On the properties of non-magnetic peculiar B, A, and early F-type stars

Analyses of high-dispersion, high signal-to-noise spectra enable stellar astronomers to infer many physical and chemical properties of the stars. This paper summarizes detailed analyses of optical spectra of main-sequence, non-magnetic, peculiar B, A, and early F-stars that we performed using the technique of fine analysis. Our primary interest in studying the chemical composition of individual stars is to understand the details of the abundances in light of the theories which predict deviations from solar abundances. Although most recent abundance studies have used fine analysis, it is likely that in the future more studies will use spectrum synthesis techniques. We therefore also review what has been accomplished, and what problems spectrum synthesis will help solve.