We used programs SYNSPEC (Hubeny et al. 1994) and WIDTH9 (Kurucz, private communication, respectively, to determine the helium and metal abundances. The adopted metal-line damping constants were the default semi-classical approximations, except for iron-peak element lines, whose values were based on the data of Kurucz (1993). We applied a 3% scattered light correction to account for light scattered along the direction of the dispersion, which is an appropriate value for clean optical systems (Gulliver et al. 1996).
Table 1 (click here) contains both the derived He/H ratios from lines on the
CASLEO spectrograms (
and 
) and the older modern
spectroscopic material. The slight changes
in the effective temperature and surface gravity help increase the He/H ratio
of 
Lep. The values derived from the CASLEO equivalent widths for
this star are slightly less than those from the DAO
equivalent widths. The CASLEO values make 7 Sex appear to be slightly more
solar-like. The values confirm the relatively high He/H
ratio for the HgMn star HR 4817 and the relatively low He/H ratio for 28
Her.
Table 2 (click here) summarizes the determination of the microturbulence using
Fe I and Fe II lines. The derived abundances are independent of the
equivalent width (
) and result in a minimum scatter about the mean
(
). For Lep and 28 Her, we find microturbulences of 0.3 and
, respectively, rather than zero as previously found
for these and most HgMn stars. The use of additional lines makes the
values from both species agree better for 7 Sex. For HR 4817, the Fe II
lines still indicate no microturbulence. Now there are substantially more
lines and a determination can be done just with MF gf values.
Tables 3 (click here)-6 (click here) (which are available only in electronic form)
contain the metal line results from our spectra. For each new line, they
contain the multiplet number, the wavelength in Å, the equivalent width
in mÅ, the gf value and its source, and the derived abundance (
) where 
is the total number of atoms per unit
volume.
Species |  Cep |  Cap | 7 Sex |  Dra | Merak | o Peg | 21 Lyn | Sun |
He I | -1.08 | -1.19 | -1.00 | -1.04 | -1.52 | -1.26 | -1.10 | -1.04 |
| C I | -3.78 | ... | -2.97 | -3.91 | -3.68 | ... | -3.71 | -3.43 |
| C II | -3.62 | -3.39 | -2.81 | -3.51 | -3.76 | -4.40 | ... | -3.43 |
| O I | ... | -3.33 | -2.94 | -3.49 | ... | -3.36 | ... | -3.09 |
| Mg I | -4.41 | -4.71 | -3.99 | -4.61 | -4.46 | -4.49 | -4.86 | -4.42 |
| Mg II | -4.55 | -4.61 | -4.27 | -4.86 | -4.59 | -4.54 | -4.79 | -4.42 |
| Al I | -5.97 | -6.03 | -5.82 | -6.07 | -5.43 | -5.58 | -6.06 | -5.53 |
| Al II | -5.66 | ... | ... | -5.76 | -5.28 | ... | ... | -5.53 |
| Si I | ... | ... | ... | ... | ... | -4.69 | ... | -4.45 |
| Si II | -4.56 | -4.69 | -4.40 | -4.89 | -4.49 | -4.43 | -4.53 | -4.45 |
| S II | -4.65: | -4.85 | -3.99 | -4.60 | ... | -4.00 | ... | -4.79 |
| Ca I | -5.71 | -5.98 | -5.05 | -6.28 | -5.75 | -5.61 | -6.00 | -5.64 |
| Ca II | -5.41 | -5.55 | -5.24 | -5.61 | -5.28 | -5.43 | -5.66 | -5.64 |
| Sc II | -9.20 | -9.34 | -8.64 | -9.41 | -9.20 | -9.30 | -9.39 | -8.90 |
| Ti II | -6.91 | -7.05 | -6.78 | -7.10 | -6.85 | -6.86 | -7.15 | -7.01 |
| V II | -8.03 | -7.64 | -7.88 | -8.04 | -7.46 | -7.31 | -7.79 | -8.00 |
| Cr I | -6.13 | -6.20 | -5.79 | -6.26 | -6.08 | -6.16 | -6.50 | -6.26 |
| Cr II | -6.21 | -6.13 | -5.96 | -6.34 | -6.10 | -6.17 | -6.41 | -6.26 |
| Mn I | ... | ... | ... | -6.84 | -6.53 | -6.42 | -6.89 | -6.45 |
| Mn II | -6.28 | -6.69 | -5.65 | -6.54 | -6.12 | -6.22 | -6.45 | -6.45 |
| Fe I | -4.54 | -4.58 | -4.16 | -4.81 | -4.28 | -4.32 | -4.70 | -4.52 |
| Fe II | -4.58 | -4.47 | -4.37 | -4.71 | -4.34 | -4.35 | -4.63 | -4.52 |
| Co I | ... | ... | ... | ... | ... | -6.54 | -6.67 | -7.08 |
| Ni I | -5.82 | -5.67 | ... | ... | -5.10 | -5.31 | -5.71 | -5.75 |
| Ni II | -5.87 | -5.67 | -5.64 | -5.91 | -5.00 | -5.00 | -5.48 | -5.75 |
| Zn I | ... | ... | ... | ... | -6.00 | ... | ... | -7.40 |
| Sr II | -8.79 | -8.77 | -9.12 | -9.52 | -8.35 | -8.01 | -8.30 | -9.10 |
| Y II | ... | ... | -9.40 | ... | -8.97 | -9.13 | -9.65 | -9.76 |
| Zr II | -8.99 | -9.36 | -8.93 | ... | -8.44 | -8.43 | -8.94 | -9.44 |
| Ba II | ... | -9.29 | -9.69 | -10.07 | -8.62 | -8.49 | -9.29 | -9.87 |
 | 10325 | 10250 | 10135 | 10025 | 9600 | 9600 | 9500 | |
 | 3.70 | 3.90 | 3.69 | 3.75 | 3.83 | 3.60 | 3.75 | |
 (km/s) | 0.3 | 0.0 | 1.8 | 0.0 | 2.5 | 1.8 | 1.6 | |
|
The CASLEO spectrograms for Lep increase the number of lines analyzed
relative to Adelman (1987). Of special interest is the
detection of Hg I (1) 5460.74 whose derived abundance is in excellent
agreement with those from Hg I (1) 4358.34 and Hg II 3983.96. The slight
changes in effective temperature and surface gravity produce minor changes
in the abundances by of order 0.1 dex. The agreement between values
derived from species of the same element is marginally worse suggesting
some further small adjustments in the effective temperature and surface
gravity may be required.
For 7 Sex, the CASLEO spectrograms yield new abundances for C I and Y II lines and improved values especially for Mg I, S II, and Mn II lines. Most abundances are slightly closer to solar (Anders & Grevesse 1989 as updated in Adelman 1996) than the previous study by Adelman & Philip (1996). The CASLEO values confirm the S and Mn overabundances. The discrepancies between the iron values derived from Fe I and Fe II lines can be reduced by making the star slightly cooler. The star appears to be slightly metal rich compared to the Sun and to the other superficially normal stars with effective temperatures near 10000 K in Table 7 (click here) (Adelman 1996 and references therein). This is consistent with the idea that 7 Sex might be the product of a binary having coalest.
New abundances have been derived from O I, Mg I, and P II lines found on the CASLEO spectrograms of HR 4817. The star is both O and Mg normal while being slightly P rich. Further the abundances from Mn I and II lines have been brought in better agreement.
The CASLEO spectrograms for 28 Her increase the number of lines analyzed relative to Adelman (1988). We now have an abunance of O I which suggests a slight deficiency. For the most part the changes in stellar parameters make the star slightly more metal rich.