Published XUV luminosity as a function of stellar effective temperature for early-type stars hosting planets with detected outflows and targets in our survey (see Sections 1 and 4.1). The XUV luminosities of the proxy MUSCLES stellar spectra used in our sunbather models are shown for reference. Shading corresponds to the projected stellar rotational velocities. The published XUV luminosities for WASP-12 and KELT-9 are upper bounds, which we plot here with downward pointing arrows. We note that WASP-33 has an unpublished XMM-Newton observation, which we use to place an upper limit on the XUV luminosity of the star, as detailed in Appendix C. Gray points correspond to reported X-ray luminosities of F stars from T. Shimura et al. (2025).