Spectral fits with the reflection model.
|Data||Total||0–60 ks||60–118 ks|
|Continuum||Γ||2.05 ± 0.04||2.00 ± 0.03||2.05 ± 0.03|
|NH,C||1.3 ± 0.1||1.3||1.3|
|Reflection||log ξR||3.0 ± 0.2||2.9 ± 0.2||3.1 ± 0.2|
|R||0.57 ± 0.08||0.44 ± 0.09||0.56 ± 0.13|
|Blurring||i||42 ± 4||42||42|
|β||2||0.1 (<1.9)||1.5 (<2.4)|
Notes. The spectral data obtained for the whole duration (total), first (0–60 ks) and second (60–118 ks) halves of the observation were fitted by the reflection model. All the three spectra are of 200-eV intervals in the 2.3–11 keV band. The fitted model is a power-law supplemented by reflection from an ionized disc including relativistic blurring, computed by relxill (García et al. 2014). Cold and ionized blueshifted absorption are also included. The NH of cold absorption was fitted for the total spectrum and fixed for the other two. The best-fit parameters of the ionized absorption are comparable among the three (see Table 1). The ionization parameter of the reflecting medium is ξR. R is the reflection fraction with respect to that from 2π solid angle. In modelling relativistic blurring, i is the inclination angle in degree, a is the dimensionless parameter of the black hole spin, and β is the slope of radial emissivity law (∝r− β). The inner disc radius is automatically set by the spin parameter a, while the outer radius is assumed to be 1000rg. For the 0–60 ks and 60–118 ks spectra, the emissivity law is assumed to have a break at 100rg and the inner β is fitted, while the outer β is fixed at 2. (†) The black hole spin a is unconstrained. The permitted range includes negative values (for a retrograde disc) down to −0.998.
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