Table 1.
Values adopted for our mock X-ray observations with Athena, eROSITA, and XMM-Newton.
| Instrument | Energy band | Bbg | fabs | Aeff |
|---|---|---|---|---|
| (keV) |
 |
(cm2) | ||
| Athena-WFI | 0.3–0.8 | 2.1 × 104 | 0.83 | 9511 |
| 0.8–1.2 | 3.1 × 103 | 0.95 | 12 139 | |
| 1.2–2.0 | 1.4 × 103 | 0.98 | 10 841 | |
| 2.0–5.0 | 3.4 × 103 | 0.99 | 4673 | |
| 5.0–7.0 | 2.0 × 103 | 1.00 | 2131 | |
| eROSITA | 0.3–0.8 | 2.2 × 103 | 0.83 | 610 |
| 0.8–1.2 | 4.6 × 102 | 0.95 | 1243 | |
| 1.2–2.0 | 4.2 × 102 | 0.98 | 1267 | |
| 2.0–5.0 | 4.1 × 102 | 0.99 | 287 | |
| 5.0–7.0 | 3.0 × 102 | 1.00 | 88 | |
| XMM | 0.3–0.8 | 4.6 × 103 | 0.83 | 1056 |
| (PN + 2MOS) | 0.8–1.2 | 1.4 × 103 | 0.95 | 1655 |
| 1.2–2.0 | 1.8 × 103 | 0.98 | 1894 | |
| 2.0–5.0 | 3.4 × 103 | 0.99 | 1337 | |
| 5.0–7.0 | 1.7 × 103 | 1.00 | 998 | |
Notes. For each different energy band we give the count rate due to the effective (sky+instrumental) background, the fraction fabs of source counts unabsorbed by the galactic column density (assuming nH = 2 × 1020 cm−2), and the mean effective collecting area Aeff in that energy range. For eROSITA, we quote values extrapolated from http://www.mpe.mpg.de/1303215/eROSITA_background_v12.pdf (Boller, priv. comm.); for XMM-Newton, we quote an average value on a set of observations obtained under different conditions (of orbits, solar cycle, time; Ghirardini, priv. comm.).
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