Table 3
Fits with a multi-coloured disc model to XMM-Newton pointed observations of XMMSL1 J0740-85.
| optxagnf a | Disc lineb | zxipcfc | C/d.o.f. | |||||||
|
|
||||||||||
| ṁ | slope | kT | τ e | f pl | E line | Norm | N H | xi | cf | |
| log(ṁedd) | (eV) | (keV) | × 10-6 | 1022 cm-2 | log | % | ||||
|
|
||||||||||
| XMM-Newton observation 1 − 2014-04-30 (XMM1) | ||||||||||
|
|
||||||||||
|
1.87 ± 0.07 |
|
|
|
404/395 | |||||
|
2.06 ± 0.10 |
|
|
|
|
|
382/393 | |||
|
1.84 ± 0.09 |
|
|
|
|
|
> 63 | 383/392 | ||
|
|
||||||||||
| XMM-Newton observation 2 − 2015-01-12 (XMM2) | ||||||||||
|
|
||||||||||
|
2.30 ± 0.12 | 114 ± 20 |
|
|
117/105 | |||||
|
2.37 ± 0.13 |
|
|
|
|
|
116/103 | |||
|
|
|
|
|
|
<6 | <1 | 117/102 | ||
Notes. All fits include absorption by the Galactic column (model TBABS, NH = 1.5 × 1021 cm-2). Errors are 90% confidence.
Shown are parameters of the optxagnf model (Done et al. 2012) with black hole mass fixed to MBH = 3.5 × 106M⊙ and spin to a = 0; accretion rate, power-law slope, electron temperature of the soft Comptonisation component, optical depth, the disc radius, within which emission changes from black-body to a Comptonised spectrum, and the fraction of energy emitted as a power-law;
observed energy of a relativistically broadened line given by the (Laor model; Laor 1991);
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