Table B.1.
Estimated biases in fluxes measured from the 2′ circles from simulations.
| Nobj | FX, S | FX, B | Mean | Mode (no PCN) | Mode (with PCN) | |
|---|---|---|---|---|---|---|
| 1 | 1 × 10−11 | 1 × 10−11 | ∼10−17 ∼ 0 | −1.1 × 10−14 | −8.5 × 10−15 | Fig.B.1 (left) |
| 1 | 1 × 10−11 | 2 × 10−14 | +6.5 × 10−15 | −6.5 × 10−15 | −3.5 × 10−15 | |
| 1 | 1 × 10−13 | 2 × 10−14 | +3.5 × 10−15 | −6.5 × 10−15 | −3.5 × 10−15 | Fig.B.1 (right) |
| 1 | 4 × 10−14 | 2 × 10−14 | +1.8 × 10−15 | −6.5 × 10−15 | −3.5 × 10−15 | |
| 36 | 1 × 10−11 | 1 × 10−11 | ∼10−17 ∼ 0 | −2.5 × 10−15 | −2.5 × 10−15 | |
| 36 | 1 × 10−11 | 2 × 10−14 | +6.4 × 10−15 | +3.5 × 10−15 | +3.5 × 10−15 | |
| 36 | 1 × 10−13 | 2 × 10−14 | +3.5 × 10−15 | +2.5 × 10−15 | +3.5 × 10−15 | Fig.B.2 |
| 36 | 4 × 10−14 | 2 × 10−14 | +1.8 × 10−15 | +1.5 × 10−15 | +1.5 × 10−15 | |
| 1 | 1 × 10−11 | 1 × 10−13 | 2.8 × 10−15 | −9.5 × 10−15 | −6.5 × 10−15 | Fig.B.3 |
| 364 | 1 × 10−11 | 1 × 10−13 | 2.8 × 10−15 | 1.5 × 10−15 | 1.5 × 10−15 | Fig.B.3 |
Notes. All fluxes are in units of erg s−1 cm−2 in the 0.5-2 keV band. The bias in the mean flux (column ‘Mean’) is caused by the different resolved fractions of CXB in the source and background regions, specified by the flux cuts FX, S and FX, B, respectively. Another bias affects the mode of the measured flux distribution (columns ‘Mode (no PCN)’ and ‘Mode (with PCN)’). are caused by the fluctuations of the number of sources below the flux cut with and without account for a typical level of Photon Counting Noise (PCN) in eROSITA all-sky data. The rows of the Table marked with Nobj = 1 correspond to the biases in the distribution of fluxes for a single measurement, while those marked as Nobj = 36 characterize the mean flux in the sample of 36 objects. The last two rows correspond to the extended sample that features 364 objects, but sources with FX > 10−13 erg s−1 cm−2 are removed only from the ‘background region. In all cases, the distribution is calculated in flux bins of 10−15 erg s−1 cm−2 and, therefore, the mode has comparable uncertainty.
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