Gaia Data Release 2
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Fig. 2


Maximum variogram value as a function of the mean G CCD magnitude for known constant and variable sources from the OGLE survey as observed by Gaia. The grey line shows the detection threshold derived from simulated Gaia-like light curves (see Roelens et al. 2017). The brown line corresponds to the same threshold definition scaled by a factor of 10. Panel a: colour-coded by period POGLE from the OGLE catalogue, and panel b: colour-coded by IQR from Gaia per-CCD G photometry. It appears that with this detection threshold γdet = 10γdet,simu, panel a: majority of constant stars and a significant fraction of longer-period variables are not detected as candidates with short-timescale variability when the variogram is used, and panel b: variable sources that are not detected with the variogram approach are low-amplitude sources.

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