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We report on a detailed abundance study of the fairly bright slow rotators HD30085 (A0 IV), HD 30963 (B9 III) and HD 174567 (A0 V), hitherto reported asnormal stars and the sharp-lined chi Lupi A (B9 IV HgMn). In the spectra of HD30085, HD 30963, the Hg II line at 3984 A line is conspicuous and numerouslines of silicon, manganese, chromium, titanium, iron, strontium, yttrium andzirconium appear to be strong absorbers. A comparison of the mean spectra of HD30085 and HD 30963 with a grid of synthetic spectra for selected unblendedlines having reliable updated atomic data reveals large overabundances ofphosphorus, 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 onthe same effective temperature scale and using the same atomic data forconsistency and comparison for HD 30085 and HD 30963. For HD 174567, milderdeficiencies and excesses are found. The abundances of sodium, magnesium andcalcium have been corrected for NLTE effects. The effective temperatures,surface gravities, low projected rotational velocities and the peculiarabundance patterns of HD 30085 and HD 30963 show that these stars are 2 newHgMn stars and should be reclassified as such. HD 174567 is most likely a newmarginally Chemically Peculiar star. A list of the identifications of linesabsorbing more than 2% in the spectrum of HD 30085 is also provided.

The chemical compositions of the 2 new HgMn stars HD 30085 and HD 30963. Comparison to $\chi$ Lupi A, $\nu$ Cap and HD 174567