Kinetic energy transfer from X-ray ultrafast outflows to mm/sub-mm cold
  molecular outflows in Seyfert galaxies
  UltraFast Outflows (UFOs), seen as X-ray blueshifted absorption lines in
active galactic nuclei (AGNs), are considered to be a key mechanism for AGN
feedback. In this scenario, UFO kinetic energy is transferred into the cold and
extended molecular outflow observed at the mm/sub-mm wavelength, which blows
away the gas and suppresses star formation and accretion onto the central black
hole (BH). However, the energy transfer between the inner UFO and the outer
molecular outflow has not yet fully studied mainly due to the limited sample.
In this paper, we performed comparison of their kinetic energy using the
mm/sub-mm published data and the X-ray archival data. Among fourteen Seyfert
galaxies whose molecular outflows are detected in the IRAM/PdBI data, eight
targets are bright enough to perform spectral fitting in X-ray, and we have
detected UFO absorption lines in six targets with 90% significance level, using
XMM-Newton and Suzaku satellites. The time-averaged UFO kinetic energy was
derived from the spectral fitting. As a result, we have found that the
energy-transfer rate (kinetic energy ratio of the molecular outflow to the UFO)
ranges from $\sim7\times10^{-3}$ to $\sim$1, and has a negative correlation
with the BH mass, which shows that the AGN feedback is more efficient in the
lower mass BHs. This tendency is consistent with the theoretical prediction
that the cooling time scale of the outflowing gas becomes longer than the flow
time scale when the BH mass is smaller.
