Table 2
Spectral parameters of the best-fit thermal models to EPIC data of HM1.
| XID | N H | k T 1 | nor m 1 | k T 2 | nor m 2 | k T 3 | nor m 3 | χ2/d.o.f. (d.o.f.) |
|
|
log (LBOL) |
|
| 1022 cm-2 | keV | 10-3 cm-5 | keV | 10-3 cm-5 | keV | 10-3 cm-5 | 10-13 erg cm-2 s-1 | 1032 erg s-1 | (L⊙) | |||
|
|
||||||||||||
| 1 | 1.1 + (0.066 ± 0.007) | 0.140 ± 0.009 | 51 ± 29 | 0.57 ± 0.03 | 0.97 ± 0.10 | 1.99 ± 0.08 | 0.44 ± 0.03 | 1.41 (414) | 15.5 | 154.7 ± 1.2 | 6.32 | −5.713 ± 0.003 |
| 2 | 0.26 ± 0.13 | 0.20 ± 0.05 | 0.06 ± 0.17 | 0.95 ± 0.04 | 0.05 ± 0.02 | 2.74 ± 0.35 | 0.108 ± 0.009 | 1.15 (136) | 2.11 | |||
| 3 | 0.32 ± 0.06 | 0.03 ± 0.02 | 37543 ± 74131 | 0.32 ± 0.02 | 0.29 ± 0.07 | 1.79 (77) | 1.54 | |||||
| 4 | 1.1 + (0.51 ± 0.07) | 0.90 ± 0.06 | 0.24 ± 0.03 | 1.15 (56) | 0.59 | 2.78 ± 0.10 | 6.23 | −7.37 ± 0.02 | ||||
| 5 | 1.1 + (0.53 ± 0.12) | 0.62 ± 0.14 | 0.35 ± 0.11 | 1.24 (34) | 0.47 | 3.00 ± 0.13 | 6.13 | −7.24 ± 0.02 | ||||
| 6 | 1.1 + (0.10 ± 0.10) | 1.98 ± 0.54 | 0.065 ± 0.012 | 1.67 (29) | 0.68 | 1.58 ± 0.09 | 6.22 | −7.61 ± 0.02 | ||||
| 7 | 1.1 + (0.40 ± 0.08) | 0.93 ± 0.07 | 0.18 ± 0.02 | 1.12 (43) | 0.49 | 2.53 ± 0.14 | 5.82 | −7.00 ± 0.02 | ||||
| 8 | 1.1 + (1.41 ± 1.05) | >7.0 | 0.44 ± 0.06 | 0.69 (21) | 5.37 | |||||||
| 9 | 1.1 + (0. ± 0.16) | 2.58 ± 0.46 | 0.064 ± 0.005 | 0.93 (17) | 0.49 | |||||||
Notes. The fitted model has the form wabs × wabs × ∑ apec, where the first, interstellar absorption was fixed to 1.1 × 1022 cm-2 for all but the known foreground sources (XID 2 and 3). Fluxes refer to the 0.5−10. keV energy band, luminosities were corrected for the interstellar absorption only, and abundances of the thermal emission component and additional absorption are solar (Anders & Grevesse 1989), except for the two WRs (XID 1 and 6, see text). For massive stars, approximate errors on X-ray luminosities and log [LX/LBOL] , shown on Fig. 4, were calculated using the relative errors on the total count rates (Tables 1 − this agrees well with results of the “flux err” command and “cflux” model within xspec for both observed fluxed and absorption-corrected ones) − other uncertainties in the absolute calibration, the spectral models, and the extinction or bolometric luminosities of the individual stars are not included in these errors.
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