  We present a detailed study of the neutral and ionised gas phases in the
galactic wind for the nearby starburst galaxy NGC 5394 based on new integral
field spectroscopy obtained with the INTEGRAL fibre system at the William
Herschel Telescope. The neutral gas phase in the wind is detected via the
interstellar NaI D doublet absorption. After a careful removal of the stellar
contribution to these lines, a significant amount of neutral gas (~10^7 Msun)
is detected in a central region of ~1.75 kpc size. This neutral gas is
blueshifted by ~165 km/s with respect to the underlying galaxy. The mass
outflow of neutral gas is comparable to the star formation rate of the host
galaxy. Simultaneously, several emission lines (Ha, [NII], [SII]) are also
analysed looking for the ionised warm phase counterpart of the wind. A careful
kinematic decomposition of the line profiles reveals the presence of a
secondary, broader, kinematic component. This component is found roughly in the
same region where the NaI D absorption is detected. It presents higher [NII]/Ha
and [SII]/Ha line ratios than the narrow component at the same locations,
indicative of contamination by shock ionization. This secondary component also
presents blueshifted velocities, although smaller than those measured for the
neutral gas, averaging to ~ -30 km/s. The mass and mass outflow rate of the
wind is dominated by the neutral gas, of which a small fraction might be able
to escape the gravitational potential of the host galaxy. The observations in
this system can be readily understood within a bipolar gas flow scenario.
