  We present detailed parameter determinations of two chemically normal late
A-type stars, HD 32115 and HD 37594, to uncover the reasons behind large
discrepancies between two previous analyses of these stars performed with a
semi-automatic procedure and a "classical" analysis. Our study is based on high
resolution, high signal-to-noise spectra obtained at the McDonald Observatory.
Our method is based on the simultaneous use of all available observables:
multicolor photometry, pressure-sensitive magnesium lines, metallic lines and
Balmer line profiles. Our final set of fundamental parameters fits, within the
error bars, all available observables. It differs from the published results
obtained with a semi-automatic procedure. A direct comparison between our new
observational material and the spectra previously used by other authors shows
that the quality of the data is not the origin of the discrepancies. As the two
stars require a substantial macroturbulence velocity to fit the line profiles,
we concluded that neglecting this additional broadening in the semi-automatic
analysis is one origin of discrepancy. The use of FeI excitation equilibrium
and of the Fe ionisation equilibrium, to derive effective temperature and
surface gravity, respectively, neglecting all other indicators leads to a
systematically erroneously high effective temperature. We deduce that the
results obtained using only one parameter indicator might be biased and that
those results need to be cautiously taken when performing further detailed
analyses, such as modelling of the asteroseismic frequencies or characterising
transiting exoplanets.
