaments can be
perturbed by the sloshing of the BCG in its cluster, and spectacular cooling
wakes have been observed. Filaments tend to occur at the border of cavities
driven in the X-ray gas by the AGN radio jets. Observations of cool core
clusters support the thermal instability scenario, which accounts for the
multiphase medium in the upper atmospheres of BCG, where the right balance
between heating and cooling is reached, and a chaotic cold gas accretion
occurs. Molecular filaments are also seen associated to ram-pressure stripped
spiral galaxies in rich galaxy clusters, and in jet-induced star formation,
suggesting a very efficient molecular cloud formation even in hostile cluster
environments.
