Best-fit parameters of our model for the broadband continuum and the Fe Kα line of NGC 7469, obtained from the 2002 and 2015 Chandra HETGS, HST COS and Swift UVOT observations.
|Primary power-law component (pow):|
|Normalisation||5.3 ± 0.1 (2002), 7.1 ± 0.1 (2015)|
|Photon index Γ||1.91 ± 0.01|
|Disk + soft X-ray excess component (comt):|
|Normalisation||6.5 ± 0.3 (2002), 5.7 ± 0.3 (2015)|
|Tseed (eV)||1.4 ± 0.1|
|Te (keV)||0.14 ± 0.02|
|Optical depth τ||21 ± 4|
|Resolved Fe Kα component (refl):|
|Incident power-law Norm.||12 ± 4 (2002), 10 ± 4 (2015)|
|Incident power-law Γ||1.91 (f)|
|Reflection scale s||0.30 ± 0.10|
|σv (km s-1)||2700 ± 800|
|Unresolved Fe Kα component (delt):|
|Flux (10−13 erg cm−2 s−1)||1.2 ± 0.3|
|E0 (keV)||6.396 ± 0.005|
|σv (km s-1)||<460|
Notes. The power-law normalisation of pow and refl components is in units of 1051 photons s−1 keV−1 at 1 keV. The normalisation of the warm Comptonisation component (comt) is in units of 1055 photons s−1 keV−1. The exponential high-energy cut-off of the power-law for both pow and refl is fixed to 170 keV (based on NuSTAR measurements). The photon index Γ of the incident power-law for the reflection component (refl) is set to the Γ of the observed primary power-law continuum (pow). The parameters that have been coupled between the two epochs in our modelling have a single value in the table.
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