Table B.1.
Results from the optical spectral fitting of the SPM spectra.
| Spectrum | Flux Hα | FWHM Hα | Flux Hβ | AGN-Luminosity | logMBH | |
|---|---|---|---|---|---|---|
| (10−14 erg cm−2 s−1) | (km s−1) | (10−14 erg cm−2 s−1) | (1043 erg s−1) | (M⊙) | ||
| (5100Å) | (3500Å) | |||||
| SPM-2022 | 3.49 ± 0.13 | 3525.00 ± 0.01 | 1.05 ± 0.03 | 1.31 ± 0.01 | 1.47 ± 0.01 | 7.61 ± 0.50 |
| SPM-2023 | 4.04 ± 0.14 | 3290.00 ± 99.19 | 1.01 ± 0.04 | 1.51 ± 0.06 | 2.133 ± 0.002 | 7.57 ± 0.51 |
Notes. Flux and FWHM columns are for broad emission lines. In the luminosity columns we compare the AGN continuum between the two spectra at two different wavelengths. For the calculation of the luminosity we used a ΛCDM cosmological model with H0 = 70 km/s/Mpc. The black hole masses are derived from the virial mass estimator using Hα. We added uncertainties of 0.5 dex to the error of the masses, as expected for virial mass estimates (Reines & Volonteri 2015).
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