Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER. (arXiv:2312.15012v1 [astro-ph.GA])

Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER. (arXiv:2312.15012v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Cutler_S/0/1/0/all/0/1">Sam E. Cutler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Whitaker_K/0/1/0/all/0/1">Katherine E. Whitaker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weaver_J/0/1/0/all/0/1">John R. Weaver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_B/0/1/0/all/0/1">Bingjie Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pan_R/0/1/0/all/0/1">Richard Pan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bezanson_R/0/1/0/all/0/1">Rachel Bezanson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Furtak_L/0/1/0/all/0/1">Lukas J. Furtak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Labbe_I/0/1/0/all/0/1">Ivo Labbe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leja_J/0/1/0/all/0/1">Joel Leja</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Price_S/0/1/0/all/0/1">Sedona H. Price</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cheng_Y/0/1/0/all/0/1">Yingjie Cheng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clausen_M/0/1/0/all/0/1">Maike Clausen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cullen_F/0/1/0/all/0/1">Fergus Cullen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dayal_P/0/1/0/all/0/1">Pratika Dayal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graaff_A/0/1/0/all/0/1">Anna de Graaff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dickinson_M/0/1/0/all/0/1">Mark Dickinson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunlop_J/0/1/0/all/0/1">James S. Dunlop</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feldmann_R/0/1/0/all/0/1">Robert Feldmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Franx_M/0/1/0/all/0/1">Marijn Franx</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giavalisco_M/0/1/0/all/0/1">Mauro Giavalisco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glazebrook_K/0/1/0/all/0/1">Karl Glazebrook</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Greene_J/0/1/0/all/0/1">Jenny E. Greene</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grogin_N/0/1/0/all/0/1">Norman A. Grogin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Illingworth_G/0/1/0/all/0/1">Garth Illingworth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koekemoer_A/0/1/0/all/0/1">Anton M. Koekemoer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kokorev_V/0/1/0/all/0/1">Vasily Kokorev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marchesini_D/0/1/0/all/0/1">Danilo Marchesini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maseda_M/0/1/0/all/0/1">Michael V. Maseda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_T/0/1/0/all/0/1">Tim B. Miller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nanayakkara_T/0/1/0/all/0/1">Themiya Nanayakkara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nelson_E/0/1/0/all/0/1">Erica J. Nelson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Setton_D/0/1/0/all/0/1">David J. Setton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shipley_H/0/1/0/all/0/1">Heath Shipley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suess_K/0/1/0/all/0/1">Katherine A. Suess</a>

We present a measurement of the low-mass quiescent size-mass relation at
Cosmic Noon (1<z<3) from the JWST PRIMER and UNCOVER treasury surveys, which
highlight two distinct classes of quiescent galaxies. While the massive
population is well studied at these redshifts, the low-mass end has been
previously under-explored due to a lack of observing facilities with sufficient
sensitivity and spatial resolution (in the rest-frame near-IR). We select a
conservative sample of robust low-mass quiescent galaxy candidates using
rest-frame UVJ colors and specific star formation rate criteria and measure
galaxy morphology in both rest-frame UV/optical wavelengths (F150W) and
rest-frame near-infrared (F444W). We confirm an unambiguous “flattening” of the
low-mass quiescent size-mass relation, which results from the separation of the
quiescent galaxy sample into two distinct populations at
$log(M_star/M_odot)sim10.3$: low-mass quiescent galaxies that are notably
younger and have disky structures, and massive galaxies with prolate
morphologies and older median stellar ages. These separate populations imply
mass quenching dominates at the massive end while other mechanisms, such as
environmental or feedback-driven quenching, form the low-mass end. This stellar
mass dependent slope of the quiescent size-mass relation could also indicate a
shift from size growth due to star formation (low masses) to growth via mergers
(massive galaxies). The transition mass between these two populations also
corresponds 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 galaxy
formation.

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