Table 1.
Selection of high X-ray flux and high Hα luminosity galaxy clusters from the BCS sample.
| Cluster | FX | LHα | Ecav | tcav | Pcav | Lcool | tcool |
|---|---|---|---|---|---|---|---|
| [erg cm−2 s−1] | [erg s−1] | [1060 erg] | [Myr] | [1043 erg s−1] | [1043 erg s−1] | [Gyr] | |
| Abell 1068 (1) | 9.4 × 10−12 | 172.3 × 1040 | – | – | 0.36 | 14 | 0.35 ± 0.04 |
| Abell 1835 (2) | 14.7 × 10−12 | 163.9 × 1040 | 1.76 | 40 | 140 | 120 | 0.30 ± 0.04 |
| Abell 2204 (3) | 21.9 × 10−12 | 159.4 × 1040 | 200 | 127 | 5000 | 160 | – |
| Abell 2390 (4) | 9.6 × 10−12 | 61.6 × 1040 | 468 | 250 | 594 | 40.4 | 0.64 ± 0.04 |
| RXJ1720+26 | 14.3 × 10−12 | 12.7 × 1040 | – | – | – | – | 0.53 ± 0.13 |
| Abell 115 | 9.0 × 10−12 | 12.7 × 1040 | – | – | – | – | – |
| ZwCl 8276 | 16.4 × 10−12 | 12.5 × 1040 | – | – | – | – | – |
| Abell 1795 (5) | 68.1 × 10−12 | 11.3 × 1040 | 0.1 | 20 | 16 | 63 | 0.72 ± 0.09 |
| Abell 478 (6) | 39.9 × 10−12 | 10.8 × 1040 | 0.09 | 30 | 10 | 144 | 0.46 ± 0.02 |
| 2A0336+096 (7) | 80.5 × 10−12 | 10.3 × 1040 | 0.04 | 50 | 2.4 | 33.8 | 0.31 ± 0.02 |
| Abell 2009 | 9.2 × 10−12 | 6.1 × 1040 | 0.63 | 20.2 | 112.4 | 43.7 | 1.31 ± 0.09 |
| ZwCl 235 (8) | 10.9 × 10−12 | 4.1 × 1040 | 0.01 | 17 | 1.2 | 10 | 0.75 ± 0.15 |
| Abell 2199 (9) | 96.8 × 10−12 | 2.7 × 1040 | 0.20 | 24 | 27 | 14.2 | – |
| Abell 2052 (10) | 47.1 × 10−12 | 2.6 × 1040 | 0.01 | 15 | 2.4 | 33.8 | 0.61 ± 0.10 |
| Abell 1668 (11) | 9.3 × 10−12 | 2.3 × 1040 | 0.001 | 5.2 | 0.89 | 1.9 | 1.40 ± 0.28 |
| Abell 2495 (12) | 11.8 × 10−12 | 2.0 × 1040 | 0.03 | 17.9 | 4.7 | 5.7 | 1.0 ± 0.2 |
| Abell 2634 | 23.1 × 10−12 | 1.3 × 1040 | – | – | – | – | – |
| Abell 1991 (13) | 9.4 × 10−12 | 1.1 × 1040 | 0.06 | 38.3 | 4.8 | 6.04 | 0.41 ± 0.04 |
Notes. The X-ray fluxes and Hα luminosities are taken from Ebeling et al. (1998) and Crawford et al. (1999), respectively. The references for the other quantities, from forth to seventh column, are: (1) McNamara et al. (2004), (2) McNamara et al. (2006), (3) Sanders et al. (2009), (4) Sonkamble et al. (2015), (5) Russell et al. (2017), (6) Sun et al. (2003), (7) Vantyghem et al. (2016), (8) Ubertosi et al. (2023c), (9) Nulsen et al. (2013), (10) Blanton et al. (2011), (11) Pasini et al. (2021), (12) Rosignoli et al. (2024), (13) Pandge et al. (2013). The reported cavity age, tcav, is the average of the ages of the detected cavities, while the cavity energy and power values, Ecav and Pcav, are the sum of the individual values for each cavity. In some cases, the properties of the identified cavities were not reported (Abell 115 and ZwCl 8276), while in some other cases no cavities were detected in the existing exposures (RXJ1720+26 and Abell 2634). The quantities without a reported uncertainty are associated with a 50% relative uncertainty in the plots of Fig. 9 (see Sect. 4.2 for details). All the values for cooling time, tcool, and their errors are taken from Rafferty et al. (2008), except for Abell 2009 (from this work), ZwCl 235 (from Ubertosi et al. 2023c), Abell 1668 (from Pasini et al. 2021), and Abell 2495 (from Rosignoli et al. 2024).
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