Table 3
Best-fit parameters of the EPIC spectra of 9 Sgr.
| Purely thermal plasma models with ionization equilibrium (Eq. (2)) | ||||||||
|
|
||||||||
| φ | log Nwind,2 | k T 2 | 104 × norm2 | k T 3 | 104 × norm3 |
|
d.o.f. | |
| (cm-2) | (keV) | (cm-5) | (keV) | (cm-5) | ||||
|
|
||||||||
| 0.627 |
|
|
|
– | – | 1.70 | 229 | |
| 0.946 | 19.90 |
|
|
|
|
1.39 | 268 | |
| 0.000 | 19.90 |
|
|
|
|
1.72 | 310 | |
| 0.055 | 19.90 |
|
|
|
|
1.50 | 293 | |
|
|
||||||||
| Thermal models with non-equilibrium ionization (Eq. (4)) | ||||||||
|
|
||||||||
| φ | log Nwind,2 | k T 2 | 104 × norm2 | k T 3 | 104 × norm3 | 10-10 × τu |
|
d.o.f. |
| (cm-2) | (keV) | (cm-5) | (keV) | (cm-5) | (s cm-3) | |||
|
|
||||||||
| 0.627 |
|
|
|
|
|
|
1.27 | 226 |
| 0.946 | 19.90 |
|
|
|
|
|
1.36 | 267 |
| 0.000 |
|
|
|
|
|
|
1.41 | 309 |
| 0.055 |
|
|
|
|
|
|
1.43 | 292 |
|
|
||||||||
| Models with a power-law component (Eq. (7)) | ||||||||
|
|
||||||||
| φ | log Nwind,2 | k T 2 | 104 × norm2 | Γ3 | 104 × norm3 |
|
d.o.f. | |
| (cm-2) | (keV) | (cm-5) | (photons keV-1 cm-2 s-1) | |||||
|
|
||||||||
| 0.627 | 19.90 |
|
|
|
|
1.36 | 227 | |
| 0.946 | 19.90 |
|
|
|
|
1.36 | 268 | |
| 0.000 | 19.90 |
|
|
|
|
1.46 | 310 | |
| 0.055 | 19.90 |
|
|
|
|
1.46 | 293 | |
Notes. EPIC spectra were fitted for energies between 0.3 and 10.0 keV. The interstellar neutral hydrogen column density was fixed to 0.234 × 1022 cm-2. Each model also included a soft thermal component with fixed parameters: log Nwind,1 = 21.47, kT1 = 0.265 keV, and norm1 = 5.24 × 10-3 cm-5. All abundances were set to solar, except for nitrogen, which was taken to be 2.7 times solar. The normalization of the thermal models is given as 
(cm-5), where ne and nH are the electron and proton densities of the X-ray emitting plasma in cm-3, and D is the distance in cm. The normalization of the power-law component is expressed as the number of photons keV-1 cm-2 s-1 at 1 keV. The quoted error bars correspond to the 90% confidence level.
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