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Table 1:

400 SD low redshift sample.

Cluster
Obs ID z $c_{\rm SB}$ T (keV) $T_{\rm core}$ $L_{\rm X}$ $R_{\rm src}$
(1) (2) (3) (4) (5) (6) (7) (8)
A3395 4944 0.0506 0.081 $\pm$ 0.006 5.13 (5.10) 5.3 1.09 -
A754 577, 6796, 6797 0.0542 0.036 $\pm$ 0.001 9.94 (8.73) 8.3 2.78 no
A3391 4943 0.0551 0.045 $\pm$ 0.002 6.07 (5.39) 7.0 1.05 -
A3667 513, 5751, 5752, 6296, 6292 0.0557 0.029 $\pm$ 0.001 6.72 (6.33) 5.4 3.14 -
A85 904 0.0557 0.167 $\pm$ 0.001 6.90 (6.45) 3.2 2.91 yes
A133 2203, 9897 0.0569 0.259 $\pm$ 0.003 3.71 (4.01) 2.3 0.96 yes
A2256 2419, 965, 1386 0.0581 0.024 $\pm$ 0.001 6.90 (8.37) 6.8 2.66 no
A3158 3201, 3712 0.0583 0.045 $\pm$ 0.001 4.94 (4.67) 5.9 1.72 -
A3266 899 0.0602 0.047 $\pm$ 0.002 8.35 (8.63) 8.0 2.69 -
A1795 5289, 5290, 6159, 6161, 6162, 6163 0.0622 0.180 $\pm$ 0.001 7.80 (6.14) 3.3 3.52 yes
A399 3230 0.0713 0.040 $\pm$ 0.001 5.80 (6.49) 7.1 2.01 no
A2065 3182 0.0723 0.087 $\pm$ 0.002 5.35 (5.44) 4.2 1.82 yes
A401 518, 2309 0.0743 0.040 $\pm$ 0.001 8.07 (7.72) 7.1 3.90 no
A3112 2216, 2516 0.0759 0.273 $\pm$ 0.001 4.28 (5.19) 2.7 2.43 -
A3822 8269 0.0760 0.045 $\pm$ 0.004 5.45 (5.23) 5.6 1.91 -
ZCl1215 4184 0.0767 0.040 $\pm$ 0.002 6.00 (6.54) 6.5 1.80 no
A2029 891, 4977, 6101 0.0779 0.169 $\pm$ 0.003 7.38 (8.22) 4.2 5.72 yes
A1650 5822, 5823, 6356, 6357, 6358, 7242, 7691 0.0823 0.112 $\pm$ 0.001 5.89 (5.29) 5.1 2.33 no
A2597 922, 6934 0.0830 0.332 $\pm$ 0.001 3.58 (3.87) 2.7 2.09 yes
A1651 4185 0.0853 0.082 $\pm$ 0.003 7.00 (6.41) 6.7 2.93 yes
A478 1669 0.0881 0.194 $\pm$ 0.001 7.07 (7.96) 3.1 7.24 yes
A2142 7692, 5005 0.0904 0.082 $\pm$ 0.001 8.24 (10.04) 6.3 7.20 no
A2244 7693 0.0989 0.103 $\pm$ 0.005 5.57 (5.37) 5.4 2.98 no
A2204 6104, 7940 0.1511 0.315 $\pm$ 0.002 6.97 (8.55) 3.5 9.35 yes
A2163 1653 0.2030 0.025 $\pm$ 0.002 12.12 (14.72) 16 13.7 no
RXC J1504.1-0248 5793 0.2169 0.333 $\pm$ 0.003 8.90 (9.89) 4.6 15.6 yes
Hydra* 4969, 4970 0.0549 - 4.30 (3.64) 2.9 1.93 yes
S1101* 1668 0.0564 - 2.65 (2.44) 2.0 1.03 -

Notes. (1) Cluster name; (2) Chandra observation identifier; (3) redshift; (4) surface brightness concentration without K-correction; (5) global temperature from Cavagnolo et al. 2009 (the values in parentheses are from Vikhlinin et al. 2009a); (6) core temperature from Cavagnolo et al. (2009); (7) soft-band luminosity in units 1044 [erg s-1]; and (8) presence of a radio source according to the NVSS archive. (*) Strong cool-core clusters observed only with ACIS-S which we did not consider in our analysis.


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