Recent discoveries of young exoplanets within their natal disks offer exciting opportunities to study ongoing planet formation. In particular, a planets mass accretion rate can be constrained by observing the accretion-induced excess emission. So far, planetary accretion is only probed by the H$alpha$ line, which is then converted to a total accretion luminosity using correlations derived for stars. However, the majority of the accretion luminosity is expected to emerge from hydrogen continuum emission, and is best measured in the ultraviolet (UV). In this paper, we present HST/WFC3/UVIS F336W (UV) and F656N (H$alpha$) high-contrast imaging observations of PDS 70. Applying a suite of novel observational techniques, we detect the planet PDS 70 b with signal-to-noise ratios of 5.3 and 7.8 in the F336W and F656N bands, respectively. This is the first time that an exoplanet has been directly imaged in the UV. Our observed H$alpha$ flux of PDS 70 b is higher by $3.5sigma$ than the most recent published result. However, the light curve retrieved from our observations does not support greater than 30% variability in the planets H$alpha$ emission in six epochs over a five-month timescale. We estimate a mass accretion rate of $1.4pm0.2times10^{-8}M_{mathrm{Jup}}/mathrm{yr}$. H$alpha$ accounts for 36% of the total accretion luminosity. Such a high proportion of energy released in line emission suggests efficient production of H$alpha$ emission in planetary accretion, and motivates using the H$alpha$ band for searches of accreting planets. These results demonstrate HST/WFC3/UVISs excellent high-contrast imaging performance and highlight its potential for planet formation studies.
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