Carbon and Iron Deficiencies in Quiescent Galaxies at z = 1–3 from JWST-SUSPENSE: Implications for the Formation Histories of Massive Galaxies

Carbon and Iron Deficiencies in Quiescent Galaxies at z = 1–3 from JWST-SUSPENSE: Implications for the Formation Histories of Massive Galaxies

We present the stellar metallicities and multielement abundances (C, Mg, Si, Ca, Ti, Cr, and Fe) of 15 massive (log M / M _⊙ = 10.2–11.2) quiescent galaxies at z = 1–3, derived from ultradeep JWST-SUSPENSE spectra. Compared to quiescent galaxies at z ∼ 0, these galaxies exhibit a deficiency of 0.26...

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Main Authors: Aliza G. Beverage, Martje Slob, Mariska Kriek, Charlie Conroy, Guillermo Barro, Rachel Bezanson, Gabriel Brammer, Chloe M. Cheng, Anna de Graaff, Natascha M. Förster Schreiber, Marijn Franx, Brian Lorenz, Pavel E. Mancera Piña, Danilo Marchesini, Adam Muzzin, Andrew B. Newman, Sedona H. Price, Alice E. Shapley, Mauro Stefanon, Katherine A. Suess, Pieter van Dokkum, David Weinberg, Daniel R. Weisz
Format: Article
Language:English
Published: IOP Publishing 2025-01-01
Series:The Astrophysical Journal
Subjects:
Galaxy quenching
Galaxy formation
Metallicity
Chemical abundances
Online Access:https://doi.org/10.3847/1538-4357/ad96b6
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Summary:We present the stellar metallicities and multielement abundances (C, Mg, Si, Ca, Ti, Cr, and Fe) of 15 massive (log M / M _⊙ = 10.2–11.2) quiescent galaxies at z = 1–3, derived from ultradeep JWST-SUSPENSE spectra. Compared to quiescent galaxies at z ∼ 0, these galaxies exhibit a deficiency of 0.26 ± 0.04 dex in [C/H], 0.16 ± 0.03 dex in [Fe/H], and 0.07 ± 0.04 dex in [Mg/H], implying rapid formation and quenching before significant enrichment from asymptotic giant branch stars and Type Ia supernovae. Additionally, we find that galaxies forming at higher redshift consistently show higher [Mg/Fe] and lower [Fe/H] and [Mg/H], regardless of their observed redshift. The evolution in [Fe/H] and [C/H] is therefore primarily driven by lower-redshift samples naturally including galaxies with longer star formation timescales. In contrast, the lower [Mg/H] likely reflects earlier-forming galaxies expelling larger gas reservoirs during their quenching phase. Consequently, the mass–metallicity relation, primarily reflecting [Mg/H], is somewhat lower at z = 1–3 compared to the lower-redshift relation. Finally, we compare our results to standard stellar population modeling approaches employing solar abundance patterns and nonparametric star formation histories (using Prospector ). Our simple stellar population (SSP)-equivalent ages agree with the mass-weighted ages from Prospector , while the metallicities disagree significantly. Nonetheless, the metallicities better reflect [Fe/H] than total [ Z /H]. We also find that the star formation timescales inferred from elemental abundances are significantly shorter than those from Prospector , and we discuss the resulting implications for the early formation of massive galaxies.
ISSN:1538-4357

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