Galactic Be star inclination angles

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+/-0.05.

There is some evidence that the H{alpha} profile fitting method overestimates the inclination angle for i<~25{deg}, 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>~70{deg}, 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.