  Observation of the H2O megamaser galaxy IC 2560 with the Chandra Observatory
reveals a complex spectrum composed of soft X-ray emission due to
multi-temperature thermal plasma, and a hard continuum with strong emission
lines. The continuum is most likely a Compton reflection (reprocessing) of
primary emission that is completely absorbed at least up to 7 keV. The lines
can be identified with fluorescence from Si, S and Fe in the lowest ionization
stages. The equivalent widths of the Si and S lines are broadly compatible with
those anticipated for reprocessing by optically thick cold plasma of Solar
abundances, while the large equivalent width of the Fe line requires some
overabundance of iron. A contribution to the line from a transmitted component
cannot be ruled out, but the limits on the strength of the Compton shoulder
make it less likely. From the bolometric luminosity of the nuclear region, we
infer that the source radiates at 1 - 10% of its Eddington luminosity, for an
adopted central mass of 3 million Solar masses. The overall spectrum is
consistent with the hypotheses that the central engines powering the detected
megamsers in accretion disks are obscured from direct view by the associated
accretion disk material itself, and that there is a correlation between the
occurrence of megamaser emission and Compton-thick absorption columns. For the
11 known galaxies with both column density measurements and maser emission
believed to arise from accretion disks, eight AGN are Compton thick.
