Constraining the chemical conditions of IRAS 4A2 protostar at planet-forming scales

Young solar-like protostars (Class 0/I YSOs, < 1 Myr age) have been recently claimed to likely host forming planets. In particular, in the hot, dense, compact of their inner envelopes, the "hot corinos", a rich complex organic chemistry can be found, with so-called interstellar complex organic molecules (iCOMs). These are found to be building blocks of key prebiotic molecules. Moreover, pristine building blocks of the Solar System, e.g. comets and asteroids, show in their composition traces of prebiotic compounds, like amino acids. Therefore, characterizing the chemical content of the earliest stages of the planetary formation process is crucial to understanding if forming planets can inherit the protostellar molecular complexity and eventually bring the emergency of life in other planetary systems than our own. The ALMA Large Program FAUST, capable of resolving the inner 50 AU scales of a sample of Class 0/I protostars, allows me to image and compare the spatial distribution of several iCOMs in the archetypical Class 0 protostar IRAS 4A2. I actually find spatial segregation in a sample of 5 iCOMs, with glycolaldehyde and methanol showing the most compact (r ~ 20 au) and extended (r ~ 40 AU) emission size, respectively. Moreover, by performing an LTE molecular lines analysis I also constrain the physical properties of the hot corino gas, namely, iCOMs column densities and gas temperature probed by these molecules. Are different iCOMs tracing different scales in the planet-forming region around a young solar-like protostar? Are these scales associated with different gas temperatures? Can we infer a gas temperature profile in the planet-forming region of such Class 0 YSO exploiting the observed iCOMs spatial segregation and emission lines?