Table 1
Results of the profile fitting for the two components in the α Leo sight line.
| Component | 1 (LIC) | 2 | Total line of sight | N(LIC)/Ntotal |
|
|
||||
| Vheliocentric (km s-1) | 8.8 ± 0.2 | 14.4 ± 0.1 | ||
| VLSR (km s-1) | 2.7 ± 0.2 | 8.3 ± 0.1 | ||
| T (K) | 6000 ± 600 | 5990 ± 700 | ||
| bturb(km s-1) | 1.78 ± 0.10 | 1.85 ± 0.19 | ||
|
|
||||
| N(C ii) | 4.5  |
2.2 |
6.7 |
0.67 |
| N(C ii*) | 2.9 ± 0.2 × 1012 | 6.6  |
3.54 ± 0.16 × 1012 | 0.82 ± 0.09 |
| N(C iv) | < 5 × 1011 | < 5 × 1011 | ||
| N(C iv)a (T = 200 000) | < 2 × 1012 | |||
| N(N i) | 7.2 ± 0.2 × 1013 | 3.3 ± 0.2 × 1013 | 1.05 ± 0.03 × 1014 | 0.69 ± 0.04 |
| N(N ii) | 7.0 |
|||
| N(N v) | < 6.8 × 1011 | < 6.8 × 1011 | ||
| N(N v)a (T = 200 000) | < 2.5 × 1012 | |||
| N(O i) | 9.5  |
2.0 ± 0.2 × 1014 | 1.15 |
0.83 |
| N(O vi)b | < 3.1 × 1012 | |||
| N(Mg i) | 2.3 ± 0.7 × 1010 | 1.0 ± 0.7 × 1010c | 3.3 |
0.70 |
| N(Mg ii) | 4.9 ± 0.2 × 1012 | 1.64 ± 0.06 × 1012 | 6.5 ± 0.2 × 1012 | 0.75 ± 0.05 |
| N(Al ii) | 1.85 ± 0.17 × 1011 | 1.00 ± 0.17 × 1011 | 2.84 ± 0.11 × 1011 | 0.65 ± 0.09 |
| N(Al iii) | < 6.8 × 1010 | < 6.8 × 1010 | ||
| N(Si ii) | 1.00 ± 0.06 × 1013 | 3.02 ± 0.30 × 1012 | 1.30 ± 0.06 × 1013 | 0.77 ± 0.08 |
| N(Si iii) | < 8.0 × 1011 | < 8.0 × 1011 | ||
| N(Si iv) | < 1.6 × 1011 | < 1.6 × 1011 | ||
| N(Si iv)a (T = 200 000) | < 4 × 1011 | |||
| N(S ii) | 1.94 ± 0.21 × 1013 | 4.9 ± 2.7 × 1012d | 2.44 ± 0.24 × 1013 | 0.80 ± 0.16 |
| N(S iii) | < 8.8 × 1012 | < 8.8 × 1012 | ||
| N(Ar i) | 1.86 ± 0.07 × 1012 | |||
| N(Ca ii)e | 5 × 109 | |||
| N(Fe ii) | 1.82 ± 0.03 × 1012 | 6.3 ± 0.3 × 1011 | 2.45 ± 0.03 × 1012 | 0.74 ± 0.02 |
|
|
||||
| N(H i)f (apparent column density for the 2-component model) | 6.6 ± 1.0 × 1018f | |||
Notes. The intervals indicate 1σ uncertainties.
Estimated for T ≃ 200 000, in the case it originates in an interface between the cloud and the surrounding hot gas;
from Rogerson et al. (1973b);
from Frisch et al. (2002);
Based on the Lyman-α absorption profile, which we believe overstates N(H I). See Sect. 6.5.
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