and frequency dependence at $l<300$. This result suggests that the CPS has only a few independent modes at large scales and the modes do not vary with frequency. Furthermore, at $l>1200$, the CPS is always positive, and this indicates unexpected systematics at small scales. ]{}

![The APS computed from visibility data with 1.28 MHz bandwidth. The redder line shows the low frequency data and the bluer shows high frequency. At small scales, the high frequency APS is smaller than the low frequency APS. However, the some of APS at high frequency enhanced at large scales. This is caused by the leakage of Galactic synchrotron emission from the side lobe. []{data-label="fig:APSfreq"}](./Fig_paper/Draft_Cl_from_vis_all_nweight_inJy.eps){width="7.5cm"}

![[Same as Fig. \[fig:APSfreq\], but for the CPS calculated from images. We show the absolute value in top panel, and the bottom panel shows the signal in linear scale. ]{}[]{data-label="fig:CPSfreq"}](./Fig_paper/X_B1.eps "fig:"){width="7.5cm"} ![[Same as Fig. \[fig:APSfreq\], but for the CPS calculated from images. We show the absolute value in top panel, and the bottom panel shows the signal in linear scale. ]{}[]{data-label="fig:CPSfreq"}](./Fig_paper/X_B1_noabs.eps "fig:"){width="7.5cm"}

Results {#S:results}
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[In this section, we discuss the APS and CPS from the MWA data and the Planck CMB map after 3 hours integration.]{}

Angular power spectrum
