Table 3
Summary of fit to extracted XMM-Newton source and background spectra of G5.9+3.1 using TBABS × APEC model.
| Parameter | Whole SNR | East rim | North rim | West rim |
|---|---|---|---|---|
| Source spectrum fit parameters | ||||
| NH (1022 cm−2) | 0.80 ± 0.04 | 0.75 |
0.84 |
0.80 |
| kT (keV) | 0.15 |
0.14 |
0.17 |
0.23 |
| Abundance (Solar) | 1.00 (Frozen) | 1.00 (Frozen) | 1.00 (Frozen) | 1.00 (Frozen) |
| Normalization (cm−5) | 4.15 × 10−2 | 5.81 × 10−3 | 1.89 × 10−3 | 2.40 × 10−3 |
| Astrophysical X-ray background spectrum fit parameters | ||||
| Constant (PN-SRC) | 1.00 (Frozen) | 1.00 (Frozen) | 1.00 (Frozen) | 1.00 (Frozen) |
| Constant (PN-BKG) | 1.00 (Frozen) | 1.00 (Frozen) | 1.00 (Frozen) | 1.00 (Frozen) |
| Constant (MOS1-SRC) | 0.85 (Frozen) | 0.85 ± 0.04 | 0.85 (Frozen) | 0.83 ± 0.05 |
| Constant (MOS1-BKG) | 0.85 (Frozen) | 0.85 ± 0.04 | 0.85 (Frozen) | 0.83 ± 0.05 |
| Constant (MOS2-SRC) | 0.85 (Frozen) | 0.83 ± 0.04 | – | – |
| Constant (MOS2-BKG) | 0.85 (Frozen) | 0.83 ± 0.04 | – | – |
| kTHalo (keV) | 0.30 |
0.29 |
0.28 |
0.28 |
| Abundance (Solar) | 1.00 (Frozen) | 1.00 (Frozen) | 1.00 (Frozen) | 1.00 (Frozen) |
| NormalizationHalo (cm−5) | 1.35 × 10−2 | 1.58 × 10−3 | 2.62 × 10−3 | 2.89 × 10−3 |
| ΓDXB | 1.46 (Frozen) | 1.46 (Frozen) | 1.46 (Frozen) | 1.46 (Frozen) |
| NormalizationDXB | 1.60 × 10−3 | 1.64 × 10−4 | 2.12 × 10−4 | 2.83 × 10−4 |
| kTLHB (keV) | 0.10 (Frozen) | 0.10 (Frozen) | 0.10 (Frozen) | 0.10 (Frozen) |
| Abundance (Solar) | 1.00 (Frozen) | 1.00 (Frozen) | 1.00 (Frozen) | 1.00 (Frozen) |
| NormalizationLHB (cm−5) | 2.42 × 10−3 | 2.60 × 10−4 | 3.62 × 10−4 | 4.55 × 10−4 |
| C-Statistic | 5510.72 | 3230.99 | 3614.57 | 3517.77 |
| Degrees of freedom | 5473 | 4033 | 3675 | 3674 |
Notes. All quoted error bounds correspond to the 90% confidence levels. In the case of the APEC model, the normalization is defined as (1014 /4πd2) ∫ nenpdV, where d is the distance to the SNR (in units of centimeters), ne and np are the number densities of electrons and protons respectively (in units of cm−3), and finally ∫ dV = V is the integral over the entire volume (in units of cm3). In the case of the power-law model, the normalization is defined as photons keV−1 cm−2 s−1 at 1 keV (see Sect. 5).
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