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Table 4
Absorption line detections for Chandra non-dip spectrum.
| Ion | Transitiona | E lab | E obs | Shift | Width | Fluxb | EQWc |
| eV | eV | km s-1 | eV | (10-4) | eV | ||
|
|
|||||||
| Mg xii | 1s − 2p | 1472.3 | 1474.0 |
350 |
1.5 ± 1.5 | 6.5 ± 3 | 0.8 ± 0.3 |
| Al xiii | 1s − 2p | 1728.6 | 1727.2 ± 2.6 | −240 ± 450 | 1.6 |
5 ± 2.5 | 0.6 ± 0.3 |
| Mg xii | 1s − 3p | 1744.7 | 1745.4 ± 1.2 | 140 ± 200 | 1.0 |
6.0 ± 2.0 | 0.9 ± 0.3 |
| XAFS | 1847.7 ± 0.7 | 2.2 ± 0.8 | 11.6 ± 2.4 | 2.0 ± 0.4 | |||
| XAFS | 1863.7 ± 1.0 | 2.4 ± 1.4 | 9 ± 2 | 1.8 ± 0.3 | |||
| Si xiv | 1s − 2p | 2005.5 | 2007.4 ± 0.4 | 280 ± 60 | 2.6 ± 0.6 | 14.4 |
2.7 ± 0.5 |
| S xvi | 1s − 2p | 2621.7 | 2623.4 |
200 |
0+4 | 6.0 ± 1.4 | 1.2 ± 0.4 |
| Ca xx | 1s − 2p | 4105.0 | 4118 ± 8 | 950 ± 600 | 13 ± 10 | 6.0 ± 2.5 | 2.4 ± 1.1 |
| Fe xxv | 1s2 − 1s2p | 6700.4 | 6706 ± 5 | 250 ± 220 | 8 ± 8 | 9.6 ± 2 | 12 ± 3 |
| Fe xxvi | 1s − 2p | 6966.2 | 6978 ± 3 | 500 ± 130 | 20.4 ± 5 | 25.2 ± 3 | 36 ± 5 |
| Fe xxvi | 1s − 3p | 8250.2 | 8273 ± 20 | 840 ± 730 | 25 ± 25 | 10 ± 5 | 22 ± 12 |
Notes. An absorbed (tbvarabs) continuum model of thermal disk emission and thermal Comptonization is used.
(a)
Rest-frame energies from Verner et al. (1996).
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