  We use multiplet 30 Cr II lines in the wings of H_beta to test the hypothesis
of an anomalous concentration of Cr in the upper layers of the atmospheres of a
sample of 10 HgMn stars. These lines are at different distances from the H_beta
line center and are therefore formed at different depths in the stellar
atmosphere. Except for HD49606, all HgMn stars show an increase of Cr abundance
with height in the stellar atmosphere. A similar vertical distribution of Cr,
but less pronounced, has been previously found in Am stars. In contrast, no
variation of Cr abundance with the depth has been found for the normal late
B-type star HD196426 and the weak magnetic late B-type star HD168733. It is
possible that in HgMn stars the vertical stratification parameter, a, depends
on T_eff, with the strongest vertical gradient being found in the hotter stars.
No correlation was found between $a$ and the average stellar abundance log
epsilon(Cr/H).
