  We utilize a multi-step modelling process to produce synthetic
interferometric and spectroscopic observables, which are then compared to their
observed counterparts. Our extensive set of interferometric observations of the
Be star 48 Per, totaling 291 data points, were obtained at the Navy Precision
Optical Interferometer from 2006 Nov 07 to 2006 Nov 23. Our models were further
constrained by comparison with contemporaneous H$\alpha$ line spectroscopy
obtained at the John S. Hall Telescope at Lowell Observatory on 2006 Nov 1.
Theoretical spectral energy distributions, SEDs, for 48~Per were confirmed by
comparison with observations over a wavelength regime of 0.4 to 60 microns from
Touhami et al. (2010) and Vieira et al. (2017). Our best-fitting combined model
from H$\alpha$ spectroscopy, H$\alpha$ interferometry and SED fitting has a
power law density fall off, $n$, of 2.3 and an initial density at the stellar
surface of $\rho_0 = 1.0 \times 10^{-11} \rm{g\,cm}^{-3}$ with a inclination
constrained by H$\alpha$ spectroscopy and interferometry of 45$^{\circ} \pm
5^{\circ}$. The position angle for the system, measured east from north, is
121$^{\circ}$ $\pm$ 1$^{\circ}$. Our best-fit model shows that the disk
emission originates in a moderately large disk with a radius of 25 R$_{*}$
which is consistent with a disk mass of approximately 5 $\times$ 10$^{24}$ g or
3 $\times$ 10$^{-10}$ M$_{*}$. Finally, we compare our results with previous
studies of 48~Per by Quirrenbach et al. (1997) with agreement but find, with
our much larger data set, that our disk size contradicts the findings of Delaa
et al. (2011).
