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We present simulations of the capabilities of the Atacama LargeMillimeter/submillimeter Array (ALMA) and of a Next Generation Very Large Array(ngVLA) to detect and resolve substructures due to terrestrial planets andSuper-Earths in nearby planet-forming disks. We adopt the results of global 2-Dhydrodynamical planet-disk simulations that account for the dynamics of gas anddust in a disk with an embedded planet. Our simulations follow the combinedevolution of gas and dust for several thousand planetary orbits. We show thatlong integrations (several tens of hours) with the ngVLA can detect andspatially resolve dust structures due to low-mass rocky planets in theterrestrial planet formation regions of nearby disks (stellocentric radii $r =1 - 3$ au), under the assumption that the disk viscosity in those regions islow ($\alpha \le 10^{-5}$). ALMA is instead unable to resolve these structuresin these disk regions. We also show that high-resolution ngVLA observationsseparated by several days to few weeks would allow to detect the proper motionof the azimuthally asymmetric structures expected in the disk regions ofterrestrial planet formation.

Imaging the Dusty Substructures due to Terrestrial Planets in Planet-forming Disks with ALMA and the Next Generation Very Large Array