The Circumgalactic Medium Traced by Mg ii Absorption with DESI: Dependence on Galaxy Stellar Mass, Star Formation Rate, and Azimuthal Angle
Understanding the circumgalactic medium (CGM) distribution of galaxies is the key to revealing the dynamical exchange of materials between galaxies and their surroundings. In this work, we use the DESI Early Data Release data set to investigate the cool CGM of galaxies (0.3 < z < 1.7) by sta...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ada942 |
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| author | Zeyu Chen Enci Wang Hu Zou Siwei Zou Yang Gao Huiyuan Wang Haoran Yu Cheng Jia Haixin Li Chengyu Ma Yao Yao Weiyu Ding Runyu Zhu |
| author_facet | Zeyu Chen Enci Wang Hu Zou Siwei Zou Yang Gao Huiyuan Wang Haoran Yu Cheng Jia Haixin Li Chengyu Ma Yao Yao Weiyu Ding Runyu Zhu |
| author_sort | Zeyu Chen |
| collection | DOAJ |
| description | Understanding the circumgalactic medium (CGM) distribution of galaxies is the key to revealing the dynamical exchange of materials between galaxies and their surroundings. In this work, we use the DESI Early Data Release data set to investigate the cool CGM of galaxies (0.3 < z < 1.7) by stacking the spectra of background quasi-stellar objects to obtain the Mg ii absorption of foreground galaxies. The equivalent width of Mg ii absorption strongly correlates with stellar mass, with EW(Mg ii ) $\propto {M}_{* }^{0.5}$ for star-forming galaxies with $\mathrm{log}{M}_{* }/{M}_{\odot }\lt 10$ , but is independent of mass for galaxies above this mass. At a given stellar mass, EW(Mg ii ) is larger for galaxies of higher star formation rate with an impact parameter less than 50 kpc, while showing little dependence on galaxy size. By studying the dependence on azimuthal angle, we find EW(Mg ii ) is strongest at the direction near the minor axis for star-forming galaxies with $\mathrm{log}{M}_{* }/{M}_{\odot }\lt 10.0$ , while no dependence on azimuthal angle is seen for luminous red galaxies. This indicates that the outflow associated with star formation enhances the Mg ii absorption. However, for galaxies with $\mathrm{log}{M}_{* }/{M}_{\odot }\gt 10.0$ , the EW(Mg ii ) at the minor axis is largely suppressed with respect to low-mass galaxies. This suggests that the competing processes, such as stellar feedback and gravity, play a key role in shaping the distribution of outflowing gas. |
| format | Article |
| id | doaj-art-e49d6535ae6e4610b7193786c0e02c62 |
| institution | DOAJ |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-e49d6535ae6e4610b7193786c0e02c622025-08-20T02:54:54ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198118110.3847/1538-4357/ada942The Circumgalactic Medium Traced by Mg ii Absorption with DESI: Dependence on Galaxy Stellar Mass, Star Formation Rate, and Azimuthal AngleZeyu Chen0https://orcid.org/0009-0004-5989-6005Enci Wang1https://orcid.org/0000-0003-1588-9394Hu Zou2https://orcid.org/0000-0002-6684-3997Siwei Zou3https://orcid.org/0000-0002-3983-6484Yang Gao4https://orcid.org/0000-0002-2851-886XHuiyuan Wang5https://orcid.org/0000-0002-4911-6990Haoran Yu6https://orcid.org/0009-0008-1319-498XCheng Jia7https://orcid.org/0009-0004-7042-4172Haixin Li8https://orcid.org/0009-0009-2660-1764Chengyu Ma9https://orcid.org/0009-0006-7343-8013Yao Yao10https://orcid.org/0000-0002-6873-8779Weiyu Ding11https://orcid.org/0000-0003-0230-4596Runyu Zhu12https://orcid.org/0000-0002-8037-3573Department of Astronomy, University of Science and Technology of China , Hefei 230026, People’s Republic of China ; czy664@mail.ustc.edu.cn, ecwang16@ustc.edu.cn; School of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of ChinaDepartment of Astronomy, University of Science and Technology of China , Hefei 230026, People’s Republic of China ; czy664@mail.ustc.edu.cn, ecwang16@ustc.edu.cn; School of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , Beijing 100012, People’s Republic of ChinaChinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories , CAS, Beijing 100101, People’s Republic of China; Department of Astronomy, Tsinghua University , Beijing 100084, People’s Republic of ChinaCollege of Physics and Electronic Information, Dezhou University , Dezhou 253023, People’s Republic of ChinaDepartment of Astronomy, University of Science and Technology of China , Hefei 230026, People’s Republic of China ; czy664@mail.ustc.edu.cn, ecwang16@ustc.edu.cn; School of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of ChinaDepartment of Astronomy, University of Science and Technology of China , Hefei 230026, People’s Republic of China ; czy664@mail.ustc.edu.cn, ecwang16@ustc.edu.cn; School of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of ChinaDepartment of Astronomy, University of Science and Technology of China , Hefei 230026, People’s Republic of China ; czy664@mail.ustc.edu.cn, ecwang16@ustc.edu.cn; School of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of ChinaDepartment of Astronomy, University of Science and Technology of China , Hefei 230026, People’s Republic of China ; czy664@mail.ustc.edu.cn, ecwang16@ustc.edu.cn; School of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of ChinaDepartment of Astronomy, University of Science and Technology of China , Hefei 230026, People’s Republic of China ; czy664@mail.ustc.edu.cn, ecwang16@ustc.edu.cn; School of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of ChinaDepartment of Astronomy, University of Science and Technology of China , Hefei 230026, People’s Republic of China ; czy664@mail.ustc.edu.cn, ecwang16@ustc.edu.cn; School of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of ChinaDepartment of Astronomy, University of Science and Technology of China , Hefei 230026, People’s Republic of China ; czy664@mail.ustc.edu.cn, ecwang16@ustc.edu.cn; School of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of China; National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100012, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , Beijing 100012, People’s Republic of China; Department of Astronomy, Xiamen University , Xiamen, Fujian 361005, People’s Republic of ChinaUnderstanding the circumgalactic medium (CGM) distribution of galaxies is the key to revealing the dynamical exchange of materials between galaxies and their surroundings. In this work, we use the DESI Early Data Release data set to investigate the cool CGM of galaxies (0.3 < z < 1.7) by stacking the spectra of background quasi-stellar objects to obtain the Mg ii absorption of foreground galaxies. The equivalent width of Mg ii absorption strongly correlates with stellar mass, with EW(Mg ii ) $\propto {M}_{* }^{0.5}$ for star-forming galaxies with $\mathrm{log}{M}_{* }/{M}_{\odot }\lt 10$ , but is independent of mass for galaxies above this mass. At a given stellar mass, EW(Mg ii ) is larger for galaxies of higher star formation rate with an impact parameter less than 50 kpc, while showing little dependence on galaxy size. By studying the dependence on azimuthal angle, we find EW(Mg ii ) is strongest at the direction near the minor axis for star-forming galaxies with $\mathrm{log}{M}_{* }/{M}_{\odot }\lt 10.0$ , while no dependence on azimuthal angle is seen for luminous red galaxies. This indicates that the outflow associated with star formation enhances the Mg ii absorption. However, for galaxies with $\mathrm{log}{M}_{* }/{M}_{\odot }\gt 10.0$ , the EW(Mg ii ) at the minor axis is largely suppressed with respect to low-mass galaxies. This suggests that the competing processes, such as stellar feedback and gravity, play a key role in shaping the distribution of outflowing gas.https://doi.org/10.3847/1538-4357/ada942Quasar absorption line spectroscopyCircumgalactic medium |
| spellingShingle | Zeyu Chen Enci Wang Hu Zou Siwei Zou Yang Gao Huiyuan Wang Haoran Yu Cheng Jia Haixin Li Chengyu Ma Yao Yao Weiyu Ding Runyu Zhu The Circumgalactic Medium Traced by Mg ii Absorption with DESI: Dependence on Galaxy Stellar Mass, Star Formation Rate, and Azimuthal Angle The Astrophysical Journal Quasar absorption line spectroscopy Circumgalactic medium |
| title | The Circumgalactic Medium Traced by Mg ii Absorption with DESI: Dependence on Galaxy Stellar Mass, Star Formation Rate, and Azimuthal Angle |
| title_full | The Circumgalactic Medium Traced by Mg ii Absorption with DESI: Dependence on Galaxy Stellar Mass, Star Formation Rate, and Azimuthal Angle |
| title_fullStr | The Circumgalactic Medium Traced by Mg ii Absorption with DESI: Dependence on Galaxy Stellar Mass, Star Formation Rate, and Azimuthal Angle |
| title_full_unstemmed | The Circumgalactic Medium Traced by Mg ii Absorption with DESI: Dependence on Galaxy Stellar Mass, Star Formation Rate, and Azimuthal Angle |
| title_short | The Circumgalactic Medium Traced by Mg ii Absorption with DESI: Dependence on Galaxy Stellar Mass, Star Formation Rate, and Azimuthal Angle |
| title_sort | circumgalactic medium traced by mg ii absorption with desi dependence on galaxy stellar mass star formation rate and azimuthal angle |
| topic | Quasar absorption line spectroscopy Circumgalactic medium |
| url | https://doi.org/10.3847/1538-4357/ada942 |
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