The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster
We report on the optical spectroscopic observations of the host galaxy of the hyperactive repeating fast radio burst (FRB) FRB 20240114A. The host galaxy is a dwarf galaxy at a redshift of z = 0.1306 ± 0.0002. With a rest-frame coverage of 4300–7900 Å, we have detected H α , H β , [O iii ] λλ 4959,...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/2041-8213/adadfd |
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| author | Xiang-Lei Chen Chao-Wei Tsai Di Li Pei Wang Yi Feng Jun-Shuo Zhang Guo-Dong Li Yong-Kun Zhang Lu-Lu Bao Mai Liao Lu-Dan Zhang Pei Zuo Dong-Wei Bao Chen-Hui Niu Rui Luo Wei-Wei Zhu Hu Zou Sui-Jian Xue Bing Zhang |
| author_facet | Xiang-Lei Chen Chao-Wei Tsai Di Li Pei Wang Yi Feng Jun-Shuo Zhang Guo-Dong Li Yong-Kun Zhang Lu-Lu Bao Mai Liao Lu-Dan Zhang Pei Zuo Dong-Wei Bao Chen-Hui Niu Rui Luo Wei-Wei Zhu Hu Zou Sui-Jian Xue Bing Zhang |
| author_sort | Xiang-Lei Chen |
| collection | DOAJ |
| description | We report on the optical spectroscopic observations of the host galaxy of the hyperactive repeating fast radio burst (FRB) FRB 20240114A. The host galaxy is a dwarf galaxy at a redshift of z = 0.1306 ± 0.0002. With a rest-frame coverage of 4300–7900 Å, we have detected H α , H β , [O iii ] λλ 4959,5007, [N ii ] λλ 6548,6583, and [S ii ] λ 6716 emission lines. The emission line ratios suggest that the ionization in the host galaxy is dominated by star formation. The star formation rate (SFR) derived from the H α emission line is (0.06 ± 0.01) M _⊙ yr ^−1 , and the spectral energy distribution fitting suggests the lower limit of the SFR(UV) is 0.09 M _⊙ yr ^−1 . The stellar mass is (4.0 ± 1.8) × 10 ^8 M _⊙ , making the specific SFR ${\rm{log}}\,{\rm{sSFR}}({\rm{H}}\alpha )=-9.17\pm 0.07\,{{\rm{yr}}}^{-1}$ . The line ratios indicate an upper limit of a metallicity of 12 + log _10 ([O/H]) ∼ 8.5. As the nearest dwarf host galaxy with a repeating FRB, the activity of FRB 20240114A and the properties of this host galaxy closely resemble those of FRB 20121102A and FRB 20190520B. The H α -traced dispersion measure provided by the ionized gas of the host galaxy has a moderate contribution of ∼200 pc cm ^−3 , assuming a warm ionized gas. We found that the distributions of the stellar mass versus SFR are significantly different between repeating and one-off FRBs, as determined by the MANOVA test with p = 0.0116. |
| format | Article |
| id | doaj-art-b69b6eb3496e4fa5bddda362f47b4239 |
| institution | DOAJ |
| issn | 2041-8205 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal Letters |
| spelling | doaj-art-b69b6eb3496e4fa5bddda362f47b42392025-08-20T03:12:39ZengIOP PublishingThe Astrophysical Journal Letters2041-82052025-01-019802L2410.3847/2041-8213/adadfdThe Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy ClusterXiang-Lei Chen0https://orcid.org/0000-0001-5738-9625Chao-Wei Tsai1https://orcid.org/0000-0002-9390-9672Di Li2https://orcid.org/0000-0003-3010-7661Pei Wang3https://orcid.org/0000-0002-3386-7159Yi Feng4https://orcid.org/0000-0002-0475-7479Jun-Shuo Zhang5https://orcid.org/0009-0005-8586-3001Guo-Dong Li6https://orcid.org/0000-0003-4007-5771Yong-Kun Zhang7https://orcid.org/0000-0002-8744-3546Lu-Lu Bao8https://orcid.org/0009-0009-6319-0888Mai Liao9https://orcid.org/0000-0002-9137-7019Lu-Dan Zhang10https://orcid.org/0009-0002-3093-0180Pei Zuo11https://orcid.org/0000-0003-3948-9192Dong-Wei Bao12https://orcid.org/0000-0003-2024-1648Chen-Hui Niu13https://orcid.org/0000-0001-6651-7799Rui Luo14https://orcid.org/0000-0002-4300-121XWei-Wei Zhu15https://orcid.org/0000-0001-5105-4058Hu Zou16https://orcid.org/0000-0002-6684-3997Sui-Jian Xue17https://orcid.org/0000-0002-0660-0432Bing Zhang18https://orcid.org/0000-0002-9725-2524National Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cn; Key Laboratory of Radio Astronomy and Technolgoy, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing, 100101, People's Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cn; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cn; Department of Astronomy, Tsinghua University , Beijing 100084, People’s Republic of China ; dili@tsinghua.edu.cnNational Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cn; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of ChinaResearch Center for Astronomical Computing , Zhejiang Laboratory, Hangzhou 311100, People’s Republic of China; Institute for Astronomy, School of Physics, Zhejiang University , Hangzhou 310027, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cn; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cn; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cnUniversity of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cn; Universidad Diego Portales , Av Republica 180, Santiago, Regíón Metropolitana, ChileNational Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cn; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cnNational Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cnInstitute of Astrophysics, Central China Normal University , Wuhan 430079, People’s Republic of ChinaDepartment of Astronomy, School of Physics and Materials Science, Guangzhou University , Guangzhou 510006, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cn; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cnNational Astronomical Observatories , Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, People’s Republic of China ; cwtsai@nao.cas.cnNevada Center for Astrophysics, University of Nevada , Las Vegas, NV 89154, USA; Department of Physics and Astronomy, University of Nevada , Las Vegas, NV 89154, USAWe report on the optical spectroscopic observations of the host galaxy of the hyperactive repeating fast radio burst (FRB) FRB 20240114A. The host galaxy is a dwarf galaxy at a redshift of z = 0.1306 ± 0.0002. With a rest-frame coverage of 4300–7900 Å, we have detected H α , H β , [O iii ] λλ 4959,5007, [N ii ] λλ 6548,6583, and [S ii ] λ 6716 emission lines. The emission line ratios suggest that the ionization in the host galaxy is dominated by star formation. The star formation rate (SFR) derived from the H α emission line is (0.06 ± 0.01) M _⊙ yr ^−1 , and the spectral energy distribution fitting suggests the lower limit of the SFR(UV) is 0.09 M _⊙ yr ^−1 . The stellar mass is (4.0 ± 1.8) × 10 ^8 M _⊙ , making the specific SFR ${\rm{log}}\,{\rm{sSFR}}({\rm{H}}\alpha )=-9.17\pm 0.07\,{{\rm{yr}}}^{-1}$ . The line ratios indicate an upper limit of a metallicity of 12 + log _10 ([O/H]) ∼ 8.5. As the nearest dwarf host galaxy with a repeating FRB, the activity of FRB 20240114A and the properties of this host galaxy closely resemble those of FRB 20121102A and FRB 20190520B. The H α -traced dispersion measure provided by the ionized gas of the host galaxy has a moderate contribution of ∼200 pc cm ^−3 , assuming a warm ionized gas. We found that the distributions of the stellar mass versus SFR are significantly different between repeating and one-off FRBs, as determined by the MANOVA test with p = 0.0116.https://doi.org/10.3847/2041-8213/adadfdRadio transient sourcesDwarf galaxiesStarburst galaxies |
| spellingShingle | Xiang-Lei Chen Chao-Wei Tsai Di Li Pei Wang Yi Feng Jun-Shuo Zhang Guo-Dong Li Yong-Kun Zhang Lu-Lu Bao Mai Liao Lu-Dan Zhang Pei Zuo Dong-Wei Bao Chen-Hui Niu Rui Luo Wei-Wei Zhu Hu Zou Sui-Jian Xue Bing Zhang The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster The Astrophysical Journal Letters Radio transient sources Dwarf galaxies Starburst galaxies |
| title | The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster |
| title_full | The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster |
| title_fullStr | The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster |
| title_full_unstemmed | The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster |
| title_short | The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster |
| title_sort | host galaxy of the hyperactive repeating frb 20240114a behind a galaxy cluster |
| topic | Radio transient sources Dwarf galaxies Starburst galaxies |
| url | https://doi.org/10.3847/2041-8213/adadfd |
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