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Table 1

Best-fit parameters for the continuum for the 20 phases and the phase-averaged spectrum.

Phase nH a kT soft Fsoft b Γ FPO c Count-rate χ2∕dof
[× 1021 cm2] keV 10−11erg cm−2 s−1 10−11erg cm−2 s−1 cts s−1
Average 1.36 0.24 1.44 ± 0.19 0.98 ± 0.10 29.8 ± 0.95 41.8 ± 0.04 1.01/190
0 1.50 0.30 ± 0.03 1.17 ± 0.30 0.92 40.1 ± 0.37 52.5 ± 0.19 1.05/181
1 1.14 0.40 1.70 ± 0.25 0.90 ± 0.04 27.8 ± 0.29 39.9 ± 0.17 0.95/177
2 1.38 0.21 1.66 ± 0.60 1.04 ± 0.03 20.1 ± 0.25 30.6 ± 0.17 1.01/169
3 1.82 0.20 2.02 ± 0.74 1.03 ± 0.02 26.4 ± 0.28 37.8 ± 0.17 1.03/171
4 1.76 0.24 1.41 ± 0.50 1.00 ± 0.02 38.9 ± 0.35 52.7 ± 0.21 1.00/183
5 0.96 – <2.17 1.01 ± 0.01 44.6 ± 0.90 59.9 ± 0.20 0.87/184
6 1.45 0.20 1.28 ± 0.87 1.01 ± 0.02 41.0 ± 0.35 55.3 ± 0.19 1.01/187
7 1.21 0.26 1.25 ± 0.38 1.01 ± 0.02 32.1 ± 0.37 45.6 ± 0.20 0.89/182
8 1.32 0.28 ± 0.03 2.14 ± 0.30 0.95 ± 0.03 27.1 ± 0.34 39.7 ± 0.17 0.81/178
9 1.27 0.23 ± 0.03 2.13 ± 0.48 0.92 ± 0.03 28.6 ± 0.40 40.2 ± 0.17 0.88/178
10 1.66 0.26 ± 0.03 2.48 ± 0.63 0.88 31.5 ± 0.28 42.9 ± 0.18 0.87/182
11 1.84 0.22 ± 0.03 2.21 ± 0.94 0.94 ± 0.04 32.0 ± 0.46 43.8 ± 0.18 1.08/178
12 1.63 0.21 2.24 ± 1.11 0.97 ± 0.03 27.7 ± 0.37 39.5 ± 0.17 1.09/173
13 1.23 0.26 1.83 ± 0.35 1.05 ± 0.03 21.8 ± 0.26 34.1 ± 0.17 0.99/173
14 1.57 0.25 2.04 ± 0.35 1.14 20.0 ± 0.25 32.4 ± 0.15 0.89/170
15 1.31 0.25 1.68 ± 0.38 1.10 20.3 ± 0.25 31.9 ± 0.15 1.07/170
16 1.12 0.27 ± 0.05 0.15 ± 0.31 1.06 20.9 ± 0.26 32.5 ± 0.15 1.01/172
17 1.43 0.24 ± 0.03 1.85 ± 0.39 0.91 ± 0.02 29.0 ± 0.31 39.5 ± 0.17 0.94/187
18 1.79 0.21 1.77 ± 0.82 0.96 ± 0.02 34.9 ± 0.33 46.6 ± 0.18 1.11/178
19 2.26 0.22 2.17 ± 0.61 0.95 ± 0.02 39.8 ± 0.36 51.5 ± 0.19 0.96/182

Notes. All errors are in the 90% confidence range. (a)Column density of the intrinsic absorption. The Galactic foreground absorption was fixed to a value of nH GAL = 7.06 × 1020 cm2 (Dickey & Lockman 1990), with abundances taken from Wilms et al. (2000). (b) Unabsorbed bolometric X-ray flux of the BB in the 0.2–12 keV band. (c)Unabsorbed X-ray flux in the 0.2–12 keV band. For the distance of 62 kpc (Graczyk et al. 2014), a conversion factor of 4.6 × 1047 cm−2 can be used to convert from flux into luminosity.

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