  We present accurate element abundance patterns based on the non-local
thermodynamic equilibrium (non-LTE, NLTE) line formation for 14 chemical
elements from He to Nd for a sample of nine A9 to B3 type stars with well
determined atmospheric parameters and low rotational velocities. We constructed
new model atom of Zr II-III and updated model atoms for Sr II and Ba II by
implementing the photoionization cross sections from calculations with the
Dirac B-spline R-matrix method. The NLTE abundances of He to Fe in the stars
HD~17081, HD~32115, HD~160762, and HD~209459 are found to be consistent with
the solar abundances, and HD~73666 being a Blue Struggler does not reveal
deviations from chemical composition of the Praesepe cluster. Three of these
stars with an effective temperature of lower than 10500~K have supersolar
abundances of Sr, Zr, Ba, and Nd, and our results suggest the presence of a
positive correlation between stellar effective temperature and abundance. For
each star, enhancement of Ba is higher than that for any other heavy element.
We propose that the solar Ba abundance is not representative of the galactic Ba
abundance at modern epoch. The status of HD~145788 was not clarified: this star
has solar abundances of C to Si and enhancements of Sr to Ba similar to that
for superficially normal stars of similar temperature, while overabundant Ca,
Ti, and Fe. The NLTE abundances of Vega support its status of a mild
lambda~Bootis star.
