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We present a measurement of the low-mass quiescent size-mass relation atCosmic Noon (1<z<3) from the JWST PRIMER and UNCOVER treasury surveys, whichhighlight two distinct classes of quiescent galaxies. While the massivepopulation is well studied at these redshifts, the low-mass end has beenpreviously under-explored due to a lack of observing facilities with sufficientsensitivity and spatial resolution (in the rest-frame near-IR). We select aconservative sample of robust low-mass quiescent galaxy candidates usingrest-frame UVJ colors and specific star formation rate criteria and measuregalaxy morphology in both rest-frame UV/optical wavelengths (F150W) andrest-frame near-infrared (F444W). We confirm an unambiguous "flattening" of thelow-mass quiescent size-mass relation, which results from the separation of thequiescent galaxy sample into two distinct populations at$\log(M_\star/M_\odot)\sim10.3$: low-mass quiescent galaxies that are notablyyounger and have disky structures, and massive galaxies with prolatemorphologies and older median stellar ages. These separate populations implymass quenching dominates at the massive end while other mechanisms, such asenvironmental or feedback-driven quenching, form the low-mass end. This stellarmass dependent slope of the quiescent size-mass relation could also indicate ashift from size growth due to star formation (low masses) to growth via mergers(massive galaxies). The transition mass between these two populations alsocorresponds with other dramatic changes in galaxy evolutions (e.g.star-formation efficiency, dust obscuration, and stellar-halo mass ratios),further highlighting the stark dichotomy between low-mass and massive galaxyformation.

Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER