  We present the results of ammonia observations toward the center of NGC 3079.
The NH3(J, K) = (1, 1) and (2, 2) inversion lines were detected in absorption
with the Tsukuba 32-m telescope, and the NH3(1,1) through (6,6) lines with the
VLA, although the profile of NH3(3,3) was in emission in contrast to the other
transitions. The background continuum source, whose flux density was ~50 mJy,
could not be resolved with the VLA beam of ~< 0."09 x 0."08. All ammonia
absorption lines have two distinct velocity components: one is at the systemic
velocity and the other is blueshifted, and both components are aligned along
the nuclear jets. For the systemic components, the relatively low temperature
gas is extended more than the high temperature gas. The blueshifted NH3(3,3)
emission can be regarded as ammonia masers associated with shocks by strong
winds probably from newly formed massive stars or supernova explosions in dense
clouds in the nuclear megamaser disk. Using para-NH3(1,1), (2,2), (4,4) and
(5,5) lines with VLA, we derived the rotational temperature Trot = 120 +- 12 K
and 157 +- 19 K for the systemic and blueshifted components, respectively. The
total column densities of NH3(0,0)-(6,6), assuming Tex ~Trot, were (8.85+-0.70)
x 10^16 cm^-2 and (4.47+-0.78) x 10^16 cm-2 for the systemic and blueshifted
components, respectively. The fractional abundance of NH3 relative to molecular
hydrogen H2 for the systemic and blueshifted was [NH3]/[H2]=1.3x10^-7 and 6.5 x
10^-8, respectively. We also found the F = 4-4 and F = 5-5 doublet lines of OH
2{Pi}3/2 J = 9/2 in absorption, which could be fitted by two velocity
components, systemic and redshifted components. The rotational temperature of
OH was estimated to be Trot,OH >~ 175 K, tracing hot gas associated with the
interaction of the fast nuclear outflow with dense molecular material around
the nucleus.
