  We present a study of NV absorption systems at 1.5 < z < 2.5 in the optical
spectra of 19 QSOs. Our analysis includes both absorbers arising from the
intergalactic medium as well as systems in the vicinity of the background
quasar. We construct detailed photoionization models to study the physical
conditions and abundances in the absorbers and to constrain the spectral
hardness of the ionizing radiation. The rate of incidence for intervening NV
components is dN/dz = 3.38 +/- 0.43, corresponding to dN/dX = 1.10 +/- 0.14.
The column density distribution function is fitted by the slope beta = 1.89 +/-
0.22, consistent with measurements for CIV and OVI. The narrow line widths
(b_NV ~ 6 km/s) imply photoionization rather than collisions as dominating
ionization process. The column densities of CIV and NV are correlated but show
different slopes for intervening and associated absorbers, which indicates
different ionizing spectra. Associated systems are found to be more metal-rich,
denser, and more compact than intervening absorbers. This conclusion is
independent of the adopted ionizing radiation. For the intervening NV systems
we find typical values of [C/H] ~ -0.6 and n_H ~ 10^-3.6 cm^-3, and sizes of a
few kpc, while for associated NV absorbers we obtain [C/H] ~ +0.7, n_H ~
10^-2.8 cm^-3, and sizes of several 10 pc. The abundance of nitrogen relative
to carbon [N/C] and alpha-elements like oxygen and silicon [N/alpha] is
correlated with [N/H], indicating the enrichment by secondary nitrogen. The
larger scatter in [N/alpha] in intervening systems suggests an inhomogeneous
enrichment of the IGM. There is an anti-correlation between [N/alpha] and
[alpha/C], which could be used to constrain the initial mass function of the
carbon- and nitrogen-producing stellar population.
