Fe abundances are similar between the two galaxies, but metal abundances are about twice as high as those of NGC 1399 in all radial regions. In Figure 9, radial profiles of the abundance ratios of O, Ne, Mg, and Si against Fe are shown, with error bars estimated from the allowed slope of the confidence contours in Figure 6. For comparison, the abundance ratios for a model of SN II (for all elements) and SN Ia (for Si) are also shown. The abundance ratios for SN II are calculated by integrating the metal mass ejected by SNe II (Iwamoto et al. 2006) with a progenitor mass from 10M$_{\odot}$ to 50M$_{\odot}$, weighting by the Salpeter initial mass function, and calculated, for example, as O: 1.80M$_{\odot}$ and Fe: 0.0907M$_{\odot}$. The W7 model (O: 0.143M$_{\odot}$ and Fe: 0.749M$_{\odot}$ ; Iwamoto et al. 1999) is used for SN Ia. The result indicates that all metal abundances can be explained by a mixture of SN II and SN Ia products. This indicates that, in NGC 4636 and NGC 1399, each metal diffused to the outside of the galaxy after mixing products from both SN II and SN Ia. For NGC 4636, all the abundance ratios 