Carbon and Iron Deficiencies in Quiescent Galaxies at z=1-3 from JWST-SUSPENSE: Implications for the Formation Histories of Massive Galaxies
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arXiv
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| Natura: | Preprint |
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2024
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| author | Beverage, Aliza G. Slob, Martje Kriek, Mariska Conroy, Charlie Barro, Guillermo Bezanson, Rachel Brammer, Gabriel Cheng, Chloe M. de Graaff, Anna Schreiber, Natascha M. Förster Franx, Marijn Lorenz, Brian Piña, Pavel E. Mancera Marchesini, Danilo Muzzin, Adam Newman, Andrew B. Price, Sedona H. Shapley, Alice E. Stefanon, Mauro Suess, Katherine A. van Dokkum, Pieter Weinberg, David Weisz, Daniel R. |
| author_facet | Beverage, Aliza G. Slob, Martje Kriek, Mariska Conroy, Charlie Barro, Guillermo Bezanson, Rachel Brammer, Gabriel Cheng, Chloe M. de Graaff, Anna Schreiber, Natascha M. Förster Franx, Marijn Lorenz, Brian Piña, Pavel E. Mancera Marchesini, Danilo Muzzin, Adam Newman, Andrew B. Price, Sedona H. Shapley, Alice E. Stefanon, Mauro Suess, Katherine A. van Dokkum, Pieter Weinberg, David Weisz, Daniel R. |
| contents | We present the stellar metallicities and multi-element abundances (C, Mg, Si, Ca, Ti, Cr, and Fe) of 15 massive (log $M/M_\odot=10.2-11.2$) 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$\pm0.04$ dex in [C/H], 0.16$\pm0.03$ dex in [Fe/H], and 0.07$\pm0.04$ 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 non-parametric star-formation histories (using Prospector). Our 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 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2407_02556 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Carbon and Iron Deficiencies in Quiescent Galaxies at z=1-3 from JWST-SUSPENSE: Implications for the Formation Histories of Massive Galaxies Beverage, Aliza G. Slob, Martje Kriek, Mariska Conroy, Charlie Barro, Guillermo Bezanson, Rachel Brammer, Gabriel Cheng, Chloe M. de Graaff, Anna Schreiber, Natascha M. Förster Franx, Marijn Lorenz, Brian Piña, Pavel E. Mancera Marchesini, Danilo Muzzin, Adam Newman, Andrew B. Price, Sedona H. Shapley, Alice E. Stefanon, Mauro Suess, Katherine A. van Dokkum, Pieter Weinberg, David Weisz, Daniel R. Astrophysics of Galaxies We present the stellar metallicities and multi-element abundances (C, Mg, Si, Ca, Ti, Cr, and Fe) of 15 massive (log $M/M_\odot=10.2-11.2$) 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$\pm0.04$ dex in [C/H], 0.16$\pm0.03$ dex in [Fe/H], and 0.07$\pm0.04$ 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 non-parametric star-formation histories (using Prospector). Our 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 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. |
| title | Carbon and Iron Deficiencies in Quiescent Galaxies at z=1-3 from JWST-SUSPENSE: Implications for the Formation Histories of Massive Galaxies |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2407.02556 |