$0\fdg49$, $0\fdg62$, and $0\fdg82$ FWHM beam widths, respectively. The maps are prepared in the HEALPix[^2] format with ${\rm nside}=512$ (Górski, Hivon, & Wandelt 1999). The total number of pixels of each map is $12\times {\rm nside}^2 = 3,145,728$. Since the K and Ka band maps are dominated by Galactic foregrounds, we use only Q, V, and W band data in our analysis.

The Galactic dust, free-free, and synchrotron emissions are highly non-Gaussian sources, and their contribution to the measured genus is not negligible even at high Galactic latitude (PPR). Therefore, we use the 100 $\mu{\rm m}$ dust (Schlegel, Finkbeiner, & Davis 1998; Finkbeiner, Davis, & Schlegel 1999), H$\alpha$ (Finkbeiner 2003), and synchrotron (Haslam et al. 1981, 1982) emission maps multiplied with coefficients given in Table 3 of Bennett et al. (2003b) to reduce the foreground emission in each differencing assembly map of the Q, V, and W bands. At each frequency band, we combine the foreground-subtracted WMAP differencing assembly maps with noise weight given by $N_{\rm obs}/\sigma_0^2$, where $N_{\rm obs}$ is the effective number of observations at each pixel, and $\sigma_0$ is the global noise level of the map (Bennett et al 2003a, Table 1). Finally, we obtain three foreground-subtracted 