  $Aims.$ We present a database of 43,340 atmospheric models ($\sim$80,000
models at the conclusion of the project) for stars with stellar masses between
9 and 120 $M_{\odot}$, covering the region of the OB main-sequence and
Wolf-Rayet (W-R) stars in the Hertzsprung--Russell (H--R) diagram.
  $Methods.$ The models were calculated using the ABACUS I supercomputer and
the stellar atmosphere code CMFGEN.
  $Results.$ The parameter space has six dimensions: the effective temperature
$T_{eff}$, the luminosity $L$, the metallicity $Z$, and three stellar wind
parameters: the exponent $\beta$, the terminal velocity $V_{\infty}$, and the
volume filling factor $F_{cl}$. For each model, we also calculate synthetic
spectra in the UV (900-2000 A), optical (3500-7000 A), and near-IR (10000-40000
A) regions. To facilitate comparison with observations, the synthetic spectra
can be rotationally broadened using ROTIN3, by covering vsin(i) velocities
between 10 and 350 km s$^{-1}$ with steps of 10 km s$^{-1}$.
  $Conclusions.$ We also present the results of the reanalysis of $\epsilon$
Ori using our grid to demonstrate the benefits of databases of precalculated
models. Our analysis succeeded in reproducing the best-fit parameter ranges of
the original study, although our results favor the higher end of the mass-loss
range and a lower level of clumping. Our results indirectly suggest that the
resonance lines in the UV range are strongly affected by the velocity-space
porosity, as has been suggested by recent theoretical calculations and
numerical simulations.
