Table 3.
Spectral fit results.
| Source | Observation | kTbb |
 |
 |
C-stat | d.o.f. | Fobserved(c) | L(d) | RBB |
|---|---|---|---|---|---|---|---|---|---|
| name (a) | ID | (eV) | (1021 cm−2) | (1021 cm−2) | /d.o.f. | (erg cm−2 s−1) | (erg s−1) | (km) | |
| J0504 | 0803460101 | 31 ± 4 | 0.64 | 1.2 |
0.66 | 19 | 7.6 ± 0.4 × 10−14 | 1.7 × 1037 | 16 000 |
| J0518 | 0690751801 | 78 ± 8 | 0.67 | 0.9 |
1.2 | 94 | 1.0 ± 0.1 × 10−13 | 2.1 × 1035 | 220 |
| eROSITA | 88 ± 4 | 0.67 | 0.09 |
1.1 | 106 | 1.7 ± 0.2 × 10−13 | 2.0 × 1035 | 135 |
|
| J0508 (b) | 0690752001 | 86 ± 9 | 0.74 | 1.9  |
1.7 | 54 | 1.7 ± 0.1 × 10−13 | 5.7 × 1035 | 290  |
| J0446 | 0801990301 | 49 ± 14 | 0.72 | 6.4 |
0.94 | 40 | 2.0 ± 0.3 × 10−14 | 7 × 1036 | 3400 |
| J0518 | 0690751801 | 78 ± 7 | 1.6 |
– | 1.2 | 94 | 1.0 × 10−13 | 9.0 × 1031 | 4.5  |
| eROSITA | 88 ± 4 | 0.75 |
– | 1.1 | 106 | 1.7 × 10−13 | 6.0 × 1031 | 2.7  |
|
| J0508 (b) | 0690752001 | 87 ± 9 | 2.5 |
– | 1.7 | 54 | 1.7 × 10−13 | 2.4 × 1032 | 6.1 |
| J0446 | 0801990301 | 50 ± 14 | 7.1 |
– | 0.96 | 40 | 2.0 × 10−14 | 5.0 × 1033 | 87 |
Notes. Best-fit parameters using a model with absorbed blackbody and bremsstrahlung emission. The bremsstrahlung component is not well constrained, and the temperature was fixed at 10 keV (see Sect. 2.1). The C-stat values include the full model. Errors indicate 90% confidence ranges.
For full source names, see Table 1.
Fluxes are provided for the 0.1–2.4 keV band to allow comparison with values published for SSSs based on ROSAT observations.
Source luminosities (0.1–2.4 keV) corrected for absorption, assuming a distance of 50 kpc (Pietrzyński et al. 2013) in the upper part of the table. The Galactic foreground column density was taken from Dickey & Lockman (1990). For the model in the lower part of the table, only a Galactic absorption component (with free column density in the fit) and a distance of 1 kpc were assumed. A note of caution regarding absorption-corrected X-ray luminosities in soft energy bands: Column densities with large errors lead to a large uncertainty on the luminosity, which is in particular the case for J0446.
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