Table 4
Results of the fits of the XIS and HXD data with a power law (top part) or eqpair (bottom part) for the continuum and the ionized reflection component reflionx.
| tbnew*(diskbb+po+kdblr*reflionx) | ||||||||||||
| Obs. | N h | T diskbb | N diskbb | F diskbb | Γ | F po | R in | ξ ref | F ref |
|
χ2/d.o.f. | |
| × 1022 | eV | × 104 | × 10-11 | × 10-10 | R g | × 10-11 | % | |||||
|
|
||||||||||||
| 1 | 0.42 |
430 |
0.03 |
11.8 | 1.73 |
13.7 | 15 |
1000 |
11.3 | 0.89 | 806/517 | |
| 2 | 0.64 |
220 |
0.33 |
3.5 | 1.67 |
9.0 | 40 |
230 |
11.1 | 0.56 | 601/517 | |
| 3 | 0.67 |
110 |
6.10 |
0.4 | 1.59 |
4.0 | >70 | 1100 |
3.8 | 0.25 | 522/514 | |
| 4 | 0.75 |
125 |
1.84 |
0.4 | 1.63 |
3.0 | >10 | 790 |
2.1 | 0.20 | 554/507 | |
| 5 | 0.82 |
<240 | < 2.13 | <2.6 | 1.63 |
2.1 | >30 | 1400 |
2.0 | 0.13 | 483/476 | |
|
|
||||||||||||
| 2008 | 0.79 |
80 |
64.64 |
0.1 | 1.65 |
1.9 | >180 | 20 |
3.0 | 0.13 | 527/517 | |
| tbnew*(diskbb+eqpair+kdblr*reflionx) | ||||||||||||
| Obs. | N h | T diskbb | F diskbb | lh/ls | τ | T bb | F eqpair | R in | ξ ref | F ref |
|
χ2/d.o.f. |
| × 1022 | eV | × 10-11 | eV | × 10-10 | R g | × 10-11 | % | |||||
|
|
||||||||||||
| 1 | 0.46 |
310 |
16.0 | 5.1 |
0.6 |
590 |
11.9 | 7.0 |
2000 |
28.8 | 0.91 | 704/515 |
| 2 | 0.62 |
240 |
7.0 | 5.7 |
2.3 |
470 |
9.3 | 32 |
270 |
7.8 | 0.60 | 544/515 |
| 3 | 0.75 |
110 |
0.8 | 9.6 |
2.1 |
210 |
4.0 | >70 | 1180 |
4.6 | 0.25 | 519/512 |
| 4 | 0.78 |
175 |
1.3 | 6.4 |
2.4 |
390 |
3.1 | >10 | 910 |
1.7 | 0.19 | 546/505 |
| 5 | 0.93 |
130 |
0.7 | 7.7 |
1.9 |
240 |
2.1 | >30 | 1450 |
2.3 | 0.13 | 475/474 |
|
|
||||||||||||
| 2008 | 0.84 |
80 |
0.2 | 7.9 |
2.1 |
190 |
2.0 | >180 | 40 |
3.2 | 0.13 | 525/515 |
Notes. In the case of the power law fit, the photon index used in reflionx is fixed to the one of the power law continuum. In the case of eqpair, we froze the photon index of reflionx to the one obtained in the power law fit. The inclination was fixed to 20 deg. We use the kernel from the laor line profile to account for the gravitational effects close to the black hole (model kdblur) of xspec. All errors have a 90 per cent confidence for one parameter. The fluxes are in units of erg cm-2 s-1 and are computed in the 0.7−70 keV energy range. The bolometric luminosity Lbol is assumed to be the sum of the luminosities of the three spectral component diskbb, eqpair and reflionx. We adopt an Eddington luminosity of LEdd ≃ 1.3 × 1039 erg s-1 (i.e. we assume a 10-solar-mass black hole) and a distance to GX 339-4 of 8 kpc.
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