  Non-LTE calculations are performed for NII in stellar atmospheric models
appropriate to main sequence B-stars to produce new grids of equivalent widths
for the strongest NII lines commonly used for abundance analysis. There is
reasonable agreement between our calculations and previous results, although we
find weaker non-LTE effects in the strongest optical NII transition. We also
present a detailed estimation of the uncertainties in the equivalent widths due
to inaccuracies in the atomic data via Monte Carlo simulation and investigate
the completeness of our model atom in terms of included energy levels.
Uncertainties in the basic NII atomic data limit the accuracy of abundance
determinations to ~+/-0.10 dex at the peak of the NII optical spectrum near
Teff~ 24,000 K.
