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El. | 11583 | 12404 | 13415 | 16149 | 18646 | 8745 | 24938 |
![]() |
[El/H] |
HeI | <11.1 | 10.89 ![]() |
- | - | 10.90 ![]() |
10.84 ![]() |
10.99 ![]() |
10.91 ![]() |
- |
OI | 7.56 ![]() |
7.84 ![]() |
7.82 ![]() |
7.73 ![]() |
7.86 ![]() |
7.83 ![]() |
7.87 ![]() |
- | - |
OI
![]() |
7.41 ![]() |
7.70 ![]() |
7.68 ![]() |
7.56 ![]() |
7.72 ![]() |
7.68 ![]() |
7.70 ![]() |
7.67 ![]() |
-1.16 ![]() |
NaI | 5.35 ![]() |
4.72 ![]() |
4.78 ![]() |
4.65 ![]() |
4.85 ![]() |
4.60 ![]() |
4.71 ![]() |
- | - |
NaI
![]() |
5.15 ![]() |
4.52 ![]() |
4.58 ![]() |
4.45 ![]() |
4.65 ![]() |
4.40 ![]() |
4.51 ![]() |
4.52 ![]() |
-1.81 ![]() |
SiII | 6.17 ![]() |
6.31 ![]() |
6.24 ![]() |
6.20 | 6.28 ![]() |
6.25 ![]() |
6.18 | 6.23 ![]() |
-1.32 ![]() |
TiII | 3.61 ![]() |
3.74 ![]() |
3.64 ![]() |
3.58 ![]() |
3.71 ![]() |
3.60 ![]() |
3.60 | 3.64 ![]() |
-1.38 ![]() |
CrII | 3.92 ![]() |
4.17 ![]() |
4.06 ![]() |
3.96 ![]() |
4.00 ![]() |
3.98 ![]() |
4.12 | 4.03 ![]() |
-1.64 ![]() |
FeI | 5.83 ![]() |
6.14 ![]() |
5.97 ![]() |
5.82 ![]() |
6.08 ![]() |
5.91 ![]() |
- | 5.96 ![]() |
-1.54 ![]() |
FeII | 5.81 ![]() |
6.01 ![]() |
5.95 ![]() |
5.92 ![]() |
5.95 ![]() |
5.89 ![]() |
5.94 ![]() |
5.92 ![]() |
-1.58 ![]() |
BaII | 0.25 | - | 0.45 | 0.55 | - | - | - | 0.42 ![]() |
-1.71 ![]() |
In the two last columns we give the average abundances and the average abundances relative to the Sun. In the calculation of the average abundances of O and Na we rejected the star #11583 because its O and Na contents deviate from the general trend (see text). For #11583 we give an upper limit for the He abundance, which is useful for the discussion, see Sect. 6. Errors for He abundance were obtained as described in Sect. 6. |
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