  We report on a detailed abundance study of the fairly bright slow rotators HD
30085 (A0 IV), HD 30963 (B9 III) and HD 174567 (A0 V), hitherto reported as
normal stars and the sharp-lined chi Lupi A (B9 IV HgMn). In the spectra of HD
30085, HD 30963, the Hg II line at 3984 A line is conspicuous and numerous
lines of silicon, manganese, chromium, titanium, iron, strontium, yttrium and
zirconium appear to be strong absorbers. A comparison of the mean spectra of HD
30085 and HD 30963 with a grid of synthetic spectra for selected unblended
lines having reliable updated atomic data reveals large overabundances of
phosphorus, titanium, chromium, manganese, strontium, yttrium, and zirconium,
barium, platinum and mercury and underabundances of helium, magnesium,
scandium, nickel. The surface abundances of chi Lupi A have been rederived on
the same effective temperature scale and using the same atomic data for
consistency and comparison for HD 30085 and HD 30963. For HD 174567, milder
deficiencies and excesses are found. The abundances of sodium, magnesium and
calcium have been corrected for NLTE effects. The effective temperatures,
surface gravities, low projected rotational velocities and the peculiar
abundance patterns of HD 30085 and HD 30963 show that these stars are 2 new
HgMn stars and should be reclassified as such. HD 174567 is most likely a new
marginally Chemically Peculiar star. A list of the identifications of lines
absorbing more than 2% in the spectrum of HD 30085 is also provided.
