Observing asymmetric structures in protoplanetary disks with MATISSE

We present a quantitative analysis of the potential capabilities of detecting local brightness asymmetries in circumstellar disks with the VLTI in the MIR wavelength range. To evaluate planet formation theories, direct observations of protoplanets still embedded in their host disk are indispensable. Due to the small angular separation from their host star, only long-baseline interferometry provides the angular resolution to detect disk asymmetries caused by protoplanets at (sub-)au scales. In particular, infrared observations are crucial to observe scattered stellar radiation and thermal re-emission in the vicinity of these planets directly. For this purpose, we performed mock observations with MATISSE in the L, M and N bands, based on radiative transfer simulations of protoplanetary disks hosting embedded companions. We find that the flux ratio of the embedded source to the central star can be as low as 0.6 % for a detection at a feasible significance level due to the heated dust in the vicinity of the embedded source. Furthermore, we find that the likelihood for detection is highest for sources at intermediate distances (2--5 au) and disk masses not higher than about 1e-4 M_sun.