The molecular gas in the central region of NGC 7213
  We present a multi-wavelength study (from X-ray to millimetre) of the nearby
low-luminosity active galactic nucleus (LLAGN) NGC 7213. We combine the
information from the different bands to characterize the source in terms of
contribution from the AGN and the host-galaxy interstellar medium (ISM). This
approach allows us to provide a coherent picture of the role of the AGN and its
impact, if any, on the star formation and molecular gas properties of the host
galaxy. We focused our study on archival ALMA Cycle 1 observations, where the
CO(2-1) emission line has been used as a tracer of the molecular gas. Using the
3DBarolo code on ALMA data, we performed the modelling of the molecular gas
kinematics traced by the CO(2-1) emission, finding a rotationally dominated
pattern. The host-galaxy molecular gas mass was estimated from the integrated
CO(2-1) emission line obtained with APEX data, assuming an $\alpha_{CO}$
conversion factor. By using the ALMA data, we would have underestimated the gas
masses by a factor $\sim$3, given the filtering out of the large scale emission
in interferometric observations. We also performed a complete X-ray spectral
analysis on archival observations, revealing a relatively faint and unobscured
AGN. The AGN results to be too faint to significantly affect the properties of
the host-galaxy, such as star formation activity and molecular gas kinematics
and distribution.
