Table 1
Properties of the catalogs after quality filtering.
| Telescope | Catalog | Sky coverage (sq. degrees) | Limiting sensitivity (erg s−1 cm−2) | Spatial resolution (FWHM, arcsec) | Sources | Detections | Dates | Reference |
|---|---|---|---|---|---|---|---|---|
| XMM-Newton | 4XMMDR11 | 560 | ~10−15 | 5 | 470000 | 700 000 | 2000–2020 | Webb et al. (2020) |
| 4XMMDR11s | 560 | ~10−15 | 5 | 34 000+ | 51 000+ | 2000–2020 | Traulsen et al. (2019) | |
| XMMSL2 | 65 000 | ~10−12 | 10 | 22 000 | 27 000 | 2001–2014 | Saxton et al. (2008) | |
| Swift | 2SXPS | 3 790 | ~10−13 | 6 | 145 000 | 300 000 | 2005–2018 | Evans et al. (2020b) |
| Chandra | CSC 2.0 | 550 | ~10−16 | 0.75–5 | 200 000 | 300 000 | 2000–2014 | Evans et al. (2020a) |
| ROSAT | RASS | 41 000 | ~10−12 | 20 | 60 000 | 60 000 | 1990–1991 | Boller et al. (2016) |
| WGACAT | 7500 | ~10−13 | 20 | 70 000 | 80 000 | 1991–1994 | White et al. (1994) | |
| eROSITA | eFEDS | 140 | ~10−14 | 5 | 20 000 | 20 000 | Nov. 2019 | Salvato et al. (2022) |
Notes. The limiting sensitivities are typical flux values in the corresponding instrument’s energy band (see Fig. 3), but numerous instrumental effects (off-axis angle, background, exposure time) will impact this value. For Chandra, the two values for spatial resolution correspond to the on-axis and 10## off-axis FWHM. For the XMM-Newton Stacked catalog, we only show the number of new sources and number of new detections (which might be associated with already known sources).
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