Table 7
Comparison of three different self-consistent, relativistically smeared reflection models (reflionx, xillver and pexriv) applied to the XMM-Newton, BeppoSAX, and RXTE spectra of 4U 1705−44 in the soft state.
| Component | Parameter | Reflionx | Xillver | Pexriv | ||
|
|
||||||
| phabs | NH (× 1022 cm-2) | 2.08 ± 0.02 | 2.04 ± 0.01 | 1.91 ± 0.02 | ||
| bbody | kTbb (keV) | 0.56 ± 0.01 |
|
0.52 ± 0.01 | ||
| bbody | Norm (× 10-2) | 2.58 ± 0.01 | 1.7 ± 0.01 | 2.94 ± 0.01 | ||
| nthComp | Γ | 2.6 ± 0.1 | 2.6 (frozen) | 2.3 ± 0.1 | ||
| nthComp | kTe (keV) | 3.0 ± 0.1 | 2.9 ± 0.1 | 2.6 ± 0.1 | ||
| nthComp | kTseed (keV) | 1.30 ± 0.02 |
|
|
||
| nthComp | Norm | 0.14 ± 0.01 | 0.11 ± 0.01 | 0.17 ± 0.01 | ||
| rdblur | Betor | −2.1 ± 0.1 | −2.1 ± 0.1 | −2.3 ± 0.1 | ||
| rdblur | Rin (GM/c2) | 13 ± 3 |
|
|
||
| rdblur | Rout (GM/c2) | 3500 (frozen) | 3500 (frozen) | 3500 (frozen) | ||
| rdblur | i (°) | 37 ± 2 | 26 ± 1 |
|
||
| edge | E (keV) | 8.7 ± 0.1 | 8.5 ± 0.1 | − | ||
| edge | Max τ (× 10-2) | 4.2 ± 0.6 | 3.4 ± 0.5 | − | ||
| gauss | E (keV) | − | − | 2.6 (frozen) | ||
| gauss | Norm (× 10-3) | − | − | 1.4 ± 0.2 | ||
| gauss | E (keV) | 3.31 ± 0.01 | − |
|
||
| gauss | Norm (× 10-3) | 1.4 ± 0.2 | − | 1.9 ± 0.2 | ||
| gauss | E (keV) | 3.92 ± 0.02 | − |
|
||
| gauss | Norm (× 10-3) | 1.4 ± 0.2 | − | 2.0 ± 0.2 | ||
| gauss | E (keV) | − | − | 6.63 ± 0.01 | ||
| gauss | Norm (× 10-3) | − | − | 4.1 ± 0.1 | ||
| highecut | cutoffE (keV) | 0.1 (frozen) | 0.1 (frozen) | − | ||
| highecut | foldE (keV) | 8.1 (2.7*kTe of nthComp) | 7.7 (2.7*kTe of nthComp) | 7.0 (2.7*kTe of nthComp) | ||
| reflection | Γ | 2.6 (=Γ of nthComp) | − | 2.3 (=Γ of nthComp) | ||
| reflection | Norm | (8 ± 1) × 10-6 | (1.5 ± 0.1) × 10-5 | 1.218 (frozen) | ||
| reflection | Fe/Solar |
|
1 (frozen) |
|
||
| reflection | Ar, Ca Abund | 1 (frozen) |
|
1 (frozen) | ||
| reflection | ξ (erg cm s-1) |
|
|
|
||
| pexriv | Rel-refl | − | − |
|
||
Total  (d.o.f.) |
1.17 (1573) | 1.26 (1576) | 1.16 (1570) | |||
Notes. The model used is const*phabs*rdblur*edge*(bbody+nthcomp+gauss+gauss+ gauss+gauss+highecut*reflection). For the pexriv model, the disk inclination is fixed to cosi = 0.78 and the disk temperature to 106 K. Here we present the best fit parameters we obtain for the XMM-Newton spectrum. A few parameters of the continuum got different best fit values for the nonsimultaneous BeppoSAX and RXTE spectra, as detailed in Table 2.
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