Using a sample of 92 Galactic Be stars, we compare inclination angles (the
angle between a star's rotation axis and the line-of-sight) determined from
H$\alpha $ emission line profile fitting to those determined by the
spectroscopic signature of gravitational darkening. We find good agreement: 70%
of the sample (64 out of 92 stars) is consistent with zero difference between
the two methods using $1\sigma $ errors, and there is a strong linear
correlation coefficient between the two methods of $r=+0.63\pm 0.05$ . There is
some evidence that the H$\alpha $ profile fitting method overestimates the
inclination angle for $i\lesssim {25}^{\circ}$ , perhaps due to the neglect of
incoherent electron scattering on the H$\alpha $ line widths, while the
gravitational darkening method underestimates the inclination angle for
$i\gtrsim {70}^{\circ}$ , perhaps due to the neglect of disk radiative transfer
effects on the optical spectrum. Overall, it is demonstrated that a single
H$\alpha $ spectrum of modest resolution and SNR can be used to extract a useful
estimate for the inclination angle of an individual Be star. This allows
equatorial rotation velocities for individual Be stars to be derived from $v\mathrm{sin}i$ measurements and will allow Be stars to be used to search for
correlated spin axes in young, open clusters if unbiased (with respect to
inclination) samples of Be stars are used.