Table 4
Spectral parameters obtained from the fit of the physical model in Sect. 4.2.1 to the averaged and dip EPIC-pn spectra of IGR J17451–3022 (see text for details).
Parameter | Value | |
|
||
(units) | Steady emission | Dips |
|
||
tbabs | ||
NH (1022 cm-2) |
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|
||
edge | ||
Eedge (keV) |
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8.14† |
τ |
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0.44† |
|
||
warmabs | ||
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log (ξ) (erg cm s-1) |
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Si |
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S |
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Ar |
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Ca |
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K | 0†† | 0† |
Cr |
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Mn |
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Fe |
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σv (km s-1) |
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![]() |
v (km s-1) |
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![]() |
|
||
Gaussian | ||
E6 (keV) |
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6.20† |
σ6 (keV) | 0† | 0† |
EW6 (keV) |
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|
||
Gaussian | ||
E7 (keV) |
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5.71† |
σ7 (keV) | 0† | 0† |
EW7 (keV) | –0.017 ± 0.007 |
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|
||
diskBB | ||
kTdiskbb (keV) |
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1.21 ± 0.01 |
N diskbb |
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![]() |
|
||
F0.5−10 keV |
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(Unabsorbed flux†††) | (5.6) | (5.3) |
χ2/ν (d.o.f) | 1.32 (121) | 0.99 (107) |
Notes. The model in Xspec is tbabs*cabs*edge*warmabs *(gaussian+gaussian+diskbb). Here, is the column density of the warm absorbing material, log (ξ) its ionization status, σv its turbulent velocity broadening, v the bulk velocity shift, and EW the equivalent width of the Gaussian lines. The abundance of each element is indicated as a fraction of the corresponding solar value.
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