Second Epoch ALMA Observations of 321 GHz Water Maser Emission in NGC
  4945 and the Circinus Galaxy
  We present the results of second epoch ALMA observations of 321 GHz H$_2$O
emission toward two nearby active galactic nuclei, NGC 4945 and the Circinus
galaxy, together with Tidbinbilla 70-m monitoring of their 22 GHz H$_2$O
masers. The two epoch ALMA observations show that the strengths of the 321 GHz
emission are variable by a factor of at least a few, confirming a maser origin.
In the second epoch, 321 GHz maser emission from NGC 4945 was not detected,
while for the Circinus galaxy the flux density significantly increased and the
velocity gradient and dispersion have been measured. With the velocity gradient
spanning $\sim$110 km/s, we calculate the disk radius to be $\sim$28 pc,
assuming disk rotation around the nucleus. We also estimate the dynamical mass
within the central 28 pc to be 4.3 $\times$ 10$^8$ M$_{\odot}$, which is
significantly larger than the larger scale dynamical mass, suggesting the
velocity gradient does not trace circular motions on that scale. The overall
direction of the velocity gradient and velocity range of the blueshifted
features are largely consistent with those of the 22 GHz maser emission in a
thin disk with smaller radii of 0.1--0.4 pc and molecular outflows within
$\sim$1 pc from the central engine of the galaxy, implying that the 321 GHz
masers could trace part of the circumnuclear disk or the nuclear outflows.
