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    PR # 31259                                                                   
     One of the most striking results on clusters of galaxies field obtain       
     ed  with ASCA is existance of metal abundance gradient in cool cD clu       
     sters.  Its scale-length of the abundance gradient is about 100kpc, w       
     hich is  smilar to the typical size of cD. The result implies a relat       
     ionship between  cD and the abaundace gradient. On the other hand, th       
     e existance of abundance  gradient in hot component extending over th       
     e cluster tells us there is no  relationship between cD and the abund       
     ace gradient. The best way to solve  the problem is to observe non-cD       
      cluster. However, there has been no  observation of non-cD cool clus       
     ters. Then, we propose two non-cD-type cool  clusters of galaxies; A4       
     00 and A539.                                                                
                                                                                 
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