We have observed the nuclear region of an edge-on spiral galaxy NGC 5793 wi
th VLBI in order to determine the morphology of the central continuum sourc
e at 6 and 18 cm and the distribution of OH molecular gas at 18 cm on parse
c scales. NGC 5793, with a type 2 Seyfert nucleus, is known to have peculia
r H2O maser features in its center, indicating the presence of a rotating d
isk/torus (Hagiwara et al. 1997). Previous interferometric observations cou
ld not clarify both the continuum and OH gas structures due to low angular
resolution (Gardner & Whiteoak 1986, Gardner et al. 1992). We find multiple
continuum peaks forming a bent jet, though the observed peculiar morpholog
y of the continuum source has no straightforward interpretation. We have al
so imaged the distribution of OH absorption toward the central continuum so
urce. Due to the relative weakness of the continuum emission only the centr
al continuum peak shows evidence of detectable opacity of the OH absorbing
gas. The OH velocity field contour map reveals a velocity gradient of 8.7 k
m s(-1) pc(-1) nearly along the galaxy's optical axis. If we suppose that t
he observed OH velocity gradient is caused by simple solid rotation around
the nucleus of the galaxy, the central binding mass is 4.2 x 10(8) Mg. The
direction of the OH velocity field shows a reversal of a sense of rotation
with respect to that of the outer galactic disk observed by CO (1 - 0), imp
lying the existence of an independent kinematical system in the central 10
parsec-scale region of the galaxy. Alternatively, the observed OH molecular
absorption might possibly arise in the parsec;scale circumnuclear region o
f NGC 5793.