CLEAR: The Morphological Evolution of Galaxies in the Green Valley

• Published in: The Astrophysical journal Vol. 951; no. 2; pp. 115 - 129
• Main Authors: Estrada-Carpenter, Vicente, Papovich, Casey, Momcheva, Ivelina, Brammer, Gabriel, Simons, Raymond C., Cleri, Nikko J., Giavalisco, Mauro, Matharu, Jasleen, Trump, Jonathan R., Weiner, Benjamin, Ji, Zhiyuan
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.07.2023; IOP Publishing
• Subjects: Astronomical models; Astrophysics; Compact galaxies; Divergence; Galactic evolution; Galaxies; Galaxy evolution; Galaxy quenching; Galaxy spectroscopy; Hubble Space Telescope; Ionization; Morphology; Red shift; Space telescopes; Star & galaxy formation; Star formation; Star formation rate; Stars; Stars & galaxies; Stellar evolution; Stellar mass; Valleys
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/acd4be

Quiescent galaxies having more compact morphologies than star-forming galaxies has been a consistent result in the field of galaxy evolution. What is not clear is at what point this divergence happens, i.e., when do quiescent galaxies become compact, and how big of a role does the progenitor effect play in this result? Here we aim to model the morphological and star formation histories of high-redshift (0.8 < z < 1.65) massive galaxies ( log ( M / M ⊙ ) > 10.2) with stellar population fits using Hubble Space Telescope/WFC3 G102 and G141 grism spectra plus photometry from the CANDELS Ly α Emission at Reionization (CLEAR) survey, constraining the star formation histories for a sample of ∼400 massive galaxies using flexible star formation histories. We develop a novel approach to classifying galaxies by their star formation activity in a way that highlights the green valley population, by modeling the specific star formation rate distributions as a function of redshift and deriving the probability that a galaxy is quiescent ( P Q ). Using P Q and our flexible star formation histories we outline the evolutionary paths of our galaxies in relation to stellar mass, Sérsic index, effective radius R eff , and stellar mass surface density. We find that the galaxies show no appreciable stellar mass growth after entering the green valley (a net decrease of 4%) while their stellar mass surface densities increase by ∼0.25 dex. Therefore galaxies are becoming compact during the green valley and this is due to an increase in the Sérsic index and a decrease in R eff .