  Gas giants' early ($\lesssim 5$ Myr) orbital evolution occurs in a disc
losing mass in part to photoevaporation driven by high energy irradiance from
the host star. This process may ultimately overcome viscous accretion to
disperse the disc and halt migrating giants by starving their orbits of gas,
imprinting on giant planet separations in evolved systems. Inversion of this
distribution could then give insight into whether stellar FUV, EUV or X-ray
flux dominates photoevaporation, constraining planet formation and disc
evolution models. We use a 1D hydrodynamic code in population syntheses for gas
giants undergoing Type II migration in a viscously evolving disc subject to
either a primarily FUV, EUV or X-ray flux from a pre-solar T Tauri star. The
photoevaporative mass loss profile's unique peak location and width in each
energetic regime produces characteristic features in the distribution of giant
separations: a severe dearth of $\lesssim$ 2 M$_{\rm J}$ planets interior to 5
AU in the FUV scenario, a sharp concentration of $\lesssim$ 3 M$_{\rm J}$
planets between $\approx 1.5 - 2$ AU in the EUV case, and a relative abundance
of $\approx 2 - 3.5$ M$_{\rm J}$ giants interior to 0.5 AU in the X-ray model.
These features do not resemble the observational sample of gas giants with mass
constraints, though our results do show some weaker qualitative similarities.
We thus assess how the differing photoevaporative profiles interact with
migrating giants and address the effects of large model uncertainties as a step
to better connect disc models with trends in the exoplanet population.
