Table 2.
Calibration of the count rate to halo mass relation parameters for eROSITA using different weak-lensing data sets and cluster samples.
| WL survey | AX | BX | FX | GX | σX |
|---|---|---|---|---|---|
| KiDS-1000 (eRASS1) | 1.63 ± 0.42 | 1.70 ± 0.28 | 1.73 ± 1.74 | −2.33 ± 1.56 | < 1.01 |
| DES Y3 (eRASS1) | 0.88 ± 0.20 | 1.62 ± 0.14 | −0.85 ± 0.93 | −0.32 ± 0.69 | 0.61 ± 0.19 |
| HSC-Y3 (eRASS1) | 0.77 ± 0.32 | 1.65 ± 0.34 | 1.20 ± 1.66 | −1.24 ± 1.60 | 0.72 ± 0.25 |
| HSC-Y3 (eFEDS) | 1.24 ± 0.21 | 1.58 ± 0.16 | 1.00 ± 1.20 | −0.44 ± 0.83 | – |
Notes. The constraints on the parameters of the count rate to halo mass relation for eROSITA selected clusters are derived from different WL surveys (KiDS, DES, HSC) and different eROSITA surveys (eRASS1, eFEDS). All of these analyses are statistically consistent with each other.
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