after foreground-template correction is known to be very low. Bennett et al. (2003b) estimate that the residual Galactic contamination after the template correction is 2.2%, 0.8%, and $< 0.4$% of the CMB power in Q, V, and W band, respectively, when the less conservative Kp2 mask is applied. Tegmark et al. (2003) also show that the foregrounds in their TCM are subdominant in all but the very innermost Galactic plane, for $\ell \la 100$. Furthermore, Galaxy foregrounds induce non-Gaussian feature by making the genus shifted to the left at all threshold levels. As for the positive $\Delta g$ on the southern hemisphere in the high resolution W band data, it is more reliable that such non-Gaussianity is caused by point sources that have not been removed by the Kp0 mask because positive $\Delta g$ means that more hot spots are present than cold spots. Furthermore, another non-Gaussian signature, the large genus amplitude difference between the north and the south, does not show frequency dependence since all WMAP band maps (Q, V, and W), ILC and TCM show the similar non-Gaussian feature. It should be noted that the three independent methods of foreground-subtraction were applied to make the WMAP band maps, 