  Using the Effelsberg 100-m telescope, sensitive measurements of the H2O
megamaser in NGC 3079 are presented. During 2000 - 2001, `high velocity'
features are seen that are red-shifted up to 225 km/s with respect to the
systemic velocity of the galaxy (about 1120 km/s). Symmetrically bracketing the
systemic velocity, the H2O emission covers a velocity range of 450 km/s with
only one potential narrow gap (20 km/s) near the systemic velocity itself.
Velocity drifts of individual components are not convincingly detected. It is
shown that the presence of red-shifted emission and the absence of detectable
velocity drifts are not inconsistent with the existence of a rotating
circumnuclear maser disk at the very center of the galaxy. Significant
differences in the overall line profile compared to NGC 4258 and a complex
morphology of the radio continuum leave, however, space for scepticism.
