摘要
We present the mid-IR (MIR) morphologies for 64 star-forming galaxies at$0.2<z<2.5$with stellar mass$\rm{M_*>10^{9}~M_\odot}$using JWST MIRI observations from the Cosmic Evolution Early Release Science survey (CEERS). The MIRI bands span the MIR (7.7--21~ $\mu$ m), enabling us to measure the effective radii ( $R_{\rm{eff}}$ ) and Sérsic indexes of these SFGs at rest-frame 6.2 and 7.7$\mu$ m, which contains strong emission from Polycyclic aromatic hydrocarbon (PAH) features, a well-established tracer of star formation in galaxies. We define a ``PAH-band'' as the MIRI bandpass that contains these features at the redshift of the galaxy. We then compare the galaxy morphologies in the PAH-bands to those in rest-frame Near-UV (NUV) using HST ACS/F435W or ACS/F606W and optical/near-IR using HST WFC3/F160W imaging from UVCANDELS and CANDELS, where the NUV-band and F160W trace the profile of (unobscured) massive stars and the stellar continuum, respectively. The$R_{\rm{eff}}$of galaxies in the PAH-band are slightly smaller ( $\sim$ 10\%) than those in F160W for galaxies with$\rm{M_*\gtrsim10^{9.5}~M_\odot}$at$z\leq1.2$ , but the PAH-band and F160W have a similar fractions of light within 1 kpc. In contrast, the$R_{\rm{eff}}$of galaxies in the NUV-band are larger, with lower fractions of light within 1 kpc compared to F160W for galaxies at$z\leq1.2$ . Using the MIRI data to estimate the$\rm{SFR_{\rm{IR}}}$surface density, we find the correlation between the$\rm{SFR_{\rm{IR}}}$surface density and stellar mass has a steeper slope than that of the$\rm{SFR_{\rm{UV}}}$surface density and stellar mass, suggesting more massive galaxies having increasing amounts of obscured fraction of star formation in their inner regions. This paper demonstrates how the high-angular resolution data from JWST/MIRI can reveal new information about the morphology of obscured-star formation.