Table D.2.
Parameter constraints for the joint fit of the spectra at all the epochs.
| Model | Parameter | X1 | X2 | X3 | S1 | C1 |
|---|---|---|---|---|---|---|
| constant | CMOS | 0.9 ± 0.1 | 0.93 ± 0.05 | 1.03 ± 0.05 | - | - |
| CXRT or CACIS | - | - | - | [1] | [1] | |
| TBabs | NH (1020 cm−2) | [2.6] | ||||
| slimdz | ṁ (ṁEdd) |
 |
=X1 | =X1 |
 |
0.10 ± 0.03 |
| θ (°) | 76 ± 3 | 71 ± 3 | 73 ± 3 | < 65 | =S1 | |
| M• (M⊙) | (5 ± 1)×104 | |||||
| a• | > 0.97 | |||||
| C-stat/d.o.f. | 119.0/123 | |||||
Notes. Same as Table D.1, but here we find that the X–ray spectra of J1231 at X1, X2, and X3 epochs can also be well explained by a slim disc model varying only the inclination θ. Although the marginal constraints of θ at X1, X2, and X3 overlaps, for any given set of {ṁ, M•, a•}, they do not overlap. During the fit, we assume at S1 and C1, decades after the first detection, any possible disc precession is terminated, and so the disc inclination is not varying. Based on the calculation of Ce and its RMS, both fits (Table D.1 and this table) should be considered good descriptions of the data.
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