Multiwavelength Observations of the Apparently Non-repeating FRB 20250316A
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2025
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| author | Li, Ye Sun, Hui Qian, Lei Li, Dong-Yue Hua, Yan-Long Xin, Li-Ping Li, Cheng-Kui Wang, Yi-Han Niu, Jia-Rui Sun, Tian-Rui Yao, Zhu-Heng Geng, Jin-Jun Jin, Chi-Chuan Rea, Nanda Liu, Yuan Pan, Zhi-Chen An, Tao Burwitz, Vadim Cai, Zhi-Ming Cao, Jin-Huang Chen, Yong Cheng, Hua-Qing Cui, Wei-Wei Feng, Hua Friedrich, Peter Han, Da-Wei Hu, Jing-Wei Hu, Lei Huang, Yu-Xiang Jia, Shu-Mei Jiang, Ji-An Li, Bin Li, Feng Liang, Ming Liang, Yi-Fang Liu, Hao Liu, He-Yang Liu, Hua-Qiu Meidinger, Norbert Pan, Hai-Wu Rau, Arne Shu, Xin-Wen Sun, Chun Tao, Lian Tang, Jin-Long Wan, Zhen Wang, Hai-Ren Wang, Jian Wang, Jing Xu, Yun-Fei Xue, Yong-Quan Yang, Xuan Yao, Da-Zhi Yao, Yu-Han Zhao, Wen Zhao, Xiao-Fan Zhang, Hong-Fei Zhang, Jia-Heng Zhang, Juan Zhang, Mo Zhang, Song-Bo Zhang, Wen-Da Zhang, Xiao-Ling Zhang, Yong-He Zhang, Yong-Kun Zheng, Xian-Zhong Zhu, Yu-Hao Zuo, Ying-Xi Sun, Sheng-Li Wei, Jian-Yan Zhu, Wei-Wei Jiang, Peng Yuan, Weimin Wu, Xue-Feng Zhang, Bing |
| author_facet | Li, Ye Sun, Hui Qian, Lei Li, Dong-Yue Hua, Yan-Long Xin, Li-Ping Li, Cheng-Kui Wang, Yi-Han Niu, Jia-Rui Sun, Tian-Rui Yao, Zhu-Heng Geng, Jin-Jun Jin, Chi-Chuan Rea, Nanda Liu, Yuan Pan, Zhi-Chen An, Tao Burwitz, Vadim Cai, Zhi-Ming Cao, Jin-Huang Chen, Yong Cheng, Hua-Qing Cui, Wei-Wei Feng, Hua Friedrich, Peter Han, Da-Wei Hu, Jing-Wei Hu, Lei Huang, Yu-Xiang Jia, Shu-Mei Jiang, Ji-An Li, Bin Li, Feng Liang, Ming Liang, Yi-Fang Liu, Hao Liu, He-Yang Liu, Hua-Qiu Meidinger, Norbert Pan, Hai-Wu Rau, Arne Shu, Xin-Wen Sun, Chun Tao, Lian Tang, Jin-Long Wan, Zhen Wang, Hai-Ren Wang, Jian Wang, Jing Xu, Yun-Fei Xue, Yong-Quan Yang, Xuan Yao, Da-Zhi Yao, Yu-Han Zhao, Wen Zhao, Xiao-Fan Zhang, Hong-Fei Zhang, Jia-Heng Zhang, Juan Zhang, Mo Zhang, Song-Bo Zhang, Wen-Da Zhang, Xiao-Ling Zhang, Yong-He Zhang, Yong-Kun Zheng, Xian-Zhong Zhu, Yu-Hao Zuo, Ying-Xi Sun, Sheng-Li Wei, Jian-Yan Zhu, Wei-Wei Jiang, Peng Yuan, Weimin Wu, Xue-Feng Zhang, Bing |
| contents | The physical origin of fast radio bursts (FRBs) remains uncertain. Although multiwavelength observations have been widely conducted, only Galactic FRB~20200428D is associated with an X-ray burst from the magnetar SGR J1935+2154. Here, we present multiwavelength follow-up observations of the nearby bright FRB~20250316A, including the Five-hundred-meter Aperture Spherical radio Telescope (FAST), Einstein Probe (EP) X-ray mission, Chandra X-ray Observatory, Wide Field Survey Telescope (WFST) and Space Variable Object Monitor/Visible Telescope (SVOM/VT). The 13.08-hour FAST follow-up campaign without pulse detection requires an energy distribution flatter than those of well-known repeating FRBs, suggesting that this burst is likely a one-off event. A prompt EP follow-up and multi-epoch observational campaign totaling $>$ 100 ks led to the detection of an X-ray source within the angular resolution of its Follow-up X-ray Telescope (FXT, $10^{\prime\prime}$). A subsequent Chandra observation revealed this source to be offset by $7^{\prime\prime}$ from the FRB position, and established a 0.5-10 keV flux upper limit of $7.6\times 10^{-15}$ $\rm erg\,cm^{-2}\,s^{-1}$ at the FRB position, corresponding to $\sim 10^{39}$ $\rm erg\,s^{-1}$ at the 40 Mpc distance of the host galaxy NGC~4141. These results set one of the most stringent limits on X-ray emission from a non-repeating FRB, disfavoring ultra-luminous X-ray sources (ULXs) as counterparts of apparently one-off FRBs and offering critical insights into afterglow models. Our study suggests that an arcsecond localization of both the FRB and its potential X-ray counterpart is essential for exploring the X-ray counterpart of an FRB. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_13999 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Multiwavelength Observations of the Apparently Non-repeating FRB 20250316A Li, Ye Sun, Hui Qian, Lei Li, Dong-Yue Hua, Yan-Long Xin, Li-Ping Li, Cheng-Kui Wang, Yi-Han Niu, Jia-Rui Sun, Tian-Rui Yao, Zhu-Heng Geng, Jin-Jun Jin, Chi-Chuan Rea, Nanda Liu, Yuan Pan, Zhi-Chen An, Tao Burwitz, Vadim Cai, Zhi-Ming Cao, Jin-Huang Chen, Yong Cheng, Hua-Qing Cui, Wei-Wei Feng, Hua Friedrich, Peter Han, Da-Wei Hu, Jing-Wei Hu, Lei Huang, Yu-Xiang Jia, Shu-Mei Jiang, Ji-An Li, Bin Li, Feng Liang, Ming Liang, Yi-Fang Liu, Hao Liu, He-Yang Liu, Hua-Qiu Meidinger, Norbert Pan, Hai-Wu Rau, Arne Shu, Xin-Wen Sun, Chun Tao, Lian Tang, Jin-Long Wan, Zhen Wang, Hai-Ren Wang, Jian Wang, Jing Xu, Yun-Fei Xue, Yong-Quan Yang, Xuan Yao, Da-Zhi Yao, Yu-Han Zhao, Wen Zhao, Xiao-Fan Zhang, Hong-Fei Zhang, Jia-Heng Zhang, Juan Zhang, Mo Zhang, Song-Bo Zhang, Wen-Da Zhang, Xiao-Ling Zhang, Yong-He Zhang, Yong-Kun Zheng, Xian-Zhong Zhu, Yu-Hao Zuo, Ying-Xi Sun, Sheng-Li Wei, Jian-Yan Zhu, Wei-Wei Jiang, Peng Yuan, Weimin Wu, Xue-Feng Zhang, Bing High Energy Astrophysical Phenomena The physical origin of fast radio bursts (FRBs) remains uncertain. Although multiwavelength observations have been widely conducted, only Galactic FRB~20200428D is associated with an X-ray burst from the magnetar SGR J1935+2154. Here, we present multiwavelength follow-up observations of the nearby bright FRB~20250316A, including the Five-hundred-meter Aperture Spherical radio Telescope (FAST), Einstein Probe (EP) X-ray mission, Chandra X-ray Observatory, Wide Field Survey Telescope (WFST) and Space Variable Object Monitor/Visible Telescope (SVOM/VT). The 13.08-hour FAST follow-up campaign without pulse detection requires an energy distribution flatter than those of well-known repeating FRBs, suggesting that this burst is likely a one-off event. A prompt EP follow-up and multi-epoch observational campaign totaling $>$ 100 ks led to the detection of an X-ray source within the angular resolution of its Follow-up X-ray Telescope (FXT, $10^{\prime\prime}$). A subsequent Chandra observation revealed this source to be offset by $7^{\prime\prime}$ from the FRB position, and established a 0.5-10 keV flux upper limit of $7.6\times 10^{-15}$ $\rm erg\,cm^{-2}\,s^{-1}$ at the FRB position, corresponding to $\sim 10^{39}$ $\rm erg\,s^{-1}$ at the 40 Mpc distance of the host galaxy NGC~4141. These results set one of the most stringent limits on X-ray emission from a non-repeating FRB, disfavoring ultra-luminous X-ray sources (ULXs) as counterparts of apparently one-off FRBs and offering critical insights into afterglow models. Our study suggests that an arcsecond localization of both the FRB and its potential X-ray counterpart is essential for exploring the X-ray counterpart of an FRB. |
| title | Multiwavelength Observations of the Apparently Non-repeating FRB 20250316A |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2508.13999 |