Table 1.
Observed fraction of clusters with radio haloes.
| z = 0.07 − 0.2 | z = 0.2 − 0.3 | z = 0.3 − 0.5 | ||||
|---|---|---|---|---|---|---|
| fRH(obs) | fRH(MC) | fRH(obs) | fRH(MC) | fRH(obs) | fRH(MC) | |
| U = no RH | ||||||
| High-mass | 0.37 | 0.40 ± 0.04 | 0.36 | 0.34 ± 0.03 | 0.60 | 0.52 ± 0.05 |
| Low-mass | 0.07 | 0.05 ± 0.03 | 0.11 | 0.13 ± 0.02 | 0.25 | 0.28 ± 0.05 |
| U = RH | ||||||
| High-mass | 0.59 | 0.60 ± 0.05 | 0.56 | 0.52 ± 0.05 | 0.71 | 0.62 ± 0.05 |
| Low-mass | 0.24 | 0.24 ± 0.04 | 0.26 | 0.29 ± 0.04 | 0.35 | 0.43 ± 0.05 |
Notes. From left to right, the diving mass between the low-mass and high-mass sub-samples is in each redshift bin M500 = 3.71 × 1014 M⊙, 4.81 × 1014 M⊙, and 5.68 × 1014 M⊙ (in the U = no RH cases); M500 = 3.71 × 1014 M⊙, 4.81 × 1014 M⊙, and 5.54 × 1014 M⊙ (in the U = RH cases). The main uncertainty for fRH(obs) is driven by the RH classification (upper vs. lower panel).
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