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Table 7
Column densities as calculated from the sulfur line equivalent widths.
| NH-like | NHe-like | NLi-like | NBe-like | NB-like | NC-like | NN-like | NO-like | NS | NH,Wilms | NH,Herrero (a) | ||
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (1015 cm −2) | (1015 cm−2) | (1021 cm−2) | (1021 cm−2) | |||||||||
| 3814 | Non-dip | 47 ± 8 | 18 ± 4 | 2.2 ± 1.6 | 0.9 ± 0.6 | 0.9 ± 0.5 | 1.5 ± 0.5 | – | – | 71 ± 18 | 2.0 ± 0.5 | 0.79 ± 0.19 |
| Weak dip | 43 ± 17 | 20 ± 8 | 5 ± 4 | – | 1.6 ± 1.0 | 1.6 ± 1.1 |  |
– | 70 ± 40 | 2.1 ± 1.1 | 0.8 ± 0.5 | |
| Dip | 64 ± 14 | 30 ± 7 | 5.8 ± 2.9 | 2.2 ± 1.1 | 2.3 ± 0.9 |  |
3.9 ± 1.9 | – | 110 ± 40 | 3.1 ± 0.9 | 1.2 ± 0.4 | |
| Strong dip | 36 ± 15 | 8 ± 8 | – | 1.5 ± 1.2 |  |
4.9 ± 0.9 | 3.7 ± 2.0 | – | 60 ± 40 | 1.6 ± 1.0 | 0.6 ± 0.4 | |
| 8525 | Non-dip | 55 ± 16 | 33 ± 7 | – | 1.5 ± 1.1 | 2.1 ± 1.0 | 2.4 ± 0.9 | – | – | 90 ± 40 | 2.8 ± 1.0 | 1.0 ± 0.4 |
| Weak dip | 68 ± 17 | 26 ± 8 | 6 ± 4 | 2.1 ± 1.2 | 4.6 ± 0.9 | 2.7 ± 1.0 | – | – | 110 ± 40 | 3.1 ± 1.1 | 1.2 ± 0.5 | |
| Dip | 53 ± 16 | 24 ± 8 |  |
2.6 ± 1.1 | 3.9 ± 0.9 | 4.4 ± 0.9 |  |
– | 100 ± 40 | 2.9 ± 1.1 | 1.1 ± 0.4 | |
| Strong dip |  |
21 ± 8 | – | – | 2.1 ± 1.0 | 4.0 ± 1.0 |  |
– | 70 ± 40 | 2.1 ± 1.1 | 0.8 ± 0.4 | |
| 9847 | Non-dip | 56 ± 14 | 14 ± 8 | – | 1.5 ± 1.1 | 1.2 ± 0.9 | 1.5 ± 0.9 | – | – | 70 ± 40 | 2.1 ± 0.9 | 0.8 ± 0.4 |
| Weak dip | – | 33 ± 9 | – | 3.2 ± 1.3 | 4.0 ± 1.1 | 3.4 ± 1.1 | – | – | 44 ± 19 | 1.2 ± 0.6 | 0.49 ± 0.21 | |
| Dip |  |
 |
– | 3.6 ± 1.3 | 3.8 ± 1.1 | 5.2 ± 1.0 | 5.8 ± 2.1 | – | 90 ± 50 | 2.5 ± 1.2 | 1.0 ± 0.5 | |
| Strong dip | 42 ± 19 | 11 ± 10 | 4 ± 4 | 3.6 ± 1.3 | 5.5 ± 1.0 | 5.1 ± 1.1 | 7.1 ± 2.2 | 8 ± 6 | 90 ± 50 | 2.5 ± 1.3 | 1.0 ± 0.5 | |
Notes. (a) Herrero et al. (1995) provide a scaling factor for the observed overabundance of helium, which we apply to the solar abundances of Wilms et al. (2000). See text for further details.
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