  PDS 70 is a $\sim$5 Myr old star with a gas and dust disc in which several
proto-planets have been discovered. We present the first UV detection of the
system along with X-ray observations taken with the \textit{Neil Gehrels Swift
Observatory} satellite. PDS 70 has an X-ray flux of 3.4$\times 10^{-13}$ erg
cm$^{-2}$ s$^{-1}$ in the 0.3-10.0 keV range, and UV flux (U band) of
3.5$\times 10^{-13}$ erg cm$^{-2}$ s$^{-1}$ . At the distance of 113.4 pc
determined from Gaia DR2 this gives luminosities of 5.2$\times 10^{29}$ erg
s$^{-1}$ and 5.4$\times 10^{29}$ erg s$^{-1}$ respectively. The X-ray
luminosity is consistent with coronal emission from a rapidly rotating star
close to the log $\frac{L_{\mathrm{X}}}{L_{\mathrm{bol}}} \sim -3$ saturation
limit. We find the UV luminosity is much lower than would be expected if the
star were still accreting disc material and suggest that the observed UV
emission is coronal in origin.
