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Zou, Hu; Sui, Jipeng; Saintonge, Amélie; Scholte, Dirk; Moustakas, John; Siudek, Malgorzata; Dey, Arjun; Juneau, Stephanie; Guo, Weijian; Canning, Rebecca; Aguilar, J.; Ahlen, S.; Brooks, D.; Claybaugh, T.; Dawson, K.; de la Macorra, A.; Doel, P.; Forero-Romero, J. E.; Gontcho A Gontcho, S.; Honscheid, K.; Landriau, M.; Le Guillou, L.; Manera, M.; Meisner, A.; Miquel, R.; Nie, Jundan; Poppett, C.; Rezaie, M.; Rossi, G.; Sanchez, E.; Schubnell, M.; Seo, H.; Tarlé, G.; Zhou, Zhimin; Zou, Siwei
The Astrophysical journal, 02/2024, Letnik: 961, Številka: 2Journal Article
Abstract Extremely metal-poor galaxies (XMPGs) at relatively low redshift are excellent laboratories for studying galaxy formation and evolution in the early universe. Much effort has been spent on identifying them from large-scale spectroscopic surveys or spectroscopic follow-up observations. Previous work has identified a few hundred XMPGs. In this work, we obtain a large sample of 223 XMPGs at z < 1 from the early data of the Dark Energy Spectroscopic Instrument (DESI). The oxygen abundance is determined using the direct T e method based on the detection of the O iii λ 4363 line. The sample includes 95 confirmed XMPGs based on the oxygen abundance uncertainty; the remaining 128 galaxies are regarded as XMPG candidates. These XMPGs are only 0.01% of the total DESI observed galaxies. Their coordinates and other properties are provided in the paper. The most XMPGs have an oxygen abundance of ∼1/34 Z ⊙ , a stellar mass of about 1.5 × 10 7 M ⊙, and a star formation rate of 0.22 M ⊙ yr −1 . The two most XMPGs present distinct morphologies suggesting different formation mechanisms. The local environmental investigation shows that XMPGs preferentially reside in relatively low-density regions. Many of them fall below the stellar mass–metallicity relations (MZRs) of normal star-forming galaxies. From a comparison of the MZR with theoretical simulations, it appears that XMPGs are good analogs to high-redshift star-forming galaxies. The nature of these XMPG populations will be further investigated in detail with larger and more complete samples from the ongoing DESI survey.
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JCR | SNIP | JCR | SNIP | JCR | SNIP | JCR | SNIP |
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in: SICRIS
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