  We present the discovery and confirmation of a transiting hot, bloated
Super-Neptune using photometry from TESS and LCOGT and radial velocity
measurements from HARPS. The host star TOI-2498 is a V = 11.2, G-type
(T$_{eff}$ = 5905 $\pm$ 12K) solar-like star with a mass of 1.12 $\pm$ 0.02
M$_{\odot}$ and a radius of 1.26 $\pm$ 0.04 R$_{\odot}$. The planet, TOI-2498
b, orbits the star with a period of 3.7 days, has a radius of 6.1 $\pm$ 0.3
R$_{\oplus}$, and a mass of 35 $\pm$ 4 M$_{\oplus}$. This results in a density
of 0.86 $\pm$ 0.25 g cm$^{-3}$. TOI-2498 b resides on the edge of the Neptune
desert; a region of mass-period parameter space in which there appears to be a
dearth of planets. Therefore TOI-2498 b is an interesting case to study to
further understand the origins and boundaries of the Neptune desert. Through
modelling the evaporation history, we determine that over its $\sim$3.6 Gyr
lifespan, TOI-2498 b has likely reduced from a Saturn sized planet to its
current radius through photoevaporation. Moreover, TOI-2498 b is a potential
candidate for future atmospheric studies searching for species like water or
sodium in the optical using high-resolution, and for carbon based molecules in
the infra-red using JWST.
