Table 2.
Spectral fit results of eRASSU J060839.5−704014 from BXA.
| Obs | kTbb | Norm |
 |
 |
log Z | d.o.f. | Cstat./d.o.f. | Fobserved(a) | L(b) | RBB |
|---|---|---|---|---|---|---|---|---|---|---|
| – | (eV) | brems | (1021 cm−2) | (1021 cm−2) | – | – | – | (erg cm−2 s−1) | (erg s−1) | (km) |
| eRO |
 |
– | 0.88 | < 0.5 | −293.3 | 249 | 1.5 |
 |
1.4 × 1035 | 70.1 |
| EPIC | 109.5 ± 1.4 | 1.9 ± 1.0 | 0.88 | < 0.6 | −418.2 | 353 | 1.2 |
 |
1.7 × 1035 | 96.8 |
| On | 109.4 ± 1.5 | 1.4 ± 1.0 | 0.88 | < 0.6 | −366.9 | 353 | 0.9 |
 |
5.6 × 1035 | 153.4 |
| Off | 110.2 ± 1.5 | 2.8 ± 1.0 | 0.88 | < 0.8 | −417.6 | 353 | 1.1 |
 |
1.4 × 1035 | 75.2 |
| eRO |
 |
– | 0.47 |
– | −283.5 | 249 | 1.3 |
 |
5.9 × 1031 | 1.03 |
| EPIC | 113.8 ± 2.7 | 2.1 ± 1.0 | 0.74 |
– | −418.7 | 353 | 1.1 |
 |
7.3 × 1031 | 2.0 |
| On | 112.8 ± 3.3 | 1.5 ± 1.0 | 0.77 |
– | −368.8 | 353 | 0.9 |
 |
2.1 × 1032 | 2.0 |
| Off | 116.1 ± 4.1 | 3.4 ± 1.0 | 0.68 |
– | −418.5 | 353 | 1.0 |
 |
5.8 × 1031 | 0.5 ± 0.3 |
Notes. The first set of the table corresponds to the fit parameter “in the LMC” interpretation (two column densities) and the second set (lower in the table) corresponds to the “foreground” interpretation. Best-fit parameters using a model with absorbed black-body and bremsstrahlung emission (in the case of XMM-Newton). The normalisation of the bremsstrahlung component is in units of 10−3. The bremsstrahlung component is not well constrained, and the temperature was fixed at 10 keV (see Sect. 3.3). The log Z indicates the goodness of the fit. Errors indicate 1σ percentile values. Corresponding Cstat./d.o.f. values are also quoted to get an independent estimate of the fit quality. Errors indicate 1σ percentile values.
Fluxes are provided for the 0.2−2.0 keV band in units of 10−13 to allow a comparison with values published for SSSs based on ROSAT observations.
Source luminosities (0.2−2.0 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 was 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. Norm denotes the normalisation of the bremsstrahlung component.
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