Table 2.
Best-fit parameters of the intrinsic broadband SED.
| Comp. | Parameter | Obs1 | Obs2 | Obs3 | Obs4 | Obs5 | Obs6 |
|---|---|---|---|---|---|---|---|
| dbb | Normalization A (1026 cm2) | 5.87 (s) | 7.51 (s) | 7.15 (s) | 6.87 (s) | 7.27 (s) | 7.39 (s) |
| comt | Normalization (1054 ph s−1 keV−1) |
 |
 |
0.50 ± 0.15 |
 |
 |
 |
| pow | Normalization (1050 ph s−1 keV−1) | 4.02 ± 0.06 | 2.93 ± 0.06 | 2.25 ± 0.04 | 3.60 ± 0.06 |
 |
 |
| Photon index Γ | 1.81 ± 0.01 | 1.73 ± 0.02 | 1.66 ± 0.01 | 1.78 ± 0.009 | 1.88 ± 0.01 | 1.86 ± 0.03 | |
| refl | Incident power-law normalization | 4.02 (c) | 2.93 (c) | 2.25 (c) | 3.60 (c) | 4.64 (c) | 4.59 (c) |
| Incident power-law photon index | 1.81 (c) | 1.73 (c) | 1.66 (c) | 1.78 (c) | 1.88 (c) | 1.86 (c) | |
| Reflection scale s | 0.67 ± 0.04 | 0.54 ± 0.07 | 0.30 ± 0.03 | 0.42 ± 0.03 | 0.68 ± 0.011 | 0.57 ± 0.05 | |
| Luminosity | 0.3−2 keV luminosity L0.3 − 2 keV | 1.28 | 0.90 | 0.66 | 1.14 | 1.42 | 1.48 |
| (1042 erg s−1) | 2−10 keV luminosity L2 − 10 keV | 1.45 | 1.20 | 1.00 | 1.32 | 1.50 | 1.54 |
| 1−1000 Ryd ionizing luminosity Lion | 19.1 | 17.8 | 14.6 | 19.8 | 19.2 | 23.5 | |
| Bolometric luminosity Lbol | 43.3 | 47.1 | 42.4 | 46.6 | 47.1 | 52.2 | |
| C-stat/C-expt. | (SED+WAs) | 3439/2794 (S1b)* | 4456/3621* | 3834/3584 | 4105/3588 | 4121/3570 | 3762/3638 (S6c) |
| (Best-fit) | (SED+OCL+WAs) | 3261/2926 (S1a) | 3819/3670 (S6b) | ||||
| (SED+OCH+OCL+WAs) | 3786/3654 (S6a) | ||||||
Notes. The disk blackbody component (dbb) normalization followed by “(s)” is obtained by scaling the dbb normalization of the 2019 observation (see Paper I) to match the OM UVW1 flux of each archival observation. Given that the spectral shape of the emission from the outer disc might not have a strong variability on short timescales, for simplicity, the following parameters are fixed to those of the 2019 observation: the dbb maximum temperature Tmax = 10 eV, the warm Comptonized disk component (comt) seed photon temperature Tseed = 10 eV, the comt electron temperature Te = 60 eV, and the comt optical depth τ = 30. The normalization of the neutral reflection component (refl) denoted by “(c)” is coupled to the normalization of the X-ray power-law component (pow) in the fit, and the photon index (Γ) of the refl denoted by “(c)” is coupled to the photon index of the pow. The 0.3−2 keV luminosity (L0.3 − 2 keV), 2−10 keV luminosity (L2 − 10 keV), 1−1000 Ryd ionizing luminosity (Lion), and bolometric luminosity (Lbol) present the intrinsic luminosities. The C-stat is the C-statistic value of the final fitting result corresponding to the best-fit model and the C-expt. is the expected C-stat. The best-fit model is shown as follows: for Obs1 S1b, Obs2, Obs3, Obs4, Obs5, or Obs6 S6c, it is the intrinsic SED plus the four warm absorbers (WAs), i.e., SED+WAs; for Obs S1a or Obs6 S6b, it is the intrinsic SED plus one low-ionization obscurer component (OCL) plus the four WAs, i.e., SED+OCL+WAs; for Obs6 S6a, it is the intrinsic SED plus one high-ionization obscurer component (OCH) plus OCL plus the four WAs, i.e., SED+OCH+OCL+WAs. The best-fit SED parameters of Obs1 is obtained by fitting the spectra of S1b, and the best-fit SED parameters of Obs6 is obtained by fitting the spectra of S6c. The SED parameters of S1a are fixed to those of S1b; the parameters of both S6a and S6b are fixed to those of S6c. Compared with other observations or slices, Obs1 S1b and Obs2 have relatively worse fitting results that are denoted by “*”, which are mainly due to the uncertainties in the intercalibration between XMM-Newton and NuSTAR.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.