Solar system analogs host a remnant of the protoplanetary disks around the central star, the so-called debris disks. These are formed as a by-product of planet formation and consist of material left over from planet formation, such as dust, gas, and planetesimals belts. Due to dust's short lifespan, it requires continuous replenishment through planetesimal collisions, highlighting the interconnected nature of these components. Additionally, substellar companions can significantly influence dust and planetesimal dynamics through gravitational effects. Even Earth-sized planets can leave distinctive marks on debris disk structures, while misaligned planets or those with elliptical orbits may reveal past gravitational interactions. Thus, tracing substellar companions such as planets or perturbers within debris disks can provide crucial insights and constraints into their evolution. Using N-body simulations, SPH simulations, and collisional evolution models of debris disk systems, the community demonstrated observable planet-disk configurations with large-scale signatures of the brightness distributions (e.g., spiral structures and/or two local azimuthal maxima).

These features are potentially detectable using high-resolution near-to-mid infrared imaging facilities. In this session, we will discuss recent observations of possible planet-disk interactions using JWST and VLT/ERIS, placing them in the context of debris disk simulations that incorporate planetary interaction. We will also highlight how future instruments on the ELT, such as MORFEO/MICADO or PCS, will enhance our understanding of the formation, architecture, and evolution of planetary systems in solar system analogues.