Table 2.
Main characteristics of the galaxy clusters employed in this study.
| Cluster name | Redshift | M200 [M⊙] | R200 [Mpc] | ⟨Z/Z⊙⟩ |
|---|---|---|---|---|
| Hercules Supercluster | 0.033 | 2.1 × 1015(1) | N/A | N/A |
| RX J2248–443 | 0.348 | 2.81 × 1015 (2) | 2.6 (3) | 0.26 (4) |
| Cl0024 (this work) | 0.395 | 5.85 × 1014 (5) | 1.73 (5) | 0.22 (6) |
| MACS J0416.1–2403 | 0.397 | 1 × 1015 (7) | 1.8 (7) | 0.24 (8) |
| Cl 0939+4713 | 0.41 | 1.7 × 1015 (3) | 2.13 (3) | 0.2 (9) |
| XMMXCS J2215.9–1738 | 1.5 | 6.3 × 1014 (10) | 1.23 (10) | N/A |
| XMM–LSS J02182–05102 | 1.62 | 7.7 × 1013 (11) | 0.49 (11) | N/A |
| PKS 1138–262 | 2.16 | 1.71 × 1014 (12) | 0.53 (12) | N/A |
Notes. First column is the cluster name, second column is the redshift of the cluster, third column is the M200 in solar masses, fourth column is the R200 in Mpc, and fith column is the mean value of the iron abundance in the intracluster gas in units of solar metallicity.
References. (1) Monteiro-Oliveira et al. (2022); (2) Kesebonye et al. (2023); (3) Koyama et al. (2011); (4) De Filippis et al. (2003); (5) Sánchez-Portal et al. (2015); (6) Zhang et al. (2005); (7) Bonamigo et al. (2018); (8) Bonamigo et al. (2017); (9) Rahaman et al. (2021); (10) Maier et al. (2019); (11) Pierre et al. (2012); (12) Shimakawa et al. (2014).
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