  The pulsating white dwarf star PY Vul (G~185-32) exhibits pulsation modes
with peculiar properties that set it apart from other variable stars in the ZZ
Ceti (DAV) class. These peculiarities include a low total pulsation amplitude,
a mode with bizarre amplitudes in the ultraviolet, and a mode harmonic that
exceeds the amplitude of its fundamental. Here, we present optical, time series
spectroscopy of PY Vul acquired with the Keck II LRIS spectrograph. Our
analysis has revealed that the mode with unusual UV amplitudes also has
distinguishing characteristics in the optical. Comparison of its line profile
variations to models suggests that this mode has a spherical degree of four. We
show that all the other peculiarities in this star are accounted for by a
dominant pulsation mode of l=4, and propose this hypothesis as a solution to
the mysteries of PY Vul.
