  We present accurate methods of abundance determination based on the non-local
thermodynamic equilibrium (NLTE) line formation for carbon, oxygen, calcium,
titanium, and iron in the atmospheres of BAF-type stars. For C I-II, O I, Ca
I-II, and Ti I-II, their comprehensive model atoms were described in our
previous papers. A fairly complete model atom of Fe I-II is first applied in
this study. We determine the NLTE abundances of the nine BAF-type stars with
well-determined atmospheric parameters, using high-resolution and high
signal-to-noise ratio spectral observations in the broad wavelength range, from
the UV to the IR. For C, Ca, Ti, and Fe, NLTE leads to consistent abundances
from the lines of the two ionisation stages. The C I, Ca II, and Fe II emission
lines were detected in the near IR spectrum of the late B-type subgiant star HD
160762. They are well reproduced in the classical model atmosphere, when
applying our NLTE methods.
