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HD141569 is a pre-main sequence star with a disc uniquely placed betweenprotoplanetary and debris discs, similar to the older `hybrid' type discs. Thiswork aims to place the mass and spatial structure of the disc midplane in thecontext of the debris, hybrid and protoplanetary discs. We observed HD~141569with ALMA in 1.3~mm continuum and $^{13}$CO (2-1). This is the first detectionand image of the optically thin gas emission from the midplane of this disc. Incontinuum emission, we detect a combination of an unresolved central peak and aring of millimetre emission at 220$\pm$10~au, slightly interior to one of therings discovered in scattered light. The minimum dust mass of the ring is0.13$\pm$0.02~M$_{\oplus}$ while the unresolved millimetre peak at the stellarlocation is predominantly thermal emission due to a minimum of1.2$\pm$0.2~M$_{\oplus}$ of dust. $^{13}$CO is distributed asymmetricallyaround the stellar position with a peak at 1.1" distance and a P.A. of-33$^\circ$. The gas is detected as far as 220$\pm$10~au, a radial separationthe same as that of the mm ring. Assuming optically thin emission and standardISM abundances, we use our $^{13}$CO data to derive the gas mass in the disc of(6.0$\pm$0.9) $\times 10^{-4}~$M$_\odot$. Comparison to published $^{12}$COdata shows that $^{12}$CO is optically thick, explaining why estimates based on$^{12}$CO underestimated the gas mass.

Unlocking the secrets of the midplane gas and dust distribution in the young hybrid disc HD 141569