Observations of the Mercury-Manganese star φ Her with the Navy Prototype Optical Interferometer (NPOI) conclusively reveal the previously unseen companion in this single-lined binary system. The NPOI data were used to predict a spectral type of A8V for the secondary star φ Her B. This prediction was subsequently confirmed by spectroscopic observations obtained at the Dominion Astrophysical Observatory. φ Her B is rotating at 50 ± 3 km s −1 , in contrast to the 8 km s −1 lines of φ Her A. Recognizing the lines from the secondary permits one to separate them from those of the primary. The abundance analysis of φ Her A shows an abundance pattern similar to those of other HgMn stars with Al being very underabundant and Sc,

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We performed elemental abundances analyses of the mercury-manganese (HgMn) stars 53 Tau, β Tau, and γ Crv consistent with previous studies of similar stars in this series. The derived v sin i values for the last two stars are 59 and 32 km s −1 , respectively, both of which are greater than those of HgMn stars previously studied. For 53 Tau this analysis using selected wavelength regions replaces one performed with coadded photographic spectra. A stricter upper limit is placed on any Hg II λ3984 line. The abundances of β Tau are usually greater than those of γ Crv. But the later star has a Hg II λ3984 line which the former lacks. Our analysis of υ Her, which was performed with spectrograms obtained with CCD detectors, is extended by using additional spectrograms to increase the range of wavelengths covered longward of λ4800. Minor changes in the derived abundances result.

Abstract. Elemental abundances analyses of the superfically normal B and A stars α Dra (A0 III), τ Her (B5 IV), γ Lyr (B9 III), and HR 7926 (B8 II-III) are performed consistent with previous studies of this series using spectrograms obtained with Reticon and CCD detectors. Comparisons of the first two analyses with those of the same stars performed earlier in this series which used mostly coadded photographic plates show the general consistency of the derived elemental abundances. A slight increase in the adopted effective temperature produces a corresponding increase in the derived abundances. In these stars the He/H ratios are found to be close to solar. Except for γ Lyr the metals show for the most part marginally subsolar abundance values. But this star has Al, Ca, Sc, and Sr abundances that are substantially underabundant as well as other underabundant values.

Elemental abundances of 28 And (A7 III) and 99 Her (F7 V), which have modest rotational velocities, are derived in a manner consistent with previous studies in this series of papers. The values for 28 And, a δ Scuti variable, show that it is slightly metal‐poor, but not a classical Am star. 99 Her, which is somewhat more metal‐poor, has a rather small microturbulence for its spectral type.