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Numerical models have shown that disc dispersal via internal photoevaporationdriven by the host star can successfully reproduce the observed pile-up of warmJupiters near 1-2 au. However, since a range of different mechanisms have beenproposed to cause the same feature, clear observational diagnostics of discdispersal leaving an imprint in the observed distribution of giant planetscould help to constrain the dominant mechanisms. We aim to assess the impact ofdisc dispersal via X-ray driven-photoevaporation (XPE) onto giant planetseparations in order to provide theoretical constraints on the location andsize of any possible features related to this process within their observedorbital distribution. For this purpose, we perform a set of 1D populationsyntheses with varying initial conditions and correlate the gas giants' finalparking locations with the X-ray luminosities of their host stars in order toquantify observables of this process within the $L_\mathrm{x}$-$a$-plane ofthese systems. We find that XPE indeed creates an underdensity of gas giantsnear the gravitational radius, with corresponding pile-ups inside and/oroutside of this location. However, the size and location of these features arestrongly dependent on the choice of initial conditions in our model, such asthe assumed formation location of the planets. XPE can strongly affect themigration process of giant planets and leave potentially observable signatureswithin the observed orbital separations of giant planets. However, due to thesimplistic approach employed in our model, which lacks a self-consistenttreatment of planet formation within an evolving disc, a quantitative analysisof the final planet population orbits is not possible. Our results howeverstrongly motivate future studies to include realistic disc dispersal mechanismsinto global planet population synthesis models.

The imprint of X-ray photoevaporation of planet-forming discs on the orbital distribution of giant planets -- II. Theoretical predictions