Non-LTE calculations are performed for N ii in stellar atmospheric models appropriate to main sequence B-stars to produce new grids of equivalent widths for the strongest N ii 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 N ii transition , \lambda 3995 .
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 N ii atomic data limit the accuracy of abundance determinations to \approx \pm 0.10 dex at the peak of the N ii optical spectrum near T _ { eff } \approx 24 , 000 K .