Table 3.
Best fitting spectral parameters for the broadband (E = 0.3 − 10 keV) X-ray spectra of each sample source, measured by assuming a model consisting of a power-law plus a blackbody component, modified by Galactic absorption.
| Obj. ID | Γ | kTbb | (C-stat/d.o.f.) (d.o.f.) | F0.5 − 2 keV | F2 − 10 keV | L0.5 − 2 keV | L2 − 10 keV | kbol, X | RS/P |
|---|---|---|---|---|---|---|---|---|---|
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
| J0300–08 | 1.9 (fixed) | 140 ± 30 | 1.22 (60) |
 |
 |
 |
 |
5100 ± 2500 | 1.24 |
| J0809+46 (a) | 2.10 ± 0.06 | – | 1.16 (169) |
 |
 |
 |
 |
150 ± 70 | – |
| J0820+23 | 2.26 ± 0.09 | 80 ± 20 | 1.08 (173) |
 |
 |
 |
 |
150 ± 70 | 0.28 |
| J0940+46 | 2.3 ± 0.1 | 134 ± 4 | 0.90 (205) |
 |
 |
 |
 |
200 ± 90 | 2.59 |
| J1048+31 (b) | 1.27 ± 0.08 | 120 ± 20 | 0.81 (210) |
 |
 |
 |
 |
140 ± 70 | 0.55 |
| J1103+41 | 1.6 ± 0.1 | 122 ± 6 | 0.84 (196) |
 |
 |
 |
 |
600 ± 300 | 2.42 |
| J1127+11 | 2.3 ± 0.1 | 170 ± 20 | 0.91 (192) |
 |
 |
 |
 |
100 ± 50 | 0.52 |
| J1127+64 | 1.5 ± 0.4 | 110 ± 20 | 0.77 (53) |
 |
 |
 |
 |
 |
4.37 |
| J1206+41 | 1.4 ± 0.2 | 128 ± 7 | 0.70 (97) |
 |
 |
 |
 |
300 ± 100 | 5.52 |
| J1207+15 | 2.0 ± 0.1 |
 |
0.97 (224) |
 |
 |
 |
 |
100 ± 50 | 0.45 |
| J1218+10 | 2.5 ± 0.2 | 160 ± 10 | 0.98 (162) |
 |
 |
 |
 |
200 ± 100 | 0.97 |
| J1245+33 | 1.3 (fixed) | 120 ± 20 | 0.96 (44) |
 |
 |
 |
 |
2000 ± 1000 | 2.93 |
| J1301+59 | 2.01 ± 0.05 | 122 ± 3 | 0.98 (295) |
 |
 |
 |
 |
140 ± 60 | 1.25 |
| J1336+17 | 1.86 ± 0.04 |
 |
1.01 (336) |
 |
 |
 |
 |
50 ± 20 | 0.10 |
Notes. (1) Abbreviated object ID; (2) photon index of the power-law continuum component; (3) rest-frame temperature of the blackbody component (eV); (4) ratio between the C-stat value of the spectral fit and the degrees of freedom; (5) flux in the E = 0.5 − 2 keV band (erg cm−2 s−1); (6) flux in the E = 2 − 10 keV band (erg cm−2 s−1); (7) luminosity in the E = 0.5 − 2 keV band (erg s−1); (8) luminosity in the E = 2 − 10 keV band (erg s−1); (9) X-ray bolometric correction; (10) value of the RS/P parameter.
The best-fit model of J0809+46 is a power law modified by a warm absorber component (see Sect. 3.1 and Fig. A.1) and it does not require a blackbody component.
The best-fit model of J1048+31 also includes a Gaussian emission line component, see Fig. A.1.
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