Irene Shivaei (Centro di Astrobiología, Madrid) 

Dust at Cosmic Noon with JWST and ALMA

A crucial component of the baryonic matter in galaxies is the ISM consisting of gas and solid-phase metals called dust. Dust determines how galaxies look from UV to IR, how the ISM behaves, and the very process of star formation. We are now at the beginning of an exciting journey with the unprecedented IR capabilities, high sensitivity, and high angular resolution of JWST/MIRI compared to its predecessors such as Spitzer. For the first time, we are able to not only detect warm dust emission in individual typical galaxies across masses and star formation rates (SFRs) at cosmic noon, but also resolve the dust-obscured SFR z~1-2. In this talk, I will show our recent results on the mid-IR dust emission of galaxies at cosmic noon (z~1-3) from the SMILES multi-band MIRI survey, particularly how the PAH mass fraction and obscured star formation fraction evolve from z~0 (local studies) to z~2. Additionally, in synergy with ALMA studies, I will present results on a tight and universal correlation between PAH and CO emission, marking a new base for the studies of dust and gas at cosmic noon.