  Whether planetary nebulae (PNe) are predominantly the product of binary
stellar evolution as some population synthesis models (PSM) suggest remains an
open question. Around 50 short period binary central stars ($P\sim1$ d) are
known, but with only four with measured orbital periods over 10 d, our
knowledge is severely incomplete. Here we report on the first discovery from a
systematic SALT HRS survey for long period binary central stars. We find a 142
d orbital period from radial velocities of the central star of NGC~1360,
HIP~16566. NGC~1360 appears to be the product of common-envelope (CE)
evolution, with nebula features similar to post-CE PNe, albeit with an orbital
period considerably longer than expected to be typical of post-CE PSM. The most
striking feature is a newly-identified ring of candidate low-ionisation
structures (LIS). Previous spatio-kinematic modelling of the nebula gives a
nebula inclination of $30\pm10$ deg, and assuming the binary nucleus is
coplanar with the nebula, multi-wavelength observations best fit a more
massive, evolved WD companion. A WD companion in a 142 d orbit is not the focus
of many PSM, making NGC~1360 a valuable system with which to improve future PSM
work. HIP~16566 is amongst many central stars in which large radial velocity
variability was found by low-resolution surveys. The discovery of its binary
nature may indicate long period binaries may be more common than PSM models
predict.
