Table 2.
Observation details and results of the XSPEC and BEHR analysis.
| Source | Obs. ID | Net exposure [ks] | Flux | log(LX, Observed) | log(LX, Predicted) | ||
|---|---|---|---|---|---|---|---|
| pn | MOS1 | MOS2 | [10−16 erg s cm−2] | [erg s−1] | [erg s−1] | ||
| BB1 | 0865260101 | 14.7 | 21.8 | 21.8 | 63 ± 9 | 40.5 ± 0.3 | 41.0 |
| BB2 | 0865260201 | 38.0 | 53.8 | 53.8 | < 8.1 | < 39.3 | 40.4 |
| BB3 | 0865260301 | 16.6 | 23.3 | 23.3 | < 9.5 | < 40.2 | 41.0 |
| BB4 | 0865260401 | 24.7 | 30.8 | 30.7 | < 2.1 | < 39.7 | 41.0 |
| BB5 | 0865260501 | 5.1 | 9.9 | 8.9 | < 1.5 | < 39.9 | 40.4 |
| BB7 | 0865260701 | 23.5 | 43.9 | 43.9 | < 4.5 | < 39.5 | 40.2 |
| BB8 | 0865260801 | 50.7 | 59.7 | 59.7 | 68 ± 8 | 40.4 ± 0.2 | 39.9 |
Notes. Rest frame fluxes and luminosities (or their upper limits) in the 0.5–8 keV band along with the predicted luminosity values calculated using the Brorby et al. (2016) scaling relation. For the two detected sources, the fluxes were determined with the use of the XSPEC software. For the rest, the upper limits on fluxes were measured using the BEHR code and the WebPIMMS flux estimate.
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