  Quasars show a remarkable degree of atomic emission line-broadening, an
observational feature which, in conjunction with a radial distance estimate for
this emission from the nucleus is often used to infer the mass of the central
supermassive black hole. The radius estimate depends on the structure and
kinematics of this so-called Broad-Line Region (BLR), which is often modeled as
a set of discrete emitting clouds. Here, we test an alternative kinematic
disk-wind model of optically thick line emission originating from a
geometrically thin accretion disk under Keplerian rotation around a
supermassive black hole. We use this model to calculate broad emission line
profiles and interferometric phases to compare to GRAVITY data and previously
published cloud modelling results. While we show that such a model can provide
a statistically satisfactory fit to GRAVITY data for quasar 3C 273, we disfavor
it as it requires 3C 273 be observed at high inclination, which observations of
the radio jet orientation do not support.
