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The formation of multiple stellar systems is a natural by-product of thestar-formation process, and its impact on the properties of protoplanetarydiscs and on the formation of planets is still to be fully understood. To date,no detailed uniform study of the gas emission from a sample of protoplanetarydiscs around multiple stellar systems has been performed. Here we analyse newALMA observations at a $\sim$21 au resolution of the molecular CO gas emissiontargeting discs in eight multiple stellar systems in the Taurus star-formingregions. $^{12}$CO gas emission is detected around all primaries and in sevencompanions. With these data, we estimate the inclination and the position anglefor all primary discs and for five secondary or tertiary discs, and measure thegas disc radii of these objects with a cumulative flux technique on thespatially resolved zeroth moment images. When considering the radius including95\% of the flux as a metric, the estimated gas disc size in multiple stellarsystems is found to be on average $\sim 4.2$ times larger than the dust discsize. This ratio is higher than what was recently found in a population of moreisolated and single systems. On the contrary, when considering the radiusincluding 68\% of the flux, no difference between multiple and single discs isfound in the distribution of ratios. This discrepancy is due to the sharptruncation of the outer dusty disc observed in multiple stellar systems. Themeasured gas disc sizes are consistent with tidal truncation models in multiplestellar systems assuming eccentricities of $\sim0.15$-$0.5$, as expected intypical binary systems.

Observational constraints on disc sizes in protoplanetary discs in multiple systems in the Taurus region. II. Gas disc sizes