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Table 5.

Best-fitting parameters of the primary continuum and details of the iron Kα line parameters for the analysis of the spectra of IC 4329A from previous XMM-Newton and Suzaku observations as in Table 4.

Obs.ID kTBB [keV] Γ EFe Kα [keV] σFe Kα[eV] EWFe Kα [eV] log(F) log(F2 − 10) χ r 2 $ \chi^2_r $
0101040401 0.08 ± 0.01 1.68 ± 0.08 −9.46 ± 0.55 0.97
0147440101 0.42( * ) ± 0.01 1.71 ± 0.01 6.35 ± 0.04 96 ± 17 87 ± 5 −12.12 ± 0.03 −10.03 ± 0.01 1.74
0702113010 0.08 ± 0.05 1.84 ± 0.01 6.38 ± 0.03 115 ± 32 84 ± 20 −11.98 ± 0.07 −9.97 ± 0.03 1.04
0702113020 0.03 ± 0.02 1.88 ± 0.02 6.40 ± 0.02 82 ± 12 48 ± 12 −12.32 ± 0.07 −9.89 ± 0.01 1.10
0702113030 0.07 ± 0.01 1.77 ± 0.01 6.37 ± 0.04 71 ± 6 42 ± 12 −12.08 ± 0.08 −9.92 ± 0.03 1.08
0702113040 0.07 ± 0.01 1.85 ± 0.01 6.39 ± 0.04 78 ± 4 47 ± 15 −12.15 ± 0.10 −9.96 ± 0.04 1.06
0702113050 0.06 ± 0.01 1.74 ± 0.01 6.36 ± 0.05 67 ± 10 96 ± 21 −12.41 ± 0.12 −10.16 ± 0.01 1.04
0707025010 0.06 ± 0.02 1.75 ± 0.01 6.36 ± 0.06 77 ± 14 51 ± 27 −12.04 ± 0.03 −9.96 ± 0.01 1.10
08800760801 0.11 ± 0.05 1.63 ± 0.03 6.39 ± 0.03 < 140 81 ± 13 −11.91 ± 0.03 −10.17 ± 0.24 0.93

Notes. The errors are at the 90% confidence levels. The FeKα flux and the 2–10 keV flux are given in units of erg cm−2 s−1. ( * )The higher value of the kTBB of this Obs.ID is not related to the variability in the soft excess, but it is most likely due to the higher NH value of the UFO component (see Table 6), which could drive the blackbody shape of the soft excess.

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