The Variability of Persistent Radio Sources of Fast Radio Bursts
Over 700 bright millisecond-duration radio transients, known as fast radio bursts (FRBs), have been identified to date. Nevertheless, the origin of FRBs remains unknown. Two repeating FRBs (FRB 20121102A and FRB 20190520B) have been verified to be associated with persistent radio sources (PRSs), mak...
Saved in:
| Main Authors: | , , , , , , , , , , , , , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2024-01-01
|
| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/ad7d02 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1846162644298366976 |
|---|---|
| author | Ai Yuan Yang Yi Feng Chao-Wei Tsai Di Li Hui Shi Pei Wang Yuan-Pei Yang Yong-Kun Zhang Chen-Hui Niu Ju-Mei Yao Yu-Zhu Cui Ren-Zhi Su Xiao-Feng Li Jun-Shuo Zhang Yu-Hao Zhu W. D. Cotton |
| author_facet | Ai Yuan Yang Yi Feng Chao-Wei Tsai Di Li Hui Shi Pei Wang Yuan-Pei Yang Yong-Kun Zhang Chen-Hui Niu Ju-Mei Yao Yu-Zhu Cui Ren-Zhi Su Xiao-Feng Li Jun-Shuo Zhang Yu-Hao Zhu W. D. Cotton |
| author_sort | Ai Yuan Yang |
| collection | DOAJ |
| description | Over 700 bright millisecond-duration radio transients, known as fast radio bursts (FRBs), have been identified to date. Nevertheless, the origin of FRBs remains unknown. Two repeating FRBs (FRB 20121102A and FRB 20190520B) have been verified to be associated with persistent radio sources (PRSs), making them the best candidates to study the nature of FRBs. Monitoring the variability in PRSs is essential for understanding their physical nature. We conducted 22 observations of the PRSs linked to FRB 20121102A and FRB 20190520B using the Karl G. Jansky Very Large Array, to study their variability. We have observed significant flux variability for the PRSs of FRB 20121102A and FRB 20190520B, with a confidence level exceeding 99.99%, based on the observations covering the longest timescale recorded to date. The observed variability of the two PRSs exhibits no significant difference in amplitude across both short and long timescales. We found that the radio-derived star formation rates of the two FRB hosts are significantly higher than those measured by the optical H _α emissions, indicating that their host galaxies are highly obscured or most radio emissions are not from star formation processes. The observed timescale of PRS flux evolution constrained the magnetic field of FRB 20121102A with B _∥ ≳ 1 mG and FRB 20190520B with B _∥ ≳ 0.1 mG. |
| format | Article |
| id | doaj-art-c57477b67ebb4356afcccbf4d2277c34 |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-c57477b67ebb4356afcccbf4d2277c342024-11-20T05:49:07ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01976216510.3847/1538-4357/ad7d02The Variability of Persistent Radio Sources of Fast Radio BurstsAi Yuan Yang0https://orcid.org/0000-0003-4546-2623Yi Feng1https://orcid.org/0000-0002-0475-7479Chao-Wei Tsai2https://orcid.org/0000-0002-9390-9672Di Li3https://orcid.org/0000-0003-3010-7661Hui Shi4Pei Wang5https://orcid.org/0000-0002-3386-7159Yuan-Pei Yang6https://orcid.org/0000-0001-6374-8313Yong-Kun Zhang7https://orcid.org/0000-0002-8744-3546Chen-Hui Niu8https://orcid.org/0000-0001-6651-7799Ju-Mei Yao9https://orcid.org/0000-0002-4997-045XYu-Zhu Cui10Ren-Zhi Su11Xiao-Feng Li12https://orcid.org/0000-0002-9093-6296Jun-Shuo Zhang13Yu-Hao Zhu14W. D. Cotton15National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; dili@nao.cas.cn, cwtsai@nao.cas.cn; Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of ChinaResearch Center for Astronomical Computing, Zhejiang Laboratory , Hangzhou 311100, People's Republic of China ; yifeng@zhejianglab.com; Institute for Astronomy, School of Physics, Zhejiang University , Hangzhou 310027, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; dili@nao.cas.cn, cwtsai@nao.cas.cn; Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; dili@nao.cas.cn, cwtsai@nao.cas.cn; Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China; Department of Astronomy, Tsinghua Univerisity , 30 Shuangqing Road, Beijing 100084, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; dili@nao.cas.cn, cwtsai@nao.cas.cn; Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; dili@nao.cas.cn, cwtsai@nao.cas.cn; Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People's Republic of ChinaSouth-Western Institute for Astronomy Research, Yunnan University , Kunming 650504, People's Republic of China; Purple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; dili@nao.cas.cn, cwtsai@nao.cas.cnInstitute of Astrophysics, Central China Normal University , Wuhan 430079, Hubei, People's Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People's Republic of ChinaResearch Center for Astronomical Computing, Zhejiang Laboratory , Hangzhou 311100, People's Republic of China ; yifeng@zhejianglab.comResearch Center for Astronomical Computing, Zhejiang Laboratory , Hangzhou 311100, People's Republic of China ; yifeng@zhejianglab.comChangzhou Institute of Technology , 666 Liaohe Road, Changzhou 213002, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; dili@nao.cas.cn, cwtsai@nao.cas.cnNational Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; dili@nao.cas.cn, cwtsai@nao.cas.cn; University of Chinese Academy of Sciences , Beijing 100049, People's Republic of ChinaNational Radio Astronomy Observatory , 520 Edgemont Road, Charlottesville, VA 22903, USAOver 700 bright millisecond-duration radio transients, known as fast radio bursts (FRBs), have been identified to date. Nevertheless, the origin of FRBs remains unknown. Two repeating FRBs (FRB 20121102A and FRB 20190520B) have been verified to be associated with persistent radio sources (PRSs), making them the best candidates to study the nature of FRBs. Monitoring the variability in PRSs is essential for understanding their physical nature. We conducted 22 observations of the PRSs linked to FRB 20121102A and FRB 20190520B using the Karl G. Jansky Very Large Array, to study their variability. We have observed significant flux variability for the PRSs of FRB 20121102A and FRB 20190520B, with a confidence level exceeding 99.99%, based on the observations covering the longest timescale recorded to date. The observed variability of the two PRSs exhibits no significant difference in amplitude across both short and long timescales. We found that the radio-derived star formation rates of the two FRB hosts are significantly higher than those measured by the optical H _α emissions, indicating that their host galaxies are highly obscured or most radio emissions are not from star formation processes. The observed timescale of PRS flux evolution constrained the magnetic field of FRB 20121102A with B _∥ ≳ 1 mG and FRB 20190520B with B _∥ ≳ 0.1 mG.https://doi.org/10.3847/1538-4357/ad7d02Radio transient sourcesBurst astrophysicsRadio interferometryRadio continuum emissionExtragalactic radio sources |
| spellingShingle | Ai Yuan Yang Yi Feng Chao-Wei Tsai Di Li Hui Shi Pei Wang Yuan-Pei Yang Yong-Kun Zhang Chen-Hui Niu Ju-Mei Yao Yu-Zhu Cui Ren-Zhi Su Xiao-Feng Li Jun-Shuo Zhang Yu-Hao Zhu W. D. Cotton The Variability of Persistent Radio Sources of Fast Radio Bursts The Astrophysical Journal Radio transient sources Burst astrophysics Radio interferometry Radio continuum emission Extragalactic radio sources |
| title | The Variability of Persistent Radio Sources of Fast Radio Bursts |
| title_full | The Variability of Persistent Radio Sources of Fast Radio Bursts |
| title_fullStr | The Variability of Persistent Radio Sources of Fast Radio Bursts |
| title_full_unstemmed | The Variability of Persistent Radio Sources of Fast Radio Bursts |
| title_short | The Variability of Persistent Radio Sources of Fast Radio Bursts |
| title_sort | variability of persistent radio sources of fast radio bursts |
| topic | Radio transient sources Burst astrophysics Radio interferometry Radio continuum emission Extragalactic radio sources |
| url | https://doi.org/10.3847/1538-4357/ad7d02 |
| work_keys_str_mv | AT aiyuanyang thevariabilityofpersistentradiosourcesoffastradiobursts AT yifeng thevariabilityofpersistentradiosourcesoffastradiobursts AT chaoweitsai thevariabilityofpersistentradiosourcesoffastradiobursts AT dili thevariabilityofpersistentradiosourcesoffastradiobursts AT huishi thevariabilityofpersistentradiosourcesoffastradiobursts AT peiwang thevariabilityofpersistentradiosourcesoffastradiobursts AT yuanpeiyang thevariabilityofpersistentradiosourcesoffastradiobursts AT yongkunzhang thevariabilityofpersistentradiosourcesoffastradiobursts AT chenhuiniu thevariabilityofpersistentradiosourcesoffastradiobursts AT jumeiyao thevariabilityofpersistentradiosourcesoffastradiobursts AT yuzhucui thevariabilityofpersistentradiosourcesoffastradiobursts AT renzhisu thevariabilityofpersistentradiosourcesoffastradiobursts AT xiaofengli thevariabilityofpersistentradiosourcesoffastradiobursts AT junshuozhang thevariabilityofpersistentradiosourcesoffastradiobursts AT yuhaozhu thevariabilityofpersistentradiosourcesoffastradiobursts AT wdcotton thevariabilityofpersistentradiosourcesoffastradiobursts AT aiyuanyang variabilityofpersistentradiosourcesoffastradiobursts AT yifeng variabilityofpersistentradiosourcesoffastradiobursts AT chaoweitsai variabilityofpersistentradiosourcesoffastradiobursts AT dili variabilityofpersistentradiosourcesoffastradiobursts AT huishi variabilityofpersistentradiosourcesoffastradiobursts AT peiwang variabilityofpersistentradiosourcesoffastradiobursts AT yuanpeiyang variabilityofpersistentradiosourcesoffastradiobursts AT yongkunzhang variabilityofpersistentradiosourcesoffastradiobursts AT chenhuiniu variabilityofpersistentradiosourcesoffastradiobursts AT jumeiyao variabilityofpersistentradiosourcesoffastradiobursts AT yuzhucui variabilityofpersistentradiosourcesoffastradiobursts AT renzhisu variabilityofpersistentradiosourcesoffastradiobursts AT xiaofengli variabilityofpersistentradiosourcesoffastradiobursts AT junshuozhang variabilityofpersistentradiosourcesoffastradiobursts AT yuhaozhu variabilityofpersistentradiosourcesoffastradiobursts AT wdcotton variabilityofpersistentradiosourcesoffastradiobursts |