Table 3
Detected absorption or emission lines (unresolved) in the time-averaged RGS 1 and RGS 2 spectra.
| Ion | Eref | Line energy | Normalization | ΔC | Instrument |
|---|---|---|---|---|---|
| [eV] | [eV] | [10−5 ph cm−2 s−1] | |||
| O VII He-α (i) | 568.7(a) | 569.4 |
2.2 |
10.4 | RGS 1 |
| O VIII Lyα | 654.12(b) | 653.8 |
2.1 |
18.0 | RGS 1 |
| O VIII Lyα | 654.12(b) | 653.4 |
1.6 |
38.6 | RGS 2 |
| Ne IX (f) | 905.74(b) | 904.8 |
1.8 |
28.2 | RGS 2 |
| Ne IX (i) | 915.58(b) | 916.2 |
3.7 |
96.5 | RGS 2 |
| Ne X Lyα | 1022.60 (c) | 1022.9 |
3.4 |
42.9 | RGS 2 |
| Fe L XXIV (?) | 1109.379(d) | 1114.2 |
2.6 |
15.1 | RGS 2 |
| Mg XI (f/i/r) | 1332.11/1344.33/1353.26(b) | 1348.1 |
3.5 |
31.3 | RGS 2 |
| Mg VI Kα | 1276.81(e) | 1275.4 |
–3.7 |
6.3 | RGS 2 |
| Mg VII Kα | 1289.95(e) | 1293.1 |
–6.1 |
10.7 | RGS 2 |
Notes. The statistical significance of the lines is denoted by ΔC, i.e., the difference of the model C-statistic value with and without the line. The error bars were calculated for a 90% confidence interval and two interesting parameters. The line at 1114.24 eV is presumably identified as a Fe L XXIV line, hence, the question mark (see Sect. 4.3.3 for discussion).
References.(a) Grant et al. (1980), (b) Drake (1988), (c) Erickson (1977), (d) Brown et al. (2002), (e) From Behar & Netzer (2002); value for MgVII Kα averages over the two strong transitions listed there.
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