  Disc winds and planet formation are considered to be two of the most
important mechanisms that drive the evolution and dispersal of protoplanetary
discs and in turn define the environment in which planets form and evolve.
While both have been studied extensively in the past, we combine them into one
model by performing three-dimensional radiation-hydrodynamic simulations of
giant planet hosting discs that are undergoing X-ray photo-evaporation, with
the goal to analyse the interactions between both mechanisms. In order to study
the effect on observational diagnostics, we produce synthetic observations of
commonly used wind-tracing forbidden emission lines with detailed radiative
transfer and photo-ionisation calculations. We find that a sufficiently massive
giant planet carves a gap in the gas disc that is deep enough to affect the
structure and kinematics of the pressure-driven photo-evaporative wind
significantly. This effect can be strong enough to be visible in the synthetic
high-resolution observations of some of our wind diagnostic lines, such as the
[OI] 6300 \r{A} or [SII] 6730 \r{A} lines. When the disc is observed at
inclinations around 40{\deg} and higher, the spectral line profiles may exhibit
a peak in the redshifted part of the spectrum, which cannot easily be explained
by simple wind models alone. Moreover, massive planets can induce asymmetric
substructures within the disc and the photo-evaporative wind, giving rise to
temporal variations of the line profiles that can be strong enough to be
observable on timescales of less than a quarter of the planet's orbital period.
