Evolution of the Sérsic index up to <i>z</i> = 2.5 from JWST and HST

Context. The Hubble Space Telescope (HST) has long been the only instrument able to allow us to investigate the structure of galaxies up to redshift z = 3, limited to the rest-frame UV and optical. The James Webb Space Telescope (JWST) is now unveiling the rest-frame near-IR structure of galaxies, less affected by dust attenuation and more representative of their underlying stellar mass profiles. Aims. We measure the evolution with redshift of the rest-frame optical and near-IR Sérsic index ( n ), and examine the dependence on stellar mass and star-formation activity across the redshift range 0.5 ≤ z ≤ 2.5. Methods. For an HST-selected parent sample in the CANDELS fields we infer rest-frame near-IR Sérsic profiles for ≈15 000 galaxies in publicly available NIRCam imaging mosaics from the COSMOS-Web and PRIMER surveys. We augment these with rest-frame optical Sérsic indices, previously measured from HST imaging mosaics. Results. The median Sérsic index evolves slowly or not at all with redshift, except for very high-mass galaxies ( M ⋆ &gt; 10 11 M ⊙ ), which show an increase from n ≈ 2.5 to n ≈ 4 at z &lt; 1. High-mass galaxies have higher n than lower-mass galaxies (the sample reaches down to M ⋆ = 10 9.5 M ⊙ ) at all redshifts, with a stronger dependence in the rest-frame near-IR than in the rest-frame optical at z &gt; 1. This wavelength dependence is caused by star-forming galaxies that have lower optical than near-IR n at z &gt; 1 (but not at z &lt; 1). Both at optical and near-IR wavelengths, star-forming galaxies have lower n than quiescent galaxies, confirming and fortifying the result that across cosmic time a connection exists between star-formation activity and the radial stellar mass distribution. Besides these general trends that confirm previous results, two new trends emerge: (1) at z &gt; 1 the median near-IR n varies strongly with star formation activity, but not with stellar mass, and (2) the scatter in near-IR n is substantially higher in the green valley (0.25 dex) than on the star-forming sequence and among quiescent galaxies (0.18 dex) – this trend is not seen in the optical because dust and young stars contribute to the variety in optical light profiles. Our newly measured rest-frame near-IR radial light profiles motivate future comparisons with radial stellar mass profiles of simulated galaxies as a stringent constraint on processes that govern galaxy formation.