@article{10902/31514,
year = {2023},
url = {https://hdl.handle.net/10902/31514},
abstract = {A tight positive correlation between the stellar mass and the gas-phase metallicity of galaxies has been observed at low redshifts. The redshift evolution of this correlation can strongly constrain theories of galaxy evolution. The advent of JWST allows probing the mass?metallicity relation at redshifts far beyond what was previously accessible. Here we report the discovery of two emission line galaxies at redshifts 8.15 and 8.16 in JWST NIRCam imaging and NIRSpec spectroscopy of targets gravitationally lensed by the cluster RX J2129.4+0005. We measure their metallicities and stellar masses along with nine additional galaxies at 7.2 < zspec < 9.5 to report the first quantitative statistical inference of the mass?metallicity relation at z ? 8. We measure ?0.9 dex evolution in the normalization of the mass?metallicity relation from z ? 8 to the local universe; at a fixed stellar mass, galaxies are 8 times less metal enriched at z ? 8 compared to the present day. Our inferred normalization is in agreement with the predictions of FIRE simulations. Our inferred slope of the mass?metallicity relation is similar to or slightly shallower than that predicted by FIRE or observed at lower redshifts. We compare the z ? 8 galaxies to extremely low-metallicity analog candidates in the local universe, finding that they are generally distinct from extreme emission line galaxies or "green peas," but are similar in strong emission line ratios and metallicities to "blueberry galaxies." Despite this similarity, at a fixed stellar mass, the z ? 8 galaxies have systematically lower metallicities compared to blueberry galaxies.},
organization = {We thank the anonymous referee whose comments helped improve the robustness of our analysis and conclusions. We thank Gabe Brammer for his identification of the high-redshift galaxy targets we present during the mask design process, and his contributions to their analysis. We also appreciate Program Coordinator Patricia Royle, and Program Scientists Armin Rest, Diane Karakala, and Patrick Ogle for their efforts with short turnaround that made the follow-up observations a success. D.L. and J.H. were supported by a VILLUM FONDEN Investigator grant (project number 16599). P.L.K. is supported by NSF grant AST-1908823 and anticipated funding from JWST DD-2767. A.Z. acknowledges support by Grant No. 2020750 from the United States–Israel Binational Science Foundation (BSF) and grant No. 2109066 from the United States National Science Foundation (NSF), and by the Ministry of Science & Technology, Israel. J.M.D. acknowledges the support of projects PGC2018-101814-B-100 and MDM-2017-0765. A.V.F. is grateful for financial assistance from the Christopher R. Redlich Fund and numerous individual donors. The UCSC team is supported in part by NSF grant AST–1815935, the Gordon & Betty Moore Foundation, and by a fellowship from the David and Lucile Packard Foundation to R.J.F. M.O. acknowledges support by JSPS KAKENHI grants JP20H00181, JP20H05856, JP22H01260, and JP22K21349. I.P.-F. and F.P. acknowledge support from the Spanish State Research Agency (AEI) under grant number PID2019-105552RB-C43. J.P. was supported by the Hubble Space Telescope program GO-16264 through the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. for NASA, under contract NAS5-26555.},
publisher = {Institute of Physics Publishing},
publisher = {Astrophysical Journal, 2023, 957(39)},
title = {Evolution of the Mass-Metallicity Relation from Redshift z ≈ 8 to the Local Universe},
author = {Langeroodi, Danial and Hjorth, Jens and Chen, Wenlei and Kelly, Patrick L. and Williams, Hayley and Lin, Yu-Heng and Scarlata, Claudia and Zitrin, Adi and Broadhurst, Tom and Diego Rodríguez, José María and Huang, Xiaosheng and Filippenko, Alexei V. and Foley, Ryan J. and Jha, Saurabh and Koekemoer, Anton M. and Oguri, Masamune and Perez-Fournon, Ismael and Pierel, Justin and Poidevin, Frederick and Strolger, Lou},
}