  A detailed study of the planetary nebula NGC6565 has been carried out on
long-slit echellograms at six, equally spaced position angles. The expansion
velocity field, the c(Hbeta) distribution and the radial profile of the
physical conditions (electron temperature and density) are obtained. The
distance, radius, mass and filling factor of the nebula and the temperature and
luminosity of the central star are derived. The radial ionization structure is
analyzed using both the classical method and the photo-ionization code CLOUDY.
Moreover, we present the spatial structure in a series of images from different
directions. NGC6565 is a young (2000--2500 years), patchy, optically thick
triaxial ellipsoid projected almost pole-on. The matter close to major axis was
swept-up by some accelerating agent forming two faint and asymmetric polar
cups. A large cocoon of almost neutral gas completely embeds the ionized
nebula. NGC6565 is in a recombination phase. The stellar decline started about
1000 years ago, but the main nebula remained optically thin for other 600 years
before the recombination phase occurred. In the near future the ionization
front will re-grow, since the dilution factor due to the expansion will prevail
on the slower and slower stellar decline. NGC6565 is at a distance of
2.0(+-0.5) Kpc and can be divided into three radial zones: the ``fully
ionized'' one, extending up to 0.029--0.035 pc at the equator (0.050 pc at the
poles), the ``transition'' one, up to 0.048--0.054 pc (0.080 pc), the ``halo'',
detectable up to 0.110 pc. The ionized mass (~0.03 Modot) is only a fraction of
the total mass (> 0.15 Modot), which has been ejected by an equatorial enhanced
superwind of 4(+-2)x10^(-5) Modot/yr lasted for 4(+-2)x10^3 years.
