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Table 3:

Properties of low entropy regions: clsters in Italics are ``AGN CC-remnants'', while clusters in bold type are ``merger CC-remnants''.

Cluster
Metal abundance (solar) BCGa
A1650 $0.397 \pm 0.021$ Y
MKW3s $0.459 \pm 0.009$ Y
A4038b $0.402 \pm 0.008$ Y
A1644b $0.703 \pm 0.049$ Y
A1689 $0.298 \pm 0.017$ Y
A3558 $0.350 \pm 0.010$ Y
A576 $0.520 \pm 0.035$ Y
A754 $0.314 \pm 0.021$ Nc
A3562 $0.471 \pm 0.021$ Y
A3571 $0.349 \pm 0.013$ Y
A3667 $0.327 \pm 0.012$ N
A2256 $0.351 \pm 0.038$ N
A2319 $0.242 \pm 0.012$ Y
A3266 $0.232 \pm 0.039$ Y
A399 $0.221 \pm 0.053$ Y
A401 $0.262 \pm 0.044$ N
A3158 $ 0.275 \pm 0.077$ N
A119 $0.242 \pm 0.078$ N
A2255d $0.547 \pm 0.224$  
A3532d $0.473 \pm 0.095$  
Triangulum Australisd $0.369 \pm 0.151$  

Notes. (a) ``Y'' if the BCG is found in the low-entropy region and ``N'' if it is elsewhere. (b) even if the central entropy of this cluster is within the reach of AGN outbursts, it also shows some indications of on-going interaction and cannot be unambiguously associated to the ``AGN CC-remnant class'' (see text). (c) The BCG 2MASSX J09083238-0937470 is not associated to the CC-remnant, which however coincides with the position of the elliptical galaxy 2MASSX J09091923-0941591. (d) Due to the large indetermination of the metal abundance estimate, we could not unambiguously detect or exclude the presence of a metal abundance excess in this object.


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