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In order to study the initial conditions of planet formation, it is crucialto obtain spatially resolved multi-wavelength observations of the innermostregion of protoplanetary discs. We evaluate the advantage of combiningobservations with MATISSE/VLTI and ALMA to constrain the radial and verticalstructure of the dust in the innermost region of circumstellar discs in nearbystar-forming regions. Based on a disc model with a parameterized dust densitydistribution, we apply 3D radiative-transfer simulations to obtain idealintensity maps. These are used to derive the corresponding wavelength-dependentvisibilities we would obtain with MATISSE as well as ALMA maps simulated withCASA. Within the considered parameter space, we find that constraining the dustdensity structure in the innermost $5\,$au around the central star ischallenging with MATISSE alone, whereas ALMA observations with reasonableintegration times allow us to derive significant constraints on the discsurface density. However, we find that the estimation of the different discparameters can be considerably improved by combining MATISSE and ALMAobservations. For example, combining a 30-minute ALMA observation (at 310 GHzwith an angular resolution of 0.03$^{\prime\prime}$) for MATISSE observationsin the L and M bands (with visibility accuracies of about $3\,\%$) allows theradial density slope and the dust surface density profile to be constrained towithin $\Delta \alpha=0.3$ and $\Delta (\alpha-\beta)=0.15$, respectively. Foran accuracy of ${\sim 1\%}$ even the disc flaring can be constrained to within$\Delta \beta=0.1$. To constrain the scale height to within $5\,$au, M bandaccuracies of $0.8\,\%$ are required. While ALMA is sensitive to the number oflarge dust grains settled to the disc midplane we find that the impact of thesurface density distribution of the large grains on the observed quantities issmall.

The potential of combining MATISSE and ALMA observations: Constraining the structure of the innermost region in protoplanetary discs