  We report on a detailed abundance study of six bright, mostly southern,
slowly rotating late B stars: HD~1279 (B8III), HD~99803 (B9V), HD~123445 (B9V),
HD~147550 (B9V), HD~171961 (B8III) and HD~202671 (B5II/III), hitherto reported
as normal stars. We compare them to the two classical HgMn stars $\mu$ Lep and
$\beta$ Scl and to the superficially normal star, $\nu$ Cap. In the spectra of
the six stars, the \ion{Hg}{2} line at 3984 \AA\ line is clearly seen and
numerous lines of P, Ti, Mn, Fe, Ga, Sr, Y, and Zr appear to be strong
absorbers. A comparison of newly acquired and archival spectra of these objects
with a grid of synthetic spectra for selected unblended lines reveals large
overabundances of P, Ti, Cr, Mn, Sr, Y, Zr, Ba, Pt and Hg and underabundances
of He, Mg, Sc and Ni. The effective temperatures, surface gravities, low
projected rotational velocities and the peculiar abundance patterns of the six
investigated stars show that they are new chemically peculiar stars, mostly new
HgMn stars, and are reclassified as such. The evolutionary status of these
stars has been inferred and their ages and masses estimated. The two most
massive objects, HD~1279 and HD~202671, might have evolved away from the
main-sequence recently, the other stars are main-sequence objects. HD~99803A is
a sharp lined HgMn star with grazing eclipses; from TESS and MASCARA photometry
we determine an orbital period of $P_{\rm orb} = 26.12022 \pm 0.00004$\,d.
