  We present phase-resolved optical spectra of the low mass X-ray binary system
V801 Ara. The spectra, obtained in 2014 with IMACS on the Magellan/Baade
telescope at Las Campanas Observatory, cover the full binary orbit of 3.8
hours. They contain strong emission features allowing us to map the emission of
HAlpha, HBeta, He II 4686, and the Bowen blend at 4640. The radial velocity
curves of the Bowen blend shows significantly stronger modulation at the
orbital period than HAlpha as expected for the former originating on the
secondary with the latter consistent with emission dominated by the disk. Our
tomograms of HAlpha and HBeta are the most detailed studies of these lines for
V801 to date and they clearly detect the accretion disk. The HBeta emission
extends to higher velocities than HAlpha, suggesting emission from closer to
the neutron star and differentiating temperature variance in the accretion disk
for the first time. The center of the accretion disk appears offset from the
center-of-mass of the neutron star as has been seen in several other X-ray
binaries. This is often interpreted to imply disk eccentricity. Our tomograms
do not show strong evidence for a hot spot at the point where the accretion
stream hits the disk. This could imply a reduced accretion rate or could be due
to the spot being drowned out by bright accretion flow around it. There is
enhanced emission further along the disk, however, which implies gas stream
interaction downstream of the hot spot.
