Table 1.
Best-fitting spectral parameters derived from our modeling of Obs.
| Component | Parameter | Time intervals |
||
|---|---|---|---|---|
| Total | QPO intervals | Non-QPO intervals | ||
| constant | CLE |
 |
 |
 |
| CME |
 |
 |
 |
|
| CHE | [1.00] | [1.00] | [1.00] | |
| diskbb | Tin (keV) |
 |
 |
 |
| Ndiskbb (km2) |
 |
 |
 |
|
| Rin (km) |
 |
 |
 |
|
| gaussian | ELine (keV) |
 |
 |
 |
| σ (keV) |
 |
 |
 |
|
| Nline |
 |
 |
 |
|
| relxill | Γ |
 |
 |
 |
| log ξ |
 |
 |
 |
|
| ZFe/ZFe,⊙ |
 |
 |
 |
|
| Ecut (keV) |
 |
 |
 |
|
| refl_frac |
 |
 |
 |
|
| Nrelxill |
 |
 |
 |
|
| χ2/ν | 1352/1369 (0.99) | 1273/1369 (0.93) | 1218/1369 (0.89) | |
| f2 − 150 (10−7 erg cm−2 s−1) | 1.07 ± 0.02 | 1.07 ± 0.02 | 1.07 ± 0.02 | |
| L2 − 150 (1038 erg s−1) | 1.1 ± 0.1 | 1.1 ± 0.1 | 1.1 ± 0.1 | |
Notes. Errors are 90% confidence limits for one interesting parameter. For the diskbb model, Rin ≡ 1.19rin = (Ndiskbb)1/2 (cos i)−1/2 (d/10 kpc) (Kubota et al. 1998), and we assumed a distance d = 2.96 kpc and a viewing angle i = 63°. f2 − 150 is the observed flux in 2–150 keV band, and L2 − 150 is the unabsorbed luminosity for isotropic emission. Fluxes and luminosities were computed with the cflux model in XSPEC. ID: P011466101502 for the full time interval and for those with and without a QPO signal.
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