Binned flux of the recovered variable stars. The flux is calibrated to a zeropoint at mag 30. The dashed lines show the baseline for each object. Since the observations used to determine the baseline cannot be binned, we show the unbinned data in the baseline region of each object. This region is marked by the black lines. All three objects vary around their central values, but the amplitude varies widely between the ZTF bands. We note that the values for PTF10qpf have been divided by 100 as the variability is so large.