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On the Stellar Populations of Galaxies at z = 9–11: The Growth of Metals and Stellar Mass at Early Times

by Schneider, Raffaella , Wilkins, Stephen M , Finkelstein, Steven L , Yung, L. Y. Aaron , Hutchison, Taylor A , Larson, Rebecca L , Grogin, Norman A , Ferguson, Henry C , Jung, Intae , Rojas-Ruiz, Sofía , Dickinson, Mark , Giavalisco, Mauro , Graziani, Luca , Tacchella, Sandro , Pirzkal, Norbert , Somerville, Rachel S , Papovich, Casey , Koekemoer, Anton M , Song, Mimi , Hathi, Nimish , Bagley, Micaela

in Attenuation / Dust / Emission / Emission lines / Galaxies / Galaxy distribution / Massive stars / Metallicity / Spectral energy distribution / Star & galaxy formation / Star formation / Stars / Stellar mass / Stellar populations / Wavelengths

2022

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On the Stellar Populations of Galaxies at z = 9–11: The Growth of Metals and Stellar Mass at Early Times

2022

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On the Stellar Populations of Galaxies at z = 9–11: The Growth of Metals and Stellar Mass at Early Times

2022

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Journal Article

On the Stellar Populations of Galaxies at z = 9–11: The Growth of Metals and Stellar Mass at Early Times

Schneider, Raffaella,

Wilkins, Stephen M,

Finkelstein, Steven L,

Yung, L. Y. Aaron,

Hutchison, Taylor A,

Larson, Rebecca L,

Grogin, Norman A,

Ferguson, Henry C,

Jung, Intae,

Rojas-Ruiz, Sofía,

Dickinson, Mark,

Giavalisco, Mauro,

Graziani, Luca,

Tacchella, Sandro,

Pirzkal, Norbert,

Somerville, Rachel S,

Papovich, Casey,

Koekemoer, Anton M,

Song, Mimi,

Hathi, Nimish,

Bagley, Micaela

2022

Overview

We present a detailed stellar population analysis of 11 bright (H < 26.6) galaxies at z = 9–11 (three spectroscopically confirmed) to constrain the chemical enrichment and growth of stellar mass of early galaxies. We use the flexible Bayesian spectral energy distribution (SED) fitting code Prospector with a range of star formation histories (SFHs), a flexible dust attenuation law, and a self-consistent model of emission lines. This approach allows us to assess how different priors affect our results and how well we can break degeneracies between dust attenuation, stellar ages, metallicity, and emission lines using data that probe only the rest-frame ultraviolet (UV) to optical wavelengths. We measure a median observed UV spectral slope β=−1.87−0.43+0.35 for relatively massive star-forming galaxies ( 9 10.

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Publisher

IOP Publishing

Subject

/ Dust

/ Galaxy distribution

/ Massive stars