Equivalent widths (measured to the nearest 0.5mÅ) and abundances
derived from the individual Mn lines are shown in Table 2.
The equivalent widths for the five binaries noted in
Table 1 have been scaled to compensate for the dilution
of light due to the continuum of their secondaries. The unweighted means
and standard deviations of the line abundances may be compared to the UV
abundances taken from SD93. In accordance with Allen's result, it was
found that Mn II 
4206 (see
below) gave rise to anomalously high
abundances. We also found that Mn II 
4326 followed a similar
pattern of anomalously high abundances. These two lines are thus examined
separately later in this paper. Examples of spectra of the remaining Mn
lines can be seen in Fig. 1.
We were unable to measure with certainty any of the lines in Table 2 for the SD93 normal or superficially-normal comparison stars. This result is consistent with their having the cosmic abundance of Mn, logA = 5.39 (Anders & Grevesse [ 1989]).
Table 2: Mn equivalent widths and abundances in the
HgMn programme
stars. 
