Table 4
Upper limits on the count rates and fluxes of the sources that were not detected.
| # | Name | Exp. rate | Obs. rate | Ratio |
|
FX,abs | FX,unabs | LX |
| (10-3 c s-1) | (1022 cm-2) | (10-12 erg cm-2 s-1) | (1033 erg s-1) | |||||
|
|
||||||||
| 1 | AX J1457.5–5901 | 8.34 | <2.47 | >3.38 | 1.7 | <0.2 | <0.4 | <3 |
| 3 | AX J1510.0–5823 | 5.60 | <2.78 | >2.00 | 1.7 | <0.2 | <0.4 | <3 |
| 4 | AX J1537.8–5556 | 6.40 | <2.11 | >3.04 | 1.9 | <0.2 | <0.3 | <2 |
| 6 | AX J1545.9–5443 | 2.91 | <2.19 | >1.33 | 1.7 | <0.2 | <0.3 | <2 |
| 9 | AX J1657.3–4321 | 2.66 | <2.73 | >0.97 | 1.6 | <0.2 | <0.4 | <3 |
| 10 | AX J1659.8–4209 | 3.30 | <4.72 | >0.70 | 1.6 | <0.3 | <0.7 | <5 |
| 15 | AX J1734.5–2915 | 7.76 | <2.44 | >3.18 | 0.6 | <0.1 | <0.2 | <2 |
| 20 | AX J1751.1–2748 | 27.5 | <3.90 | >7.04 | 1.2 | <0.3 | <0.5 | <4 |
| 21 | AX J1753.5–2745 | 4.34 | <3.06 | >1.42 | 1.0 | <0.2 | <0.3 | <2 |
| 23 | AX J1758.0–2812 | 4.21 | <5.10 | >0.83 | 0.5 | <0.3 | <0.4 | <3 |
| 24 | AX J1832.5–0916 | 2.58 | <3.65 | >0.71 | 1.6 | <0.3 | <0.5 | <4 |
| 25 | AX J1833.9–0822 | 18.7 | <3.31 | >5.66 | 1.7 | <0.2 | <0.5 | <4 |
| 26 | AX J1834.6–0801 | 2.49 | <2.26 | >1.10 | 1.8 | <0.2 | <0.3 | <2 |
| 27 | AX J1835.1–0806 | 3.02 | <2.22 | >1.36 | 1.8 | <0.2 | <0.3 | <2 |
| 28 | AX J1836.3–0647 | 27.6 | <2.82 | >9.80 | 1.6 | <0.2 | <0.4 | <3 |
| 31 | AX J1847.6–0219 | 5.21 | <1.95 | >2.67 | 1.8 | <0.1 | <0.3 | <2 |
| 33 | AX J1856.8+0245 | 1.91 | <1.36 | >1.40 | 1.5 | <0.1 | <0.2 | <2 |
| 34 | AX J1857.3+0247 | 2.29 | <1.28 | >1.79 | 1.5 | <0.1 | <0.2 | <2 |
| 35 | AX J1900.1+0427 | 2.80 | <2.17 | >1.29 | 1.7 | <0.1 | <0.3 | <2 |
Notes. All quoted count rates, fluxes and luminosities are given in the 0.3–10 keV energy range. We list both the expected (exp.) and observed (obs.) XRT count rates (see text), as well as the ratio of the two (expected/observed). The listed 3σ count rate upper limits were translated into fluxes using pimms by assuming a fiducial absorbed powerlaw model with a spectral index of Γ = 1.9 and a hydrogen column density corresponding to the listed Galactic values from Kalberla et al. (2005). The luminosities were calculated from the unabsorbed flux by adopting a distance of 8 kpc for all sources.
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