A Novel Test of Quasar Orientation
  The orientation of the disk of material accreting onto supermassive black
holes that power quasars is one of most important quantities that are needed to
understand quasars -- both individually and in the ensemble average. We present
a hypothesis for determining comparatively edge-on orientation in a subset of
quasars (both radio loud and radio quiet). If confirmed, this orientation
indicator could be applicable to individual quasars without reference to radio
or X-ray data and could identify some 10-20% of quasars as being more edge-on
than average, based only on moderate resolution and signal-to-noise
spectroscopy covering the CIV 1549A emission feature. We present a test of said
hypothesis using X-ray observations and identify additional data that are
needed to confirm this hypothesis and calibrate the metric.
