Table D.3.
Parameter constraints from fitting the time–resolved spectra at X2 and X3 with the slimdz model.
| Model | Parameter | X2–p | X2–v | X3–p | X3–v |
|---|---|---|---|---|---|
| constant | CMOS | 0.94 ± 0.07 | 0.8 ± 0.1 | 0.97 ± 0.08 | 1.1 ± 0.1 |
| TBabs | NH (1020 cm−2) | [2.6] | [2.6] | ||
| slimdz | ṁ (ṁEdd) | 1.74 ± 0.08 | 0.64 ± 0.03 | 1.05 ± 0.04 | 0.55 ± 0.02 |
| θ (°) | [10] | [10] | |||
| M• (M⊙) | [5.7 × 104] | [5.7 × 104] | |||
| a• | [0.99] | [0.99] | |||
| C-stat/d.o.f. | 74.9/64 | 74.7/64 | |||
Notes. The total fit function is "constant*TBabs*slimdz". Values held fixed during the fit are given in square brackets. Assuming the best–fit black hole parameters (M•, a•, and θ) derived from Table D.1, we test the disc explanation of the quasi–periodic variation observed at X2 and X3. At each epoch of X2 and X3, we jointly fit the average spectrum of the peaks (X2–p or X3–p) and that of the valleys (X2–v or X3–v). Here Ce ≈ 68 with an RMS of ≈12 for each epoch. We find the difference between the source spectra at peaks and valleys can be explained by a varying ṁ.
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.