  We investigate the morphology and resolved physical properties of a sample of
22 IR-selected DSFG at cosmic noon using the JWST/NIRCam images obtained in the
EGS field for the CEERS survey. The resolution of the NIRCam images allowed to
spatially resolve these galaxies up to 4.4um and identify their bulge even when
extinguished by dust. The goal of this study is to obtain a better
understanding of the formation and evolution of FIR-bright galaxies by
spatially resolving their properties using JWST in order to look through the
dust and bridge the gap between the compact FIR sources and the larger optical
SFG. Based on RGB images from the NIRCam filters, we divided each galaxy into
several uniformly colored regions, fitted their respective SEDs, and measured
physical properties. After classifying each region as SF or quiescent, we
assigned galaxies to three classes, depending on whether active SF is located
in the core, in the disk or in both. We find (i) that galaxies at a higher z
tend to have a fragmented disk with a low core mass fraction. They are at an
early stage of bulge formation. When moving toward a lower z, the core mass
fraction increases, and the bulge growth is associated with a stabilization of
the disk: the NIRCam data clearly point toward bulge formation in preexisting
disks. (ii) Lopsidedness is a common feature of DSFGs. It could have a major
impact on their evolution; (iii) 23% of galaxies have a SF core embedded in a
quiescent disk. They seem to be undergoing outside-in quenching, often
facilitated by their strong lopsidedness inducing instabilities. (iv) We show
that half of our galaxies with SF concentrated in their core are good SMG
counterpart candidates, demonstrating that compact SMGs are usually surrounded
by a larger, less obscured disk. (v) Finally, we found surprising evidence for
clump-like substructures being quiescent or residing in quiescent regions.
