  The compact object in the interacting binary AR Sco has widely been presumed
to be a rapidly rotating, magnetized white dwarf (WD), but it has never been
detected directly. Isolating its spectrum has proven difficult because the
spin-down of the WD generates pulsed synchrotron radiation that far outshines
the WD's photosphere. As a result, a previous study of AR Sco was unable to
detect the WD in the averaged far-ultraviolet spectrum from a Hubble Space
Telescope (HST) observation. In an effort to unveil the WD's spectrum, we
reanalyze these HST observations by calculating the average spectrum in the
troughs between synchrotron pulses. We identify weak spectral features from the
previously unseen WD and estimate its surface temperature to be 11500$\pm$500K.
Additionally, during the synchrotron pulses, we detect broad Lyman-$\alpha$
absorption consistent with hot WD spectral models. We infer the presence of a
pair of hotspots, with temperatures between 23000K and 28000K, near the
magnetic poles of the WD. As the WD is not expected to be accreting from its
companion, we describe two possible mechanisms for heating the magnetic poles.
The Lyman-$\alpha$ absorption of the hotspots appears relatively undistorted by
Zeeman splitting, constraining the WD's field strength to be 100 MG, but the
data are insufficient to search for the subtle Zeeman splits expected at lower
field strengths.
