The Astrophysical Journal (Jan 2024)
A Large Sample of Extremely Metal-poor Galaxies at z < 1 Identified from the DESI Early Data
- Hu Zou,
- Jipeng Sui,
- Amélie Saintonge,
- Dirk Scholte,
- John Moustakas,
- Malgorzata Siudek,
- Arjun Dey,
- Stephanie Juneau,
- Weijian Guo,
- Rebecca Canning,
- J. Aguilar,
- S. Ahlen,
- D. Brooks,
- T. Claybaugh,
- K. Dawson,
- A. de la Macorra,
- P. Doel,
- J. E. Forero-Romero,
- S. Gontcho A Gontcho,
- K. Honscheid,
- M. Landriau,
- L. Le Guillou,
- M. Manera,
- A. Meisner,
- R. Miquel,
- Jundan Nie,
- C. Poppett,
- M. Rezaie,
- G. Rossi,
- E. Sanchez,
- M. Schubnell,
- H. Seo,
- G. Tarlé,
- Zhimin Zhou,
- Siwei Zou
Affiliations
- Hu Zou
- ORCiD
- Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China [email protected]; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 101408, People's Republic of China
- Jipeng Sui
- Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China [email protected]; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 101408, People's Republic of China
- Amélie Saintonge
- ORCiD
- Department of Physics & Astronomy, University College London , Gower Street, London, WC1E 6BT, UK
- Dirk Scholte
- ORCiD
- Department of Physics & Astronomy, University College London , Gower Street, London, WC1E 6BT, UK
- John Moustakas
- ORCiD
- Department of Physics and Astronomy, Siena College , 515 Loudon Road, Loudonville, NY 12211, USA
- Malgorzata Siudek
- Institute of Space Sciences , ICE-CSIC, Campus UAB, Carrer de Can Magrans s/n, E-08913 Bellaterra, Barcelona, Spain
- Arjun Dey
- NSF’s NOIRLab , 950 N. Cherry Avenue, Tucson, AZ 85719, USA
- Stephanie Juneau
- NSF’s NOIRLab , 950 N. Cherry Avenue, Tucson, AZ 85719, USA
- Weijian Guo
- ORCiD
- Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China [email protected]
- Rebecca Canning
- Institute of Cosmology & Gravitation, University of Portsmouth , Dennis Sciama Building, Portsmouth, PO1 3FX, UK
- J. Aguilar
- Lawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720, USA
- S. Ahlen
- ORCiD
- Physics Dept., Boston University , 590 Commonwealth Avenue, Boston, MA 02215, USA
- D. Brooks
- Department of Physics & Astronomy, University College London , Gower Street, London, WC1E 6BT, UK
- T. Claybaugh
- Lawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720, USA
- K. Dawson
- Department of Physics and Astronomy, The University of Utah , 115 South 1400 East, Salt Lake City, UT 84112, USA
- A. de la Macorra
- ORCiD
- Instituto de Física, Universidad Nacional Autónoma de México , Cd. de México C.P. 04510, México
- P. Doel
- Department of Physics & Astronomy, University College London , Gower Street, London, WC1E 6BT, UK
- J. E. Forero-Romero
- ORCiD
- Observatorio Astronómico, Universidad de los Andes , Cra. 1 No. 18A-10, Edificio H, CP 111711 Bogotá, Colombia
- S. Gontcho A Gontcho
- ORCiD
- Lawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720, USA
- K. Honscheid
- Department of Physics, The Ohio State University , 191 West Woodruff Avenue, Columbus, OH 43210, USA
- M. Landriau
- ORCiD
- Lawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720, USA
- L. Le Guillou
- ORCiD
- Sorbonne Université , CNRS/IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies (LPNHE), F-75005 Paris, France
- M. Manera
- ORCiD
- Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology , Campus UAB, E-08193 Bellaterra, Barcelona, Spain
- A. Meisner
- ORCiD
- NSF’s NOIRLab , 950 N. Cherry Avenue, Tucson, AZ 85719, USA
- R. Miquel
- ORCiD
- Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology , Campus UAB, E-08193 Bellaterra, Barcelona, Spain
- Jundan Nie
- ORCiD
- Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China [email protected]
- C. Poppett
- Space Sciences Laboratory, University of California , Berkeley, 7 Gauss Way, Berkeley, CA 94720, USA
- M. Rezaie
- ORCiD
- Department of Physics, Kansas State University , 116 Cardwell Hall, Manhattan, KS 66506, USA
- G. Rossi
- Department of Physics and Astronomy, Sejong University , Seoul, 143-747, Republic of Korea
- E. Sanchez
- ORCiD
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT) , Madrid, Spain
- M. Schubnell
- Department of Physics & Astronomy, Ohio University , Athens, OH 45701, USA
- H. Seo
- ORCiD
- Department of Physics & Astronomy, Ohio University , Athens, OH 45701, USA
- G. Tarlé
- ORCiD
- University of Michigan , Ann Arbor, MI 48109, USA
- Zhimin Zhou
- ORCiD
- Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China [email protected]
- Siwei Zou
- ORCiD
- Department of Astronomy, Tsinghua University , 30 Shuangqing Road, Haidian District, Beijing, 100190, People's Republic of China
- DOI
- https://doi.org/10.3847/1538-4357/ad1409
- Journal volume & issue
-
Vol. 961,
no. 2
p. 173
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.
Keywords
