Table D.1.
Evolution of spectral lines identified in the orbit-resolved Resolve spectra.
| Line ID | Erest (keV) | orbit | vreal (km s−1) | σ (eV) | Δv (km s−1) | EW (eV) | Δ C-stat |
|---|---|---|---|---|---|---|---|
| slow Fe XXV Lyβ | 7.878 | 1 | - | - | - | ![]() |
2 |
| 2 | −270 ± 230 | - | - | ![]() |
12 | ||
| 3 | - | - | - | ![]() |
6 | ||
| 4 | - | - | - | ![]() |
5 | ||
| 5 | - | - | - | ![]() |
2 | ||
| slow Fe XXVI Lyα1 | 6.973 | 1 |
|
- | - | ![]() |
18 |
| 26 ± 9 | 10 | ||||||
| 2 |
|
|
|
![]() |
33 | ||
![]() |
|||||||
| 3 |
|
- | - | ![]() |
10 | ||
![]() |
|||||||
| slow Fe XXVI Lyα2 | 6.952 | 4 |
|
- | - | ![]() |
7 |
![]() |
|||||||
| 5 |
|
0+4.1 | 0+180 | ![]() |
27 | ||
![]() |
|||||||
| Fe XXV Hew | 6.700 | 1 |
|
|
|
![]() |
29 |
| 75 ± 23 | |||||||
| 2 |
|
- | - | ![]() |
30 | ||
![]() |
|||||||
| 3 |
|
|
|
![]() |
52 | ||
![]() |
|||||||
| Fe XXV Hey | 6.668 | 4 |
|
10−8.4† | 450−380† | ![]() |
18 |
![]() |
|||||||
| 5 |
|
|
|
138 ± 38 | 57 | ||
![]() |
|||||||
| Cr XXIII Hew | 5.682 | 1 | - | - | - | ![]() |
4 |
| 2 | - | - | - | ![]() |
2 | ||
| 3 | - | - | - | ![]() |
2 | ||
| 4 | ![]() |
4.7
|
250
|
![]() |
13 | ||
| 5 | - | - | - | 13 ± 13 | 1 | ||
| Ne X Lyα | 1.022 | 1 | - | - | - | ![]() |
0 |
| 2 | - | - | - | ![]() |
9 | ||
| 3 | - | - | - | 37 ± 10 | 17 | ||
| 4 | - | - | - | 77 ± 18 | 33 | ||
| 5 | - | - | - | ![]() |
35 | ||
Notes. For a more straightforward assessment of changes between orbits, we show the errors with an uncertainty of 1σ. The quoted rest wavelengths are adopted from NIST. The energies of all unresolved lines are taken as the 2/1 mean of the main transitions using the NIST values. For the two line complexes fitted with single transitions, the line shifts and widths between the two transitions are tied. The velocities given include the correction of −117 ± 13 km s−1, sum of all nonintrinsic velocity components within the line of sight (see Appendix A).
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