4636, but the galaxy density is high around them and thus they are identified as centers of galaxy groups. We also compare with galaxy clusters such as Abell 262, Abell 1060, AWM 7, and Centaurus. Following Sato at al. (2009b), we plot the correlation between temperature and MLR at 0.1 $r_{180}$ in figure 12. This result shows that MLR of groups and galaxies with a temperature of $\sim$1 keV, including NGC 4636, is $\sim$5 times lower than that for clusters. Among galaxies and groups, NGC 4636, NGC 5044 and HCG 62 exhibit a spherically symmetric X-ray emission, and NGC 4636 has the lowest MLR among them. A possible correlation between temperature and MLR is suggested only for these spherically symmetric objects. Such a correlation could be explained by higher temperature systems possessing a deeper gravitational potential which prevents dispersal of the metals. Although galaxy velocity dispersion is larger for higher temperature clusters, there are no big galaxies around cD galaxies. Therefore, we think that the deep potential can confine the metals even if a small galaxy passes around the cD galaxy. On the other hand, the X-ray asymmetric groups NGC 1399 and NGC 507 show a relatively low MLR. These 