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Home All issues Volume 507 / No 2 (November IV 2009) A&A, 507 2 (2009) 661-669 Full HTML
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Table 1:

Radio and X-ray properties of clusters used in this paper.
Cluster's z $L_{\rm X}$ $L_{\rm bol}$ P1.4 Ref.
name   [1044 erg/s ] [1044 erg/s ] [1024 Watt/Hz]  
1E50657-558 0.2994 $23.03\pm 1.81$ $87.10\pm 6.82$ $28.21\pm 1.97$ 1, 7
A2163 0.2030 $23.17\pm 1.48$ $86.50\pm 5.52$ $18.44\pm 0.24$ 1, 8
A2744 0.3080 $12.92\pm 2.41$ $36.81\pm 6.88$ $17.16\pm 1.71$ 1, 9
A2219 0.2280 $12.73\pm 1.37$ $38.55\pm 4.05$ $12.23\pm 0.59$ 2, 10
CL0016+16 0.5545 $18.83\pm 1.88$ $55.59\pm 5.56$   $\:6.74\pm 0.67$ 4, 11
A1914 0.1712 $10.71\pm 1.02$ $34.51\pm 3.28$   $\:5.21\pm 0.24$ 3, 10
A665 0.1816   $\:9.84\pm 1.54$ $27.61\pm 4.32$   $\:3.98\pm 0.39$ 2, 11
A520 0.2010   $\:8.83\pm 1.99$ $23.77\pm 5.34$   $\:3.91\pm 0.39$ 2, 10
A521 0.2475   $\:8.18\pm 1.36$ $19.63\pm 3.26$   $\:1.16\pm 0.11$ 1, 12
A2254 0.1780   $\:4.32\pm 0.92$ $11.35\pm 2.43$   $\:2.94\pm 0.29$ 3, 10
A2256 0.0581   $\:3.81\pm 0.17$   $\:9.54\pm 0.43$   $\:0.68\pm 0.12$ 3, 13, 14
A773 0.2170   $\:8.10\pm 1.35$ $22.70\pm 3.78$   $\:1.73\pm 0.17$ 2, 9
A545 0.1530   $\:5.66\pm 0.49$ $12.50\pm 1.09$   $\:1.48\pm 0.06$ 1, 10
A2319 0.0559   $\:7.40\pm 0.40$ $21.42\pm 1.16$   $\:1.12\pm 0.11$ 3, 15
A1300 0.3071 $13.96\pm 2.05$ $41.97\pm 6.17$   $\:6.09\pm 0.61$ 1, 15
A1656 (Coma) 0.0231   $\:3.77\pm 0.10$ $10.44\pm 0.28$   $\:0.72^{+0.07}_{-0.04}$ 3, 16, 17
A2255 0.0808   $\:2.65\pm 0.12$   $\:6.61\pm 0.30$   $\:0.89\pm 0.05$ 3, 18
A754 0.0535   $\:4.31\pm 0.33$ $12.94\pm 0.99$   $\:1.08\pm 0.06$ 3, 10
A209 0.2060   $\:6.29\pm 0.65$ $16.26\pm1.69$   $\:1.19\pm 0.26$ 1, 19*
RXJ2003 0.3171   $\:9.25\pm 1.53$ $27.23\pm4.95$ $12.30\pm 0.71$ 1, 20
MACS J0717 0.5548 $24.6\pm 0.3$ $84.18\pm1.01$ $50.0\pm 10.0$ 5, 21, 22
A2390 0.228 $13.49\pm 3.16$     $\:9.77 \pm 0.45$ 2, 10
Z7160 0.258   $\:8.51\pm 2.12$     $\:2.19 \pm 0.26$ 2, 23
RXJ1314 0.2439 $10.96 \pm 1.81$     $\:0.75 \pm 0.15$ 1, 19*, 24*
A2697 0.2320   $\:6.88 \pm 0.85$   <0.40 1, 25
A141 0.2300   $\:5.76 \pm 0.90$   <0.36 1, 25
A3088 0.2537   $\:6.95 \pm 1.20$   <0.42 1, 25
RXJ1115.8 0.3499 $13.58\pm 2.99$   <0.45 1, 25
S780 0.2357 $15.53\pm 2.80$   <0.36 1, 25
RXJ1512.2 0.3152 $10.19\pm 1.76$   <0.63 1, 25
A2537 0.2966 $10.17\pm 1.45$   <0.50 1, 25
A2631 0.2779   $\:7.57 \pm 1.50$   <0.39 1, 25
A2667 0.2264 $13.65\pm 1.38$   <0.42 1, 25
RXJ0027.6 0.3649 $12.29\pm 3.88$   <0.68 6, 25
A611 0.2880   $\:8.86 \pm 2.53$   <0.40 6, 25
A781 0.2984 $11.29\pm 2.82$   <0.36 2, 25
Z2089 0.2347   $\:6.79 \pm 1.76$   <0.27 2, 25
Z2701 0.2140   $\:6.59 \pm 1.15$   <0.42 2, 25
A1423 0.2130   $\:6.19 \pm 1.34$   <0.41 2, 25
Z5699 0.3063   $\:8.96 \pm 2.24$   <0.54 6, 25
Z5768 0.2660   $\:7.47 \pm 1.66$   <0.36 6, 25
Z7215 0.2897   $\:7.34 \pm 1.91$   <0.55 6, 25
RXJ1532.9 0.3450 $16.49\pm 4.50$   <0.62 2, 25
RXJ2228.6 0.4177 $19.44\pm 5.55$   <0.91 6, 25

Giant radio halos (first sector), mini-halos in cool core clusters (second sector), small scale halos (tirdth sector), clusters with no Mpc-scale radio emission (last sector). GMRT clusters are reported in bold. In Col. (1): Cluster name. Column (2): Cluster redshift. Column (3): X-ray luminosity in the energy range [0.1-2.4] keV in unit of h70-2 1044 erg/s. Column (4): Bolometric X-ray luminosity in the energy range [0.01-40] keV in unit of h70-2 1044 erg/s. Column (5): Radio power at 1.4 GHz in unit of h70-2  1024 Watt/Hz. Column (6) References: 1 = Boehringer et al. (2004), 2 = Ebeling et al. (1998), 3 = Ebeling et al. (1996), 4 = Tsuru et al. (1996), 5 = Ebeling et al. (2007), 6 = Ebeling et al. (2000), 7 = Liang et al. (2000), 8 = Feretti et al. (2001), 9 = Govoni et al. (2001), 10 = Bacchi et al. (2003), 11 = Giovannini & Feretti (2000), 12 = Dallacasa et al. (2009), 13 = Clarke & Ensslin (2006), 14 = Brentjens (2008), 15 = Feretti (2002), 16 = Kim et al. (1990), 17 = Deiss et al. (1997), 18 = Govoni et al. (2005), 19 = Venturi et al. (2007), 20 = Giacintucci et al. (2009), 21 = van Weeren et al. (2009), 22 = Bonafede et al. (2009), 23 = Cassano et al. (2008b), 24 = Giacintucci (2007) (integrating the diffuse radio emission between the two radio relics). (*) P1.4 of A209 and RXJ1314 is estimated from that at 610 MHz by adopting $\alpha =1.2$.

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