MHz is larger than the APS at 197 MHz on the small scale. On the other hand, as shown in the left panel, the APS at 197 MHz exceeds the APS at 168 MHz in range of $\rm LST< -13$ and $\rm LST > 16$ on large scale. During observation with these LST, the pointing is off-zenith and then the MWA has large side lobes (e.g. [@2015RaSc...50..614N]). Furthermore the gain of the side lobe is high at high frequency, and the second side lobe is close to the Galactic center. Thus, the enhancement of the APS at 197 MHz on large scale shows the leakage of the Galactic synchrotron emission. [ The top left panel of Fig. \[fig:CPSLST\] shows the LST dependence of the absolute CPS at $l=100$. As is the case for the APS, the CPS increases at LST $<$ –13 degrees where the APS has serious foreground contamination, and the CPS at 197 MHz is larger than the CPS at 168 MHz. The LST dependence is apparent in the bottom left panel, which shows the CPS in linear scale. Apart from foreground contamination at LST $<$ -13 degrees, the amplitude of CPS at 167 MHz is larger than 