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The combination of high resolution and sensitivity offered by ALMA isrevolutionizing our understanding of protoplanetary discs, as their bulk gasand dust distributions can be studied independently. In this paper we presentresolved ALMA observations of the continuum emission ($\lambda=1.3$ mm) and COisotopologues ($^{12}$CO, $^{13}$CO, C$^{18}$O $J=2-1$) integrated intensityfrom the disc around the nearby ($d = 162$ pc), intermediate mass($M_{\star}=1.67\,M_{\odot}$) pre-main-sequence star CQ Tau. The data show aninner depression in continuum, and in both $^{13}$CO and C$^{18}$O emission. Weemploy a thermo-chemical model of the disc reproducing both continuum and gasradial intensity profiles, together with the disc SED. The models show that agas inner cavity with size between 15 and 25 au is needed to reproduce the datawith a density depletion factor between $\sim 10^{-1}$ and $\sim 10^{-3}$. Theradial profile of the distinct cavity in the dust continuum is described by aGaussian ring centered at $R_{\rm dust}=53\,$au and with a width of$\sigma=13\,$au. Three dimensional gas and dust numerical simulations of a discwith an embedded planet at a separation from the central star of $\sim20\,$auand with a mass of $\sim 6\textrm{-} 9\,M_{\rm Jup}$ reproduce qualitativelythe gas and dust profiles of the CQ Tau disc. However, a one planet modelappears not to be able to reproduce the dust Gaussian density profile predictedusing the thermo-chemical modeling.

A dust and gas cavity in the disc around CQ Tau revealed by ALMA