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tokens: time-series, but all data points available in the original time-series are published in DR2. Consequently, all measurements are shown in the figures displaying Gaia light curves in this paper, and the disregarded measurements are identified by magenta crosses. Fig. 3 Skydistribution in Galactic coordinates of all LPV candidates published in Gaia DR2. Each star is drawn with a purple–red–yellow colour-grading scale according to the median ( G BP ) −median ( G RP e ) colour scale shown on the right of the figure. 3 Overview of the <italic>Gaia</italic> all-sky LPV survey We present in this section an overview of the all-sky Gaia DR2 catalogue of LPV candidates, together with light-curve examples. Validations on catalogue subsets according to distance to the Sun or stellar populations are presented in the next sections. 3.1 Sky distribution overview The sky distribution of all DR2 LPV candidates is shown in Fig. 3 , colour-coded with the G BP − G RP e colours 1 of the stars according to the colour-scale on the right of the figure. The Galactic disc, bulge, and halo are clearly visible, as well as the extra-galactic populations of the Magellanic Clouds (the two concentration areas below the Galactic plane at Galactic longitudes of about 285° for the Large Magellanic Cloud (LMC) and 303° for the Small Magellanic Cloud (SMC)) and of the Sagittarius dwarf galaxy (elongated tail below the Galactic bulge). The reddest LPV candidates (yellowish colour in the figure) are seen to be distributed in the Galactic plane, where dust leads to high extinctions. Fig. 4 Histogram of G time-series durations, in days, of all Gaia DR2 LPV candidates. The dashed blue histogram represents the subset of the catalogue published with periods for the sources. 3.2 Light-curve overview The histogram of the G -band time-series durations of all LPV candidates is shown in Fig. 4 , with the subset of sources with published periods shown by the dashed blue histogram. Only 27 sources have durations shorter than one year, while 90% of the sources have observationsover more than 1.5 yr. The time coverage of the measurements over the observation duration is equally important. To compute the time coverage, we divided the time-series into 20 equally spaced sub-time intervals, and computed the fraction of sub-time intervals that have non-zero measurements. The histogram of the resulting time coverage is shown in Fig. 5 . It shows a distribution of the number of stars with time coverages between 35% and 90% that is about equal. Fig. 5 Histogram of the time coverage (see Sect. 3.2 ), in percentage, of measurements in the cleaned G time-series of all Gaia DR2 LPV candidates (grey bars) and of the subset with published periods (blue bars). Fig. 6 Sky distribution of the G -band time-series durations of each DR2 LPV candidate, according to the colour scale shown on the right of the figure. Time-series with durations shorter than 500 d are plotted in yellow (they are mostly located in the