Table A.1.
Best fitting parameters for fits to the 0.4–1 keV light curves from all observations with QPEs.
| Trec | C | N | σ | χ2/dof | |
|---|---|---|---|---|---|
| [ s ] | [ cts s−1 ] | [ cts s−1 ] | [ s ] | ||
| XMM3 | 414/246 | ||||
| QPE(w) | 29757 ± 34 | 0.046 ± 0.001 | 0.96 ± 0.04 | 810 ± 25 | |
| QPE(s) | − | 1.37 ± 0.04 | 809 ± 18 | ||
| XMM4 | 875/644 | ||||
| QPE(s) | 33089 ± 40 | 0.0451 ± 0.0009 | 1.24 ± 0.04 | 818 ± 25 | |
| QPE(w) | 31266 ± 37 | − | 0.87 ± 0.03 | 817 ± 23 | |
| QPE(s) | 32592 ± 35 | − | 1.10 ± 0.04 | 805 ± 19 | |
| QPE(w) | 31656 ± 35 | − | 0.93 ± 0.04 | 800 ± 22 | |
| QPE(s) | − | 1.22 ± 0.04 | 808 ± 18 | ||
| Chandra | 14/61 | ||||
| QPE(s) | 33551 ± 191 | 0.069 ± 0.01 | 1.59 ± 0.23 | 828 ± 91 | |
| QPE(w) | 31865 ± 211 | − | 0.81 ± 0.17 | 757 ± 119 | |
| QPE(s) | − | 1.06 ± 0.19 | 708 ± 99 | ||
| XMM5 | 867/636 | ||||
| QPE(w) | 30081 ± 42 | 0.0242 ± 0.0006 | 0.56 ± 0.03 | 743 ± 29 | |
| QPE(s) | 33458 ± 38 | − | 0.93 ± 0.04 | 810 ± 22 | |
| QPE(w) | 31182 ± 38 | − | 0.72 ± 0.03 | 759 ± 22 | |
| QPE(s) | 33373 ± 41 | − | 0.89 ± 0.03 | 831 ± 21 | |
| QPE(w) | − | 0.76 ± 0.03 | 854 ± 30 | ||
| XMM6 | 745/634 | ||||
| QPE(s) | 26428 ± 88 | 0.070 ± 0.001 | 0.28 ± 0.02 | 611 ± 40 | |
| QPE(w) | 28794 ± 88 | − | 0.22 ± 0.02 | 749 ± 52 | |
| QPE(s) | 35700 ± 76 | − | 0.41 ± 0.03 | 851 ± 51 | |
| QPE(w) | − | 0.31 ± 0.02 | 744 ± 50 | ||
Notes. We use time bins of 200 s and 500 s for XMM-Newton and Chandra observations respectively. Our model consists of an observation-dependent constant C representing the quiescent count rate and a series of Gaussian functions with normalisation N and width σ describing the QPEs. Superscripts in the first column denote strong (s) and weak (w) QPEs respectively. The separation between a QPE and the next is denoted by Trec. The Chandra light curve has been re-scaled to match the XMM-Newton EPIC-pn detector effective area prior to fitting (see text for details). Errors represent the 1-σ confidence intervals.
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