Table 4
Results of spectral fitting of blackbody models.
| Model |  (d.o.f.) |
N H |
|
|
ϵ 1 | ϵ 2 | F X ‡ |
 †
|
 †
|
| (× 1021 cm-2) | (eV) | (eV) | (keV) | (keV) | ( erg s-1 cm-2) | (km) | (km) | ||
|
|
|||||||||
| (A) | 1.98 (169) | 3.20(15) | – | 133.1(1.9) | – | – |
|
– |
|
| (B) | 1.34 (167) | 5.3(3) |
|
117.8(2.2) | – | – |
|
a
|
|
| (C) | 1.48 (168) | 3.75(17) | – | 121.3(2.1) | – | – |
|
– |
|
| (D) | 1.08 (165) |
|
– | 157(5) | – |
|
|
– |
|
| (E) | 1.03 (165) | 2.16(20) | – | 144(3) |
|
|
|
– | 2.5(4) |
| (F) | 1.02 (165) |
|
36(4) | 150(5) | – |
|
|
b
|
|
Notes. Errors are 1σ confidence levels. All tbabs models assume Wilms et al. (2000) abundances. Models: (A) tbabs(bbody); (B) tbabs(bbody+bbody); (C) vphabs(bbody), with best-fit oxygen overabundance of ZO = 1.60(7) in solar units; (D) vphabs(bbody+gauss), with ZO = 1.64(12), best-fit Gaussian σ ~ 0.2 keV, and line equivalent width of EW ~ 220 eV; (E) tbabs(bbody+gauss+gauss), with fixed Gaussian σ1 = 0.1 keV and σ2 = 0.2 keV, and EW1 ~ 90 eV and EW2 ~ 120 eV; (F) tbabs(bbody+bbody+gauss), with fixed Gaussian σ2 = 0.2 keV and EW2 ~ 210 eV.
The radiation radii are estimated normalising the distance to the source to that of Eta Carinae, dCar = 2.3 kpc.
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