  We present the first detailed spatio-kinematical analysis and modelling of
the planetary nebula Abell 65, which is known to host a post-common envelope,
binary, central star system. As such, this object is of great interest in
studying the link between nebular morphology and central star binarity.
  [OIII]5007A and H-alpha+[NII]6584A longslit spectra and imagery of Abell 65
were obtained with the Manchester Echelle Spectrometer on the 2.1-m telescope
at the San Pedro Martir Observatory (MES-SPM). Further [OIII]5007A longslit
spectra were obtained with the Ultraviolet and Visual Echelle Spectrograph on
the Very Large Telescope (VLT-UVES). These data were used to develop a
spatio-kinematical model for the [OIII]5007A emission from Abell 65. A
"best-fit" model was found by comparing synthetic spectra and images rendered
from the model to the data. The model comprises an outer shell and an inner
shell, with kinematical ages of 15000 +/- 5000 yr kpc^-1 and 8000 +/- 3000 yr
kpc^-1, respectively. Both shells have peanut-shaped bipolar structures with
symmetry axes at inclinations of 55 +/- 10 deg (to the line-of-sight) for the
outer shell and 68 +/- 10 deg for the inner shell. The near-alignment between
the nebular shells and the binary orbital inclination (of 68 +/- 2 deg) is
strongly indicative that the binary is responsible for shaping the nebula.
Abell 65 is one of a growing number of planetary nebulae (seven to date,
including Abell 65 itself) for which observations and modelling support the
shaping influence of a central binary.
