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Fig. 4


Summary of observed radio flux variability (left panel) and fractional radio flux variability (right panel). We omitted sources which were not detected in both our 10 GHz observations and the previous 7.5 GHz observations of Dzib et al. (2013), since there is essentially no constraint on their time variability. For sources detected from at least one of those observations, we present the flux variation by calculating the average of the differences between the measured 10 GHz flux in our VLA observations and the expected 10 GHz flux derived by re-scaling the 7.5 GHz flux from Dzib et al. (2013) to 10 GHz assuming α = − 0.1 and 2.0. Vertical error bars take the measurement errors and the spectral index range [−0.1, 2.0] into consideration. Dashed lines in the left panel show the expected radio fluxes from EUV photoevaporation winds from protoplanetary disks, assuming the EUV flux ΦEUV = 1040 (bottom), 1041 (middle), and 1042 photons s−1 (top).

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