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dc.contributor.authorCurti, Mirko
dc.contributor.authorMaiolino, Roberto
dc.contributor.authorCurtis-Lake, Emma
dc.contributor.authorChevallard, Jacopo
dc.contributor.authorCarniani, Stefano
dc.contributor.authorD'Eugenio, Francesco
dc.contributor.authorLooser, Tobias J.
dc.contributor.authorScholtz, Jan
dc.contributor.authorCharlot, Stephane
dc.contributor.authorCameron, Alex
dc.contributor.authorÜbler, Hannah
dc.contributor.authorWitstok, Joris
dc.contributor.authorBoyett, Kristian
dc.contributor.authorLaseter, Isaac
dc.contributor.authorSandles, Lester
dc.contributor.authorArribas, Santiago
dc.contributor.authorBunker, Andrew
dc.contributor.authorGiardino, Giovanna
dc.contributor.authorMaseda, Michael V.
dc.contributor.authorRawle, Tim
dc.contributor.authorPino, Bruno Rodríguez Del
dc.contributor.authorSmit, Renske
dc.contributor.authorWillott, Chris J.
dc.contributor.authorEisenstein, Daniel J.
dc.contributor.authorHausen, Ryan
dc.contributor.authorJohnson, Benjamin
dc.contributor.authorRieke, Marcia
dc.contributor.authorRobertson, Brant
dc.contributor.authorTacchella, Sandro
dc.contributor.authorWilliams, Christina C.
dc.contributor.authorWillmer, Christopher
dc.contributor.authorBaker, William M.
dc.contributor.authorBhatawdekar, Rachana
dc.contributor.authorEgami, Eiichi
dc.contributor.authorHelton, Jakob M.
dc.contributor.authorJi, Zhiyuan
dc.contributor.authorKumari, Nimisha
dc.contributor.authorPerna, Michele
dc.contributor.authorShivaei, Irene
dc.contributor.authorSun, Fengwu
dc.date.accessioned2024-10-07T21:30:01Z
dc.date.available2024-10-07T21:30:01Z
dc.date.issued2024-04-10
dc.identifier.citationCurti , M , Maiolino , R , Curtis-Lake , E , Chevallard , J , Carniani , S , D'Eugenio , F , Looser , T J , Scholtz , J , Charlot , S , Cameron , A , Übler , H , Witstok , J , Boyett , K , Laseter , I , Sandles , L , Arribas , S , Bunker , A , Giardino , G , Maseda , M V , Rawle , T , Pino , B R D , Smit , R , Willott , C J , Eisenstein , D J , Hausen , R , Johnson , B , Rieke , M , Robertson , B , Tacchella , S , Williams , C C , Willmer , C , Baker , W M , Bhatawdekar , R , Egami , E , Helton , J M , Ji , Z , Kumari , N , Perna , M , Shivaei , I & Sun , F 2024 , ' JADES: Insights into the low-mass end of the mass–metallicity–SFR relation at 3 <z <10 from deepJWST/NIRSpec spectroscopy ' , Astronomy & Astrophysics , vol. 684 , A75 . https://doi.org/10.1051/0004-6361/202346698
dc.identifier.issn0004-6361
dc.identifier.otherArXiv: http://arxiv.org/abs/2304.08516v2
dc.identifier.otherORCID: /0000-0002-9551-0534/work/169402630
dc.identifier.urihttp://hdl.handle.net/2299/28316
dc.description© The Authors 2024. This is Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
dc.description.abstractWe analysed the gas-phase metallicity properties of a sample of low-stellar-mass (log M⋆/M⊙ ≲ 9) galaxies at 3 < z < 10 observed with JWST/NIRSpec as part of the JADES programme in its deep GOODS-S tier. By combining this sample with more massive galaxies at similar redshifts from other programmes, we study the scaling relations between stellar mass (M⋆), oxygen abundance (O/H), and star-formation rate (SFR) for 146 galaxies spanning three orders of magnitude in stellar mass and out to the epoch of early galaxy assembly. We find evidence for a shallower slope at the low-mass end of the mass–metallicity relation (MZR), with 12+log(O/H) = (7.72 ± 0.02) + (0.17 ± 0.03) log(M⋆/108 M⊙), in good agreement with the MZR probed by local analogues of high-redshift systems, such as the ‘Green Pea’ and ‘Blueberry’ galaxies. The inferred slope is well matched by models including ‘momentum-driven’ supernova (SN) winds, suggesting that feedback mechanisms in dwarf galaxies (and at high z) might be different from those in place at higher masses. The evolution in the normalisation is observed to be relatively mild compared to previous determinations of the MZR at z ∼ 3 (∼0.1 − 0.2 dex across the explored mass regime). We observe a deviation from the local fundamental metallicity relation (FMR) for our sample at high redshift, especially at z > 6, with galaxies significantly less enriched than predicted given their M⋆ and SFR (with a median offset in log(O/H) of ∼0.5 dex, significant at ∼5σ). These observations are consistent with an enhanced stochasticity in the gas accretion and star-formation history of high-redshift systems, prompting us to reconsider the nature of the relationship between M⋆, O/H, and SFR in the early Universe.en
dc.format.extent22
dc.format.extent1602882
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysics
dc.subjectastro-ph.GA
dc.titleJADES: Insights into the low-mass end of the mass–metallicity–SFR relation at 3<z <10 from deepJWST/NIRSpec spectroscopyen
dc.contributor.institutionCentre for Astrophysics Research (CAR)
dc.contributor.institutionDepartment of Physics, Astronomy and Mathematics
dc.contributor.institutionSchool of Physics, Engineering & Computer Science
dc.description.statusPeer reviewed
rioxxterms.versionofrecord10.1051/0004-6361/202346698
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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