  New determinations of effective temperatures of 23 magnetic, chemically
peculiar (mCP) stars were obtained from a fit of metal enhanced model
atmospheres to the observed spectral energy distributions (SED) from UV to red.
The root-mean-square (RMS) method was used to fit the theoretical SED to the
observations corrected for reddening if necessary, with metallicity and
effective temperature as the fitting parameters. Gravity was assumed to be
equal to log g = 4 for main sequence stars and to log g = 3 for two giants in
the considered sample. Equal weights were given to the UV part and visual part
of SED. Independently of the formal quality of fit resulting from the RMS
method applied to the whole SED, the quality of fit was additionally checked
for each star by determination of the temperature from the best fitting model
atmosphere to the UV part and the visual part of SED separately. Both
temperatures should be close to one another if the global best fitting model
satisfactorily describes the full observed SED. This is the case for about a
half of the investigated stars but the difference exceeds 750 K for the
remaining stars with the extreme values above 2000 K. Possible reasons for such
discrepancies are discussed. New, revised calibrations of effective temperature
and bolometric corrections of mCP stars in terms of reddening free Stromgren
indices are given.
