| Row . | Parameter . | LF . | HF . | J21 . | F23 . |
|---|---|---|---|---|---|
| (1) | |$N_{\mathrm{H,Gal}}$| | 2.77|$\times 10^{20}$| | 2.77|$\times 10^{20}$| | 2.77|$\times 10^{20}$| | 2.77|$\times 10^{20}$| |
| (2) | Z | 1 | 1 | 1 | 1 |
| (3) | |$A_{\mathrm{Fe}}$| | 6.9|$_{-3.3}^{+9.0}$| | 6.9 | 6.9 | 6.9 |
| (4) | z | 0.026385 | 0.026385 | 0.026385 | 0.026385 |
| agnsed | |||||
| (5) | |$M_{\mathrm{BH}}$| | |$3.7\times 10^7$| | |$3.7\times 10^7$| | |$3.7\times 10^7$| | |$3.7\times 10^7$| |
| (6) | D | 112 | 112 | 112 | 112 |
| (7) | |$\log (\dot{m})$| | –2.05|$\pm 0.06$| | –1.57|$\pm 0.01$| | –1.72|$\pm 0.02$| | –1.99|$\pm 0.04$| |
| (8) | |$a_{*}$| | 0 | 0 | 0 | 0 |
| (9) | |$\cos (i)$| | 0.788 | 0.788 | 0.788 | 0.788 |
| (10) | |$kT_{\mathrm{hot}}$| | 300 | 300 | 300 | 300 |
| (11) | |$kT_{\mathrm{warm}}$| | 0.25|$\pm 0.02$| | 0.25|$\pm 0.03$| | 0.30|$\pm 0.03$| | 0.26|$\pm 0.03$| |
| (12) | |$\Gamma _{\mathrm{hot}}$| | 1.65|$\pm 0.06$| | 1.73|$\pm 0.03$| | 1.70|$\pm 0.03$| | 1.68|$\pm 0.09$| |
| (13) | |$\Gamma _{\mathrm{warm}}$| | 2.23|$\pm 0.32$| | 2.29|$\pm 0.39$| | 2.45|$\pm 0.16$| | 2.38|$\pm 0.30$| |
| (14) | |$R_{\mathrm{hot}}$| | 168|$\pm 35$| | 124|$\pm 47$| | 104|$\pm 8$| | 127|$\pm 24$| |
| (15) | |$R_{\mathrm{warm}}$| | |$4.7(\pm 2.8)\times 10^4$| | |$5.7(\pm 2.6)\times 10^4$| | |$4.3(\pm 2.9)\times 10^4$| | |$6.0(\pm 2.8)\times 10^4$| |
| (16) | |$\log R_{\mathrm{out}}$| | |$\equiv R_{\mathrm{warm}}$| | |$\equiv R_{\mathrm{warm}}$| | |$\equiv R_{\mathrm{warm}}$| | |$\equiv R_{\mathrm{warm}}$| |
| (17) | |$h_{\mathrm{max}}$| | 10 | 10 | 10 | 10 |
| pexmon | |||||
| (18) | N|$_{\mathrm{cont}}$| | |$3.4(\pm 1.0)\times 10^{-4}$| | 4.2|$(\pm 4.0)\times 10^{-4}$| | |$(5.5\pm 1.1)\times 10^{-4}$| | |$(3.8_{-3.8}^{+8.2})\times 10^{-4}$| |
| Instrumental | |||||
| (19) | |$C_{\mathrm{MOS1}}$| | 1.03|$\pm 0.01$| | 1.05|$\pm 0.01$| | 0.99|$\pm 0.01$| | 1.01|$\pm 0.01$| |
| (20) | |$C_{\mathrm{MOS2}}$| | 1.04|$\pm 0.01$| | 1.03|$\pm 0.01$| | 0.99|$\pm 0.01$| | 1.03|$\pm 0.01$| |
| (21) | |$C_{\mathrm{FPMA}}$| | 0.89|$\pm 0.04$| | 1.18|$\pm 0.06$| | 0.84|$\pm 0.01$| | 1.14|$\pm 0.01$| |
| (22) | |$C_{\mathrm{FPMB}}$| | 0.90|$\pm 0.03$| | 1.20|$\pm 0.03$| | 0.87|$\pm 0.01$| | 1.17|$\pm 0.01$| |
| (23) | |$C_{\mathrm{UVOT}}$| | 1 | 1 | 1 | 1 |
| Row . | Parameter . | LF . | HF . | J21 . | F23 . |
|---|---|---|---|---|---|
| (1) | |$N_{\mathrm{H,Gal}}$| | 2.77|$\times 10^{20}$| | 2.77|$\times 10^{20}$| | 2.77|$\times 10^{20}$| | 2.77|$\times 10^{20}$| |
| (2) | Z | 1 | 1 | 1 | 1 |
| (3) | |$A_{\mathrm{Fe}}$| | 6.9|$_{-3.3}^{+9.0}$| | 6.9 | 6.9 | 6.9 |
| (4) | z | 0.026385 | 0.026385 | 0.026385 | 0.026385 |
| agnsed | |||||
| (5) | |$M_{\mathrm{BH}}$| | |$3.7\times 10^7$| | |$3.7\times 10^7$| | |$3.7\times 10^7$| | |$3.7\times 10^7$| |
| (6) | D | 112 | 112 | 112 | 112 |
| (7) | |$\log (\dot{m})$| | –2.05|$\pm 0.06$| | –1.57|$\pm 0.01$| | –1.72|$\pm 0.02$| | –1.99|$\pm 0.04$| |
| (8) | |$a_{*}$| | 0 | 0 | 0 | 0 |
| (9) | |$\cos (i)$| | 0.788 | 0.788 | 0.788 | 0.788 |
| (10) | |$kT_{\mathrm{hot}}$| | 300 | 300 | 300 | 300 |
| (11) | |$kT_{\mathrm{warm}}$| | 0.25|$\pm 0.02$| | 0.25|$\pm 0.03$| | 0.30|$\pm 0.03$| | 0.26|$\pm 0.03$| |
| (12) | |$\Gamma _{\mathrm{hot}}$| | 1.65|$\pm 0.06$| | 1.73|$\pm 0.03$| | 1.70|$\pm 0.03$| | 1.68|$\pm 0.09$| |
| (13) | |$\Gamma _{\mathrm{warm}}$| | 2.23|$\pm 0.32$| | 2.29|$\pm 0.39$| | 2.45|$\pm 0.16$| | 2.38|$\pm 0.30$| |
| (14) | |$R_{\mathrm{hot}}$| | 168|$\pm 35$| | 124|$\pm 47$| | 104|$\pm 8$| | 127|$\pm 24$| |
| (15) | |$R_{\mathrm{warm}}$| | |$4.7(\pm 2.8)\times 10^4$| | |$5.7(\pm 2.6)\times 10^4$| | |$4.3(\pm 2.9)\times 10^4$| | |$6.0(\pm 2.8)\times 10^4$| |
| (16) | |$\log R_{\mathrm{out}}$| | |$\equiv R_{\mathrm{warm}}$| | |$\equiv R_{\mathrm{warm}}$| | |$\equiv R_{\mathrm{warm}}$| | |$\equiv R_{\mathrm{warm}}$| |
| (17) | |$h_{\mathrm{max}}$| | 10 | 10 | 10 | 10 |
| pexmon | |||||
| (18) | N|$_{\mathrm{cont}}$| | |$3.4(\pm 1.0)\times 10^{-4}$| | 4.2|$(\pm 4.0)\times 10^{-4}$| | |$(5.5\pm 1.1)\times 10^{-4}$| | |$(3.8_{-3.8}^{+8.2})\times 10^{-4}$| |
| Instrumental | |||||
| (19) | |$C_{\mathrm{MOS1}}$| | 1.03|$\pm 0.01$| | 1.05|$\pm 0.01$| | 0.99|$\pm 0.01$| | 1.01|$\pm 0.01$| |
| (20) | |$C_{\mathrm{MOS2}}$| | 1.04|$\pm 0.01$| | 1.03|$\pm 0.01$| | 0.99|$\pm 0.01$| | 1.03|$\pm 0.01$| |
| (21) | |$C_{\mathrm{FPMA}}$| | 0.89|$\pm 0.04$| | 1.18|$\pm 0.06$| | 0.84|$\pm 0.01$| | 1.14|$\pm 0.01$| |
| (22) | |$C_{\mathrm{FPMB}}$| | 0.90|$\pm 0.03$| | 1.20|$\pm 0.03$| | 0.87|$\pm 0.01$| | 1.17|$\pm 0.01$| |
| (23) | |$C_{\mathrm{UVOT}}$| | 1 | 1 | 1 | 1 |
Note. Best-fitting parameters for our optical–UV–X-ray model based on agnsed (Section 4.2), for the low-flux (LF) and high-flux (HF) data sets. The uncertainties correspond to 1|$\sigma$| intervals derived from the Markov chain Monte Carlo posterior distributions. Parameters listed in grey are held constant during the model fit procedure. (1) Column density for Galactic absorption, units of cm|${^{-2}}$|. (2) Metallicity relative to Solar. (3) Iron abundance relative to Solar. (4) Source redshift. (5) Black hole mass in units of Solar mass, as estimated via reverberation mapping (Peterson et al. 2004). (6) Co-moving distance in Mpc; as the redshift is small (|$z=0.026385$|) we set this to the luminosity distance. (7) Mass accretion rate, scaled by the Eddington accretion rate. (8) Black hole rotation parameter. (9) Inclination angle; here, we constrain the agnsed and pexmon inclinations to the best-fitting value from our X-ray analysis. (10) Electron temperature in the hot Comptonizing region, units of keV. (11) Electron temperature in the warm Comptonizing region. (12) Photon index for hot Comptonized emission. (13) Photon index for warm Comptonized emission. (14) Radius of the hot Comptonization region, in units of the gravitational radius |$r_g$|. (15) Radius of the warm Comptonization region. (16) Outer radius; for this model we do not include an outer disc, so it is equal to |$R_{\mathrm{warm}}$|. (19) Height above the disc of the ‘lamp-post’ X-ray source that irradiates the disc. We set this to 10 |$r_g$|, as for the disc reflection model in our X-ray analysis. (18) Incident continuum normalization for the distant reflection component. For the optical–UV–X-ray modelling, as we are mainly interested in the overall spectral energy distribution, we set the pexmon reflection strength to |$R=-1$| and use |$N_{\mathrm{cont}}$| to scale the reflection spectrum. (19–23) Instrumental scaling factors relative to XMM–Newton pn. We set |$C_{\mathrm{UVOT}}\equiv 1$|, as we are testing whether the overall UV flux level can be reproduced by the soft excess model; allowing for UV to X-ray flux offsets would defeat this purpose. Instead, our use of averaged UVOT photometry should minimize the influence of luminosity variability.
| Row . | Parameter . | LF . | HF . | J21 . | F23 . |
|---|---|---|---|---|---|
| (1) | |$N_{\mathrm{H,Gal}}$| | 2.77|$\times 10^{20}$| | 2.77|$\times 10^{20}$| | 2.77|$\times 10^{20}$| | 2.77|$\times 10^{20}$| |
| (2) | Z | 1 | 1 | 1 | 1 |
| (3) | |$A_{\mathrm{Fe}}$| | 6.9|$_{-3.3}^{+9.0}$| | 6.9 | 6.9 | 6.9 |
| (4) | z | 0.026385 | 0.026385 | 0.026385 | 0.026385 |
| agnsed | |||||
| (5) | |$M_{\mathrm{BH}}$| | |$3.7\times 10^7$| | |$3.7\times 10^7$| | |$3.7\times 10^7$| | |$3.7\times 10^7$| |
| (6) | D | 112 | 112 | 112 | 112 |
| (7) | |$\log (\dot{m})$| | –2.05|$\pm 0.06$| | –1.57|$\pm 0.01$| | –1.72|$\pm 0.02$| | –1.99|$\pm 0.04$| |
| (8) | |$a_{*}$| | 0 | 0 | 0 | 0 |
| (9) | |$\cos (i)$| | 0.788 | 0.788 | 0.788 | 0.788 |
| (10) | |$kT_{\mathrm{hot}}$| | 300 | 300 | 300 | 300 |
| (11) | |$kT_{\mathrm{warm}}$| | 0.25|$\pm 0.02$| | 0.25|$\pm 0.03$| | 0.30|$\pm 0.03$| | 0.26|$\pm 0.03$| |
| (12) | |$\Gamma _{\mathrm{hot}}$| | 1.65|$\pm 0.06$| | 1.73|$\pm 0.03$| | 1.70|$\pm 0.03$| | 1.68|$\pm 0.09$| |
| (13) | |$\Gamma _{\mathrm{warm}}$| | 2.23|$\pm 0.32$| | 2.29|$\pm 0.39$| | 2.45|$\pm 0.16$| | 2.38|$\pm 0.30$| |
| (14) | |$R_{\mathrm{hot}}$| | 168|$\pm 35$| | 124|$\pm 47$| | 104|$\pm 8$| | 127|$\pm 24$| |
| (15) | |$R_{\mathrm{warm}}$| | |$4.7(\pm 2.8)\times 10^4$| | |$5.7(\pm 2.6)\times 10^4$| | |$4.3(\pm 2.9)\times 10^4$| | |$6.0(\pm 2.8)\times 10^4$| |
| (16) | |$\log R_{\mathrm{out}}$| | |$\equiv R_{\mathrm{warm}}$| | |$\equiv R_{\mathrm{warm}}$| | |$\equiv R_{\mathrm{warm}}$| | |$\equiv R_{\mathrm{warm}}$| |
| (17) | |$h_{\mathrm{max}}$| | 10 | 10 | 10 | 10 |
| pexmon | |||||
| (18) | N|$_{\mathrm{cont}}$| | |$3.4(\pm 1.0)\times 10^{-4}$| | 4.2|$(\pm 4.0)\times 10^{-4}$| | |$(5.5\pm 1.1)\times 10^{-4}$| | |$(3.8_{-3.8}^{+8.2})\times 10^{-4}$| |
| Instrumental | |||||
| (19) | |$C_{\mathrm{MOS1}}$| | 1.03|$\pm 0.01$| | 1.05|$\pm 0.01$| | 0.99|$\pm 0.01$| | 1.01|$\pm 0.01$| |
| (20) | |$C_{\mathrm{MOS2}}$| | 1.04|$\pm 0.01$| | 1.03|$\pm 0.01$| | 0.99|$\pm 0.01$| | 1.03|$\pm 0.01$| |
| (21) | |$C_{\mathrm{FPMA}}$| | 0.89|$\pm 0.04$| | 1.18|$\pm 0.06$| | 0.84|$\pm 0.01$| | 1.14|$\pm 0.01$| |
| (22) | |$C_{\mathrm{FPMB}}$| | 0.90|$\pm 0.03$| | 1.20|$\pm 0.03$| | 0.87|$\pm 0.01$| | 1.17|$\pm 0.01$| |
| (23) | |$C_{\mathrm{UVOT}}$| | 1 | 1 | 1 | 1 |
| Row . | Parameter . | LF . | HF . | J21 . | F23 . |
|---|---|---|---|---|---|
| (1) | |$N_{\mathrm{H,Gal}}$| | 2.77|$\times 10^{20}$| | 2.77|$\times 10^{20}$| | 2.77|$\times 10^{20}$| | 2.77|$\times 10^{20}$| |
| (2) | Z | 1 | 1 | 1 | 1 |
| (3) | |$A_{\mathrm{Fe}}$| | 6.9|$_{-3.3}^{+9.0}$| | 6.9 | 6.9 | 6.9 |
| (4) | z | 0.026385 | 0.026385 | 0.026385 | 0.026385 |
| agnsed | |||||
| (5) | |$M_{\mathrm{BH}}$| | |$3.7\times 10^7$| | |$3.7\times 10^7$| | |$3.7\times 10^7$| | |$3.7\times 10^7$| |
| (6) | D | 112 | 112 | 112 | 112 |
| (7) | |$\log (\dot{m})$| | –2.05|$\pm 0.06$| | –1.57|$\pm 0.01$| | –1.72|$\pm 0.02$| | –1.99|$\pm 0.04$| |
| (8) | |$a_{*}$| | 0 | 0 | 0 | 0 |
| (9) | |$\cos (i)$| | 0.788 | 0.788 | 0.788 | 0.788 |
| (10) | |$kT_{\mathrm{hot}}$| | 300 | 300 | 300 | 300 |
| (11) | |$kT_{\mathrm{warm}}$| | 0.25|$\pm 0.02$| | 0.25|$\pm 0.03$| | 0.30|$\pm 0.03$| | 0.26|$\pm 0.03$| |
| (12) | |$\Gamma _{\mathrm{hot}}$| | 1.65|$\pm 0.06$| | 1.73|$\pm 0.03$| | 1.70|$\pm 0.03$| | 1.68|$\pm 0.09$| |
| (13) | |$\Gamma _{\mathrm{warm}}$| | 2.23|$\pm 0.32$| | 2.29|$\pm 0.39$| | 2.45|$\pm 0.16$| | 2.38|$\pm 0.30$| |
| (14) | |$R_{\mathrm{hot}}$| | 168|$\pm 35$| | 124|$\pm 47$| | 104|$\pm 8$| | 127|$\pm 24$| |
| (15) | |$R_{\mathrm{warm}}$| | |$4.7(\pm 2.8)\times 10^4$| | |$5.7(\pm 2.6)\times 10^4$| | |$4.3(\pm 2.9)\times 10^4$| | |$6.0(\pm 2.8)\times 10^4$| |
| (16) | |$\log R_{\mathrm{out}}$| | |$\equiv R_{\mathrm{warm}}$| | |$\equiv R_{\mathrm{warm}}$| | |$\equiv R_{\mathrm{warm}}$| | |$\equiv R_{\mathrm{warm}}$| |
| (17) | |$h_{\mathrm{max}}$| | 10 | 10 | 10 | 10 |
| pexmon | |||||
| (18) | N|$_{\mathrm{cont}}$| | |$3.4(\pm 1.0)\times 10^{-4}$| | 4.2|$(\pm 4.0)\times 10^{-4}$| | |$(5.5\pm 1.1)\times 10^{-4}$| | |$(3.8_{-3.8}^{+8.2})\times 10^{-4}$| |
| Instrumental | |||||
| (19) | |$C_{\mathrm{MOS1}}$| | 1.03|$\pm 0.01$| | 1.05|$\pm 0.01$| | 0.99|$\pm 0.01$| | 1.01|$\pm 0.01$| |
| (20) | |$C_{\mathrm{MOS2}}$| | 1.04|$\pm 0.01$| | 1.03|$\pm 0.01$| | 0.99|$\pm 0.01$| | 1.03|$\pm 0.01$| |
| (21) | |$C_{\mathrm{FPMA}}$| | 0.89|$\pm 0.04$| | 1.18|$\pm 0.06$| | 0.84|$\pm 0.01$| | 1.14|$\pm 0.01$| |
| (22) | |$C_{\mathrm{FPMB}}$| | 0.90|$\pm 0.03$| | 1.20|$\pm 0.03$| | 0.87|$\pm 0.01$| | 1.17|$\pm 0.01$| |
| (23) | |$C_{\mathrm{UVOT}}$| | 1 | 1 | 1 | 1 |
Note. Best-fitting parameters for our optical–UV–X-ray model based on agnsed (Section 4.2), for the low-flux (LF) and high-flux (HF) data sets. The uncertainties correspond to 1|$\sigma$| intervals derived from the Markov chain Monte Carlo posterior distributions. Parameters listed in grey are held constant during the model fit procedure. (1) Column density for Galactic absorption, units of cm|${^{-2}}$|. (2) Metallicity relative to Solar. (3) Iron abundance relative to Solar. (4) Source redshift. (5) Black hole mass in units of Solar mass, as estimated via reverberation mapping (Peterson et al. 2004). (6) Co-moving distance in Mpc; as the redshift is small (|$z=0.026385$|) we set this to the luminosity distance. (7) Mass accretion rate, scaled by the Eddington accretion rate. (8) Black hole rotation parameter. (9) Inclination angle; here, we constrain the agnsed and pexmon inclinations to the best-fitting value from our X-ray analysis. (10) Electron temperature in the hot Comptonizing region, units of keV. (11) Electron temperature in the warm Comptonizing region. (12) Photon index for hot Comptonized emission. (13) Photon index for warm Comptonized emission. (14) Radius of the hot Comptonization region, in units of the gravitational radius |$r_g$|. (15) Radius of the warm Comptonization region. (16) Outer radius; for this model we do not include an outer disc, so it is equal to |$R_{\mathrm{warm}}$|. (19) Height above the disc of the ‘lamp-post’ X-ray source that irradiates the disc. We set this to 10 |$r_g$|, as for the disc reflection model in our X-ray analysis. (18) Incident continuum normalization for the distant reflection component. For the optical–UV–X-ray modelling, as we are mainly interested in the overall spectral energy distribution, we set the pexmon reflection strength to |$R=-1$| and use |$N_{\mathrm{cont}}$| to scale the reflection spectrum. (19–23) Instrumental scaling factors relative to XMM–Newton pn. We set |$C_{\mathrm{UVOT}}\equiv 1$|, as we are testing whether the overall UV flux level can be reproduced by the soft excess model; allowing for UV to X-ray flux offsets would defeat this purpose. Instead, our use of averaged UVOT photometry should minimize the influence of luminosity variability.
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