  We report VLA B-configuration observations of the HI 21 cm line on the close
disk galaxy pair NGC 5595 and NGC 5597. At the angular resolution of the
observations, $\sim7.1'' \times 4.2''$, while most of the HI 21 cm in NGC 5595
and in NGC 5597 has the same extent as the optical disk, we have detected for
the first time extended structures (streamers) to the north-east (NE), and
south-west (SW) of NGC 5595 with no counterparts in blue, red optical
(continuum), 20 cm radio continuum, or H$\alpha$ spectral-line emission. One
structure is extended by $\sim 45''$ to the NE with blue-shifted velocities,
and the other by $\sim 20''$ to the SW with red-shifted velocities with respect
to the systemic velocity. No HI 21 cm emission is detected from the innermost
central (nuclear) regions of either galaxy. Lower angular resolution HI 21 cm
imaging indicates the non-existence of any intergalactic HI 21 cm gas as tails
or bridges between the two galaxies. Our new 20 cm radio continuum emission
image of NGC 5597 shows a strong unresolved elongated structure at the central
region, in the north-east south-west direction, very similar to the spatial
location of the innermost H$\alpha$ spectral line emission. There is no 20 cm
continuum emission from its north spiral arm. In NGC 5595, the 20 cm radio
continuum image shows no continuum emission from the NE nor the SW extended
structures with HI 21 cm emission.
