  Recent studies have shown that galaxies at cosmic noon are redder in the
center and bluer in the outskirts, mirroring results in the local universe.
These color gradients could be caused by either gradients in the stellar age or
dust opacity; however, distinguishing between these two causes is impossible
with rest-frame optical photometry alone. Here we investigate the underlying
causes of the gradients from spatially-resolved rest-frame $U-V$ vs. $V-J$
color-color diagrams, measured from early observations with the James Webb
Space Telescope. We use $1\, \mu m - 4\, \mu m$ NIRCam photometry from the
CEERS survey of a sample of 54 galaxies with $M_* / M_\odot>10$ at redshifts
$1.7<z<2.3$ selected from the 3D-HST catalog. We model the light profiles in
the F115W, F200W and F356W NIRCam bands using \texttt{imcascade}, a Bayesian
implementation of the Multi-Gaussian expansion (MGE) technique which flexibly
represents galaxy profiles using a series of Gaussians. We construct resolved
rest-frame $U-V$ and $V-J$ color profiles. The majority of star-forming
galaxies have negative gradients (i.e. redder in the center, bluer in the
outskirts) in both $U-V$ and $V-J$ colors consistent with radially decreasing
dust attenuation. A smaller population (roughly 15\%) of star-forming galaxies
have positive $U-V$ but negative $V-J$ gradients implying centrally
concentrated star-formation. For quiescent galaxies we find a diversity of UVJ
color profiles, with roughly one-third showing star-formation in their center.
This study showcases the potential of JWST to study the resolved stellar
populations of galaxies at cosmic noon.
