Table A.1.
Spectral fit results for eRO-QPE3.
| Epoch | Spectrum | Model | kTdisk |
 |
 |
kTQPE |
 |
ΔlogZ |
|---|---|---|---|---|---|---|---|---|
| [eV] | [erg s−1 cm−2] | [erg s−1 cm−2] | [eV] | [erg s−1 cm−2] | ||||
| eRASS1 | Quiescence | disk |
 |
(1.4 ± 0.2)×10−12 | – | – | – | 2 |
| disk+pl |
 |
 |
 |
– | – | 0 | ||
| QPE | disk+pl+bb | 100 | 1.4 × 10−12 | 2.9 × 10−13 |
 |
(3.0 ± 0.7)×10−12 | – | |
| Full | disk+pl |
 |
 |
 |
– | – | – | |
| eRASS2 | Quiescence | disk |
 |
 |
– | – | – | 1.5 |
| disk+pl (free) |
 |
< 4.2 × 10−13 |
 |
– | – | 0.5 | ||
| disk+pl |
 |
 |
 |
– | – | 0 | ||
| QPE | disk+pl+bb | 89 | 3.1 × 10−13 | 2.4 × 10−13 |
 |
 |
– | |
| eRASS3 | Quiescence | disk | – | < 2.7 × 10−14 | – | – | – | – |
| QPE | bb | – | – | – |
 |
 |
– | |
| eRASS4 | Quiescence | disk | – | < 3.5 × 10−13 | – | – | – | – |
| QPE | bb | – | – | – |
 |
 |
– | |
| eRASS5 | Quiescence | disk | – | < 7.2 × 10−15 | – | – | – | – |
| QPE | bb | – | – | – |
 |
 |
– | |
| XMM1 burst1 | Quiescence | disk | – | < 1.2 × 10−14 | – | – | – | – |
| QPE rise1 | bb | – | – | – |
 |
 |
– | |
| QPE rise2 | bb | – | – | – | (121 ± 6) |
 |
– | |
| QPE peak | bb | – | – | – |
 |
 |
– | |
| QPE decay1 | bb | – | – | – |
 |
 |
– | |
| QPE decay2 | bb | – | – | – | (86 ± 7) |
 |
– | |
Fit values show the median and related 16th-84th percentiles of the fit posteriors. We mark in boldface the adopted best-fit model, if more than one is reported, which has the highest Bayesian evidence. The difference between the logarithmic Bayesian evidence values is shown in the last column for these cases. For eRASS2, the disk+pl(free) model has no constraint on the power-law normalization, whilst in the disk+pl model the power-law is tied to that of the disk with the same ratio observed in the eRASS1 spectrum. During the QPE fit, the quiescence model is held fixed, if detected. For eRASS5, the QPE fit is compatible with background within 3σ and the fit parameters should be interpreted with caution. For XMM-Newton, the different phases are shown in Fig. 10 and A.9. Given the spectroscopic redshift and the cosmology adopted (Hinshaw et al. 2013), the conversion for related luminosity values for eRO-QPE3 is 1.34 × 1054 cm2 in this paper.
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