Table 1.
Our selected clusters observed by LOFAR.
| Cluster name | RA, Dec | Redshift | Scale | Mass | Dynamics | Halo P1.4 corr | RH corr | re |
|---|---|---|---|---|---|---|---|---|
| (Obs ID) | J2000 | z | kpc arcsec−1 | (1014 M⊙) | w500 kpc, c100 kpc | log10 (W Hz−1) | (kpc) | (kpc) |
| Abell 1314 | 11h34m50.5s, | 0.0335 | 0.672 | 0.68a | 0.063 ± 0.003, | N/A | N/A | N/A |
| (L229509) | +49d03m28s | Low | 0.026 ± 0.01 | |||||
| Abell 1319 | 11h34m13.2s, | 0.2906 | 4.395 |
 |
0.013, | 23.80 | 351 | 135 |
| (L403936) | +40d02m36s | Intermediate | 0.148b | |||||
| RXC J1501.3+4220 | 15h01m23.0s, | 0.2917 | 4.406 |
 |
0.096 ± 0.06, | 24.13 | 422 | 162 |
| – Z7215 – | +42d20m40s | Intermediate | 0.052 ± 0.09 | |||||
| (L371804) |
Notes. The mass listed for Abell 1319 and Z7215 are SZ mass-estimates from Planck (Planck Collaboration XXIX 2014). The last three columns give the characteristics of a radio halo falling on the P − M correlation from Cassano et al. (2013) for a cluster corresponding to that mass. We use these correlation values to compare to the diffuse emission detected by LOFAR.
Our mass-estimate from XMM-Newton observations and scaling relations from Reichert et al. (2011). Since this cluster is at such a low mass, the P − M correlation is not applicable.
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