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   PR # 41273
   One of the most striking results on clusters of galaxies field
   obtained with ASCA is existance of metal abundance gradient in cool
   cD clusters. Its scale-length of the abundance gradient is about
   100kpc, which is smilar to the typical size of cD. The result implies
   a relationship between cD and the abaundace gradient. On the other
   hand, the existance of abundance gradient in hot component extending
   over the cluster tells us there is no relationship between cD and the
   abundace gradient. The best way to solve the problem is to observe
   non-cD cluster. However, there has been no observation of non-cD cool
   clusters. Then, we propose two non-cD-type cool clusters of galaxies;
   A168.
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