  Planets that reside close-in to their host star are subject to intense
high-energy irradiation. Extreme-ultraviolet (EUV) and X-ray radiation
(together, XUV) is thought to drive mass loss from planets with volatile
envelopes. We present $\textit{XMM-Newton}$ observations of six nearby stars
hosting transiting planets in tight orbits (with orbital period, $P_\text{orb}
< 10\,$d), wherein we characterise the XUV emission from the stars and
subsequent irradiation levels at the planets. In order to reconstruct the
unobservable EUV emission, we derive a new set of relations from Solar
$\textit{TIMED/SEE}$ data that are applicable to the standard bands of the
current generation of X-ray instruments. From our sample, WASP-80b and
HD$\,$149026b experience the highest irradiation level, but HAT-P-11b is
probably the best candidate for Ly$\,\alpha$ evaporation investigations because
of the system's proximity to the Solar System. The four smallest planets have
likely lost a greater percentage of their mass over their lives than their
larger counterparts. We also detect the transit of WASP-80b in the near
ultraviolet with the Optical Monitor on $\textit{XMM-Newton}$.
