the observed values in Table 3 at all Q, V, and W bands is only 1.4%.

![image](jfig5.eps){width="160mm"}

With a Galactic cut at $b=30\degr$, the large cold spots are removed (Fig. 4$c$). However, the trend of the genus amplitudes and asymmetries in the north and south are not significantly changed by the Galactic cuts (see Tables 1 and 3). For the Galactic cut at $b=30\degr$, $A_{-}^{\rm N}-A_{-}^{\rm S}$ and $\Delta g$ still deviate from the Gaussian prediction at $1.6\sigma$ and $1.8\sigma$ levels, respectively. Since the genus amplitude significantly decreases with higher Galactic cut, it is natural that the difference between $A_{-/+}^{\rm N}$ and $A_{-/+}^{\rm S}$ should be smaller while its standard deviation in the mock observations becomes larger due to sample variance. However, the probability that such genus amplitude differences are larger than the measured values for $b=30\degr$ cut is still 4.6%. All non-Gaussian features of the W band map described above are also seen in the TCM (Tables 1 and 3; Fig. 5$d$).

Origin of the Non-Gaussianity
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Let us consider possible sources that may induce the non-Gaussian signatures shown in $\S4$. First, the foreground effect on the genus may not be negligible, causing non-Gaussianity. The residual of the foregrounds 