Table 6
Summary of performance characteristics of the eROSITA telescope and its survey sensitivity.
| Energy range | |||
|---|---|---|---|
| Soft band | Hard band | ||
| 0.2–2.3 keV | 2.3–8 keV | ||
| FoV averaged effective area [cm2] | 1,365 at 1keV | 139 at 5 keV | |
| Total background [10−3 cts s−1 arcmin−2] | ≈3.7 | ≈2.1 | |
| Point source sensitivity eRASS:1 | |||
| Ecliptic equatorial region | Total exposure [s] = 200 | 5 × 10−14 erg s−1 cm−2 | 7 × 10−13 erg s−1 cm−2 |
| Ecliptic polar region | Total exposure [s] = 4000 | 7 × 10−15 erg s−1 cm−2 | 9 × 10−14 erg s−1 cm−2 |
| Point source sensitivity eFEDS | |||
| eFEDS field | Total exposure [s] = 2500 | 9 × 10−15 erg s−1 cm−2 | 1.3 × 10−13 erg s−1 cm−2 |
| Point source sensitivity eRASS:8 (predicted) | |||
| Ecliptic equatorial region | Total/Effective exposure [s] = 1600 | 1.1 × 10−14 erg s−1 cm−2 | 2.5 × 10−13 erg s−1 cm−2 |
| Ecliptic polar region | Total exposure [s] = 30 000 | 2.5 × 10−15 erg s−1 cm−2 | 4 × 10−14 erg s−1 cm−2 |
Notes. The background counts are based on the first all-sky survey data. For eRASS:1 and the PV eFEDS 140 deg2 survey (Brunner et al. 2021), the flux sensitivity in each band has been computed by taking all sources detected above a likelihood of8 (soft band) or 10 (hard band), and measuring the flux below which the logarithmic number counts start declining. For eRASS:8 the predictions are based on detailed simulations that include all instrumental effects and particle background intensity consistent with that measured at L2. For each field or region, we quote the total (unvignetted) exposure in seconds. The corresponding effective (vignetted) exposures can be computed by dividing the total exposure by 1.8 and 3.31 for the soft and hard band, respectively.
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