For HR 4487, the Mg I and Mg II abundances are in acceptable agreement while the difference between the Fe I and Fe II abundances is 0.3 dex. The Mn I and Mn II abundances are in still worse agreement. But the two Mn I lines are weak and thus we believe the result from the Mn II lines. The disagreement between Fe I and Fe II line results suggest that the effective temperature and surface gravity might need a slight adjustment, but we do not have the data to do this. For 14 Hya the Mn I and Mn II lines give similar results. While for 3 Cen A the Si II multiplet 3 lines better agree with the abundance derived from Si III lines than do the Si II multiplet 1 lines which yield larger results. The P II and P III line abundances are in fair agreement while the Fe II and Fe III lines show excellent agreement.
Our results for 3 Cen A compared with those for Jugaku et al. (1969) reflect changes in the gf values over the past 25 years. In Table 4 we compare our results with those of Castelli et al. (1997). For most of the derived elements in common, the agreement is at least acceptable (0.4 dex or better). Our analysis finds O is about 1 dex underabundant while Castelli et al. find a solar value. But the visible region analysis of Hardorp et al. (1968) agrees with our value. Also we find Cr +0.5 dex overabundant compared with their solar value.
In Table 5 (click here) we compare our results with those of some of the hotter HgMn stars and the Sun. Although many of its abundances are similar to those of the hottest HgMn stars, 3 Cen A is 2500 K hotter than any of these which makes a comparison difficult. It is C, O, Mg and Ca underabundant, Si, Fe, and Ni normal, N, A, and Cr overabundant, and P, Mn, and Ga very overabundant. In making these comparisons, the error in He/H is about 0.01 while in those of other elements is typically 0.3 dex.
Considering the errors in the abundances, most of those derived for HR 4487 are within the range of values seen at its effective temperature in other HgMn stars (Table 6 (click here), Adelman et al. 1996; Adelman & Pintado 1997). It is apparently one of the most Si rich members, a result which needs to be confirmed. It may be the most S, Cr, Ni, and Zr rich HgMn star studied with modern analyses.
Compared with other HgMn stars 14 Hya has a relatively mild He underabundance. Its other abundanc generally fall within the range of values seen at its effective temperature except that it is slightly less P rich. Obtaining additional abundances of this star and the other two analyzed in this paper would be desirable.
| 3 | 33 | HR | HR | HR | ||||||
| Species | Cen A | Gem | 7361 |  Cnc | 8349 | 7664 |
 Boo | Sun | ||
| He I | -1.70 | -1.96 | -2.00 | -2.26 | -1.72 | -2.10 | -1.72 | -1 | . | 04 |
| C II | -4.44 | -3.82 | -3.89 | -3.97 | -3.54 | -3.88 | -3.81 | -3 | . | 43 |
| N II | -4.11 | ... | ... | ... | ... | ... | ... | -3 | . | 95 |
| O I | ... | ... | -3.23 | ... | ... | ... | -3.43 | -3 | . | 14 |
| O II | -4.04 | -3.23 | -2.82 | ... | -2.59 | ... | -2.76 | -3 | . | 14 |
| Mg I | ... | ... | ... | -5.17 | -5.27 | ... | -5.20 | -4 | . | 42 |
| Mg II | -5.19 | -4.81 | -5.14 | -5.17 | -4.94 | -5.75 | -4.79 | -4 | . | 42 |
| Al I | ... | ... | ... | ... | -6.29 | ... | ... | -5 | . | 53 |
| Si II | -4.66: | ... | -4.19 | -4.48 | -4.16 | -4.48 | -4.31 | -4 | . | 45 |
| Si III | -4.88 | -4.76 | -4.56 | -4.47 | -4.26 | -4.80 | -4.47 | -4 | . | 45 |
| P II | -4.84 | -4.54 | -4.52 | -4.73 | -4.65 | -4.99 | -5.66 | -6 | . | 55 |
| P III | -5.09 | ... | -4.45 | -4.77 | -4.88 | ... | ... | -6 | . | 55 |
| S II | ... | ... | -5.66 | -5.56 | -5.08 | -5.48 | -5.24 | -4 | . | 67 |
| Ar II | -5.36 | ... | ... | ... | ... | ... | ... | -5 | . | 44: |
| Ca II | -6.38 | ... | -4.93 | -5.67 | -4.95 | -5.55 | -5.17 | -5 | . | 64 |
| Sc II | ... | -7.45 | -7.94 | -8.37 | -7.67 | -9.14 | -7.64 | -8 | . | 90 |
| Ti II | ... | -5.82 | -6.83 | -6.82 | -6.86 | -6.20 | -6.75 | -7 | . | 01 |
| V II | ... | ... | ... | -7.60 | ... | ... | ... | -8 | . | 00 |
| Cr II | -5.75 | -5.89 | -6.15 | -6.42 | -6.11 | -6.70 | -5.69 | -6 | . | 26 |
| Mn I | ... | ... | -3.97 | -4.39 | -4.28 | ... | -4.07 | -6 | . | 45 |
| Mn II | -4.95 | -4.21 | -4.10 | -4.45 | -4.16 | -5.42 | -4.18 | -6 | . | 45 |
| Fe I | ... | -3.80 | -4.23 | -4.49 | -4.65 | -3.96 | -4.84 | -4 | . | 52 |
| Fe II | -4.26 | -3.90 | -4.41 | -4.57 | -4.46 | -4.44 | -4.08 | -4 | . | 52 |
| Fe III | -4.22 | -4.31 | -4.26 | -4.44 | -4.22 | -4.04 | -4.64 | -4 | . | 52 |
| Ni II | -5.59 | ... | -6.21 | -6.18 | -6.11 | -6.15 | -6.77 | -5 | . | 75 |
| Ga II | -5.57 | -6.63 | -4.81 | -4.75 | ... | -6.14 | -4.86 | -9 | . | 12 |
| Sr II | ... | ... | -8.46: | -8.54 | -7.88 | -8.75 | -6.84 | -9 | . | 10 |
| Y II | ... | ... | -7.59 | -8.33 | -7.17 | -8.21 | -6.36 | -9 | . | 76 |
| Zr II | ... | ... | ... | ... | -7.33 | ... | ... | -9 | . | 40 |
| Xe II | ... | -5.55 | -5.22 | -5.60 | ... | ... | ... | (-9 | . | 77) |
| Ba II | ... | ... | ... | ... | ... | ... | ... | -9 | . | 87 |
| Hg I | ... | ... | ... | ... | ... | ... | ... | (-10 | . | 91) |
| Hg II | ... | ... | -6.00 | -5.98 | -5.67 | -7.40 | -5.27 | (-10 | . | 91) |
 | 17500 | 14375 | 13300 | 13125 | 12975 | 12875 | 12700 | |||
| log g | 3.80 | 3.90 | 3.75 | 3.59 | 3.90 | 3.51 | 4.02 | |||
| . | ||||||||||
| Species | Boo |  Lep | 14 Hya | 53 Tau |  Her | 
Her | HR 4487 | HR 4072A | 28 Her | HR 7775 |  Cnc | Sun | . | |
| He I | -1.72 | -1.57 | -1.40 | -1.80 | -1.82 | -1.62 | -1.53 | -1.46 | -2.00 | -1.60 | -1.57 | (-1 | . | 01) |
| C I | ... | ... | ... | ... | ... | ... | -3.47 | -3.37 | ... | ... | ... | -3 | . | 34 |
| C II | -3.81 | -3.68 | ... | -3.95 | -4.07 | -3.58 | -3.13 | -3.23 | -3.94 | -4.10 | -3.88 | -3 | . | 34 |
| O I | -3.43 | ... | ... | ... | ... | ... | -3.24 | ... | -3.37 | -3.58 | ... | -3 | . | 07 |
| O II | -2.76 | ... | ... | ... | ... | ... | ... | ... | ... | ... | ... | -3 | . | 07 |
| Mg I | -5.20 | -5.17 | ... | ... | -5.56 | -5.28 | -4.77 | -4.65 | -5.51 | -4.74 | -4.66 | -4 | . | 42 |
| Mg II | -4.79 | -4.76 | -4.77 | -4.94 | -5.08 | -4.80 | -4.98 | -4.57 | -5.26 | -4.67 | -4.71 | -4 | . | 42 |
| Al I | ... | ... | ... | ... | ... | ... | ... | -6.42 | ... | -6.69 | -6.38 | -5 | . | 53 |
| Al II | ... | ... | ... | ... | ... | ... | ... | -6.85 | ... | ... | ... | -5 | . | 53 |
| Si I | ... | ... | ... | ... | ... | ... | ... | ... | ... | ... | -4.78 | -4 | . | 45 |
| Si II | -4.31 | -4.29 | ... | -4.65 | -4.82 | -4.64 | -4.30 | -4.53 | -4.78 | -4.50 | -4.50 | -4 | . | 45 |
| Si III | -4.47 | -4.22 | ... | -4.59 | -4.85 | ... | ... | ... | ... | ... | ... | -4 | . | 45 |
| P II | -5.66 | -5.41 | -6.07 | ... | -5.82 | ... | ... | -5.54 | -5.60 | -5.59 | ... | -6 | . | 55 |
| P III | ... | ... | ... | ... | ... | ... | ... | ... | ... | ... | ... | -6 | . | 55 |
| S II | -5.24 | -4.68 | -4.72 | -5.34 | -5.29 | -4.91 | -3.94 | -4.64 | -4.35 | -4.72 | -5.05 | -4 | . | 79 |
| Ca I | ... | ... | ... | -5.34 | ... | -5.20 | -5.67 | -5.24 | -6.11 | -5.24 | -6.21 | -5 | . | 64 |
| Ca II | -5.17 | -5.27 | ... | -5.02 | -5.83 | -5.36 | ... | -4.80 | -5.51 | -5.25 | -6.06 | -5 | . | 64 |
| Sc II | -7.64 | -8.43 | ... | -9.54 | -9.06 | -7.47 | -8.13 | -8.40 | ... | -9.55 | -8.19 | -8 | . | 90 |
| Ti II | -6.75 | -6.41 | -5.69 | -5.76 | -6.26 | -6.37 | -6.76 | -6.16 | -6.82 | -6.08 | -6.38 | -7 | . | 01 |
| V II | ... |  -7.44 | ... | ... | ... | ... | ... | -8.68 | ... | -8.18 | -8.20 | -8 | . | 00 |
| Cr I | ... | ... | ... | -5.80 | ... | -5.18 | ... | -5.69 | -5.90 | -5.75 | -5.73 | -6 | . | 33 |
| Cr II | -5.69 | -5.89 | -5.53 | -5.89 | -6.12 | -5.50 | -5.35 | -5.62 | -6.16 | -5.72 | -5.88 | -6 | . | 33 |
| Mn I | -4.07 | -4.58 | -4.46 | -4.45 | -4.70 | -4.92 | -4.35: | -5.51 | -5.62 | -5.83 | -6.21 | -6 | . | 61 |
| Mn II | -4.18 | -4.45 | -4.68 | -4.56 | -4.88 | -5.08 | -5.13 | -5.38 | -5.48 | -5.84 | -5.84 | -6 | . | 61 |
| Fe I | -4.84 | -4.77 | ... | -5.28 | -4.76 | -4.35 | -4.10 | -4.00 | -4.37 | -4.12 | -4.44 | -4 | . | 52 |
| Fe II | -4.88 | -4.62 | -4.67 | -5.24 | -4.85 | -4.59 | -4.39 | -4.08 | -4.35 | -4.22 | -4.60 | -4 | . | 52 |
| Fe III | -4.64 | -4.67 | ... | -4.65 | -4.68 | -4.64 | ... | -3.97 | -4.32 | -4.08 | ... | -4 | . | 52 |
| Ni I | ... | ... | ... | ... | ... | ... | ... | ... | ... | ... | -5.58 | -5 | . | 75 |
| Ni II | -6.77 | -6.32 | ... | -6.49 | -6.77 | -6.26 | -5.07 | -6.62 | ... | -6.60 | -5.62 | -5 | . | 75 |
| Ga II | -4.86 | -4.44: | ... | -6.41 | -5.64 | -6.00 | ... | ... | ... | -5.34 | ... | -9 | . | 12 |
| Sr II | -6.84 | -7.32 | ... | -8.17 | -8.10 | -8.34 | -6.74 | -6.49 | -6.62 | -6.48 | -8.01 | -9 | . | 10 |
| Y II | -6.36 | -7.14 | -7.08 | -8.20 | -7.76 | -6.72 | -7.02 | -6.56 | -6.67 | -6.94 | -7.76 | -9 | . | 76 |
| Zr II | ... | -8.34 | ... | -7.49 | -8.95 | -7.32 | -6.76 | -8.04 | -8.53 | -8.73 | -7.60 | -9 | . | 40 |
| Ba II | ... | ... | ... | -9.55 | -8.85 | -8.06 | ... | -9.14 |
-9.81 | -9.70 | -6.97 | -9 | . | 87 |
| La II | ... | ... | ... | ... | ... | ... | ... | -9.29 | ... | ... | ... | -10 | . | 78 |
| Pr II | ... | ... | ... | ... | ... | ... | ... | ... | ... | -7.72 | ... | -11 | . | 29 |
| Nd II | ... | ... | ... | ... | ... | ... | ... | ... | ... | -7.82 | ... | -10 | . | 50 |
| Gd II | ... | ... | ... | ... | ... | ... | ... | ... | ... | -9.15 | -9.29 | -10 | . | 88 |
| Ho II | ... | ... | ... | ... | ... | ... | ... | ... | ... | -8.90 | ... | -11 | . | 7 |
| Tm II | ... | ... | ... | ... | ... | ... | ... | ... | ... | -9.47 | ... | -12 | . | 00 |
| Pt I | ... | ... | ... | ... | ... | ... | ... | ... | ... | -5.53: | ... | -10 | . | 2 |
| Pt II | ... | ... | ... | ... | ... | ... | ... | -7.32: | -7.68: | -7.23: | ... | -10 | . | 2 |
| Au II | ... | ... | ... | ... | ... | ... | ... | -7.34: | ... | -7.18: | ... | -10 | . | 99 |
| Hg I | ... | -5.75 | ... | ... | -6.02 | -6.33 | ... | -5.67 | ... | -5.90 | ... | (-10 | . | 91) |
| Hg II | -5.27 | -5.65 | ... | ... | -5.76 | -6.38 | ... | -5.83 | -7.80 | -6.06 | -7.80 | (-10 | . | 91) |
|
| 12700 | 12400 | 12000 | 12000 | 11900 | 11325 | 11020 | 10900 | 10900 | 10650 | 10650 | . | ||
| log g | 4.02 | 3.91 | 3.75 | 4.21 | 3.74 | 3.79 | 3.92 | 4.07 | 3.96 | 4.13 | 4.13 | . | ||
| . |
Acknowledgements
OIP is grateful to the staff of CASLEO for their assistance during the observing runs. The authors acknowledge the use of the CCD and data reduction acquisition system supported by US NSF Grant AST 90-15827 to R.M. Rich. SJA thanks The Citadel Development Foundation for several grants which supported in part this collaboration.