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Fig. A.1


Measured r-band amplitudes (Δr) and corresponding slopes (Δr/ Δ(ur)) are compared for WTTS members of spectral type M1 in our sample. Error bars on photometric amplitudes follow from the photometric noise estimate based on field stars sequence in Fig. 2; error bars on slope values are computed by simulating 1000 random (Δr,Δ(ur)) pairs uniformly distributed around the observed values within the uncertainties and measuring the corresponding scatter on computed slopes.

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