Mitchell Institute for Fundamental Physics & Astronomy
College Station, Texas 77843
Tracking spatially resolved star formation in galaxies will provide insight into galaxy‘s structural and size evolution. However, dust obscuration posts an immense challenge in uncovering spatially resolved star-formation activities, due to insufficient data to measure the profile of dust-obscured star formation. The Mid-Infrared Instrument (MIRI) on the James Webb Space Telescope (JWST) enables us to measure the morphology of galaxy in mid-IR region which probe more on the obscured star formation. In this talk, we present the mid-IR morphologies for 70 star-forming galaxies at 0.2<z<2.5 using JWST MIRI observations from the Cosmic Evolution Early Release Science survey (CEERS). Particularly, we focus on the morphology measured in rest-frame 6.2 and 7.7 micron, which contains strong emission from Polycyclic aromatic hydrocarbon (PAH) features, a well-established tracer of star formation in galaxies. We compare the PAH-band morphologies to those measured in rest-frame Near-UV (NUV) and optical/near-IR using HST imaging from UVCANDELS and CANDELS, which trace the profile of (unobscured) massive stars and the stellar continuum, respectively.