Fig. D.1
Eclipses of KELT-9b for AORs r67667712 (left panel) and r67667968 (right panel). Top row: raw photometric lightcurve with our best fit PLD model. Middle row: corrected lightcurves with the best fit eclipse model. Bottom row: RMS vs. binsize of the data; since this closely follows the photon noise line (
) we can see that we are capturing the systematics well.
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