  A new semi-automatic approach is employed to carry out the abundance analysis
of high-resolution spectra of HD41076 and HD148330 obtained recently with the
spectropolarimetre ESPaDOnS at the CFHT. This approach allows to prepare in a
semi-automatic mode the input data for the modified ZEEMAN2 code and to analyse
several hundreds of line profiles in sequence during a single run. It also
provides more information on abundance distribution for each chemical element
at the deeper atmospheric layers. Our analysis of the Balmer profiles observed
in the spectra of HD41076 and HD148330 has resulted in the estimates of their
effective temperature, gravity, metallicity and radial velocity. The respective
models of stellar atmosphere have been calculated with the code PHOENIX and
used to carry out abundance analysis employing the modified ZEEMAN2 code. The
analysis shows a deficit of the C, N, F, Mg, Ca, Ti, V, Cu, Y, Mo, Sm and Gd,
and overabundance of Cr, Mn, Fe, Co, Ni, Sr, Zr, Ba, Ce, Nd and Dy in the
stellar atmosphere of HD41076. In the atmosphere of HD148330, the C, N and Mo
appear to be underabundant, while the Ne, Na, Al, Si, P, Ca, Ti, V, Cr, Mn, Fe,
Co, Ni, Zn, Sr, Y, Zr, Ba, Ce, Pr, Nd, Sm, Eu, Gd and Dy are overabundant. We
also have found signatures of vertical abundance stratification of Fe, Ti, Cr
and Mn in HD41076, and of Fe, Ti, V, Cr, Mn, Y, Zr, Ce, Nd, Sm and Gd in
HD148330.
