Multiwavelength Observations of the Apparently Nonrepeating FRB 20250316A

Abstract 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 Objects Monitor/Visible Telescope (SVOM/VT). The 13.08 hr 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 multiepoch 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″). A subsequent Chandra observation revealed this source to be offset by 7″ from the FRB position and established a 0.5–10 keV flux upper limit of 7.6 × 10 −15 erg cm −2 s −1 at the FRB position, corresponding to ∼10 39 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 nonrepeating FRB, disfavoring ultraluminous X-ray sources 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.

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Journal
The Astrophysical Journal
Published
2025-12-02
DOI
https://doi.org/10.3847/1538-4357/ae1463
Primary Topic
Pulsars and Gravitational Waves Research
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article
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article

Multiwavelength Observations of the Apparently Nonrepeating FRB 20250316A

N. Rea, Juncheng Cao, Yu‐Hao Zhu, S. M. Jia et al.
The Astrophysical Journal
Pulsars and Gravitational Waves Research
article

Multiwavelength Observations of the Apparently Nonrepeating FRB 20250316A

N. Rea, Juncheng Cao, Yu‐Hao Zhu, S. M. Jia, Xianzhong Zheng, Wen Zhao, Jin-Jun Geng, Ji-an Jiang, Tao An, Zhichen Pan, Jiarui Niu, Weiwei Zhu, H.M Liu, Chichuan Jin, Weimin Yuan, Yong Chen, Dongyue Li, Cheng-Kui Li, He‐Yang Liu, Lian Tao, Yunfei Xu, Yongquan Xue, Yuhan Yao, Tianrui Sun, J. L. Zhang, Haiwu Pan, Zhu-Heng Yao, Chunwen Sun, Zhen Wan, Norbert Meidinger, Hui Sun, Huaqing Cheng, A. Rau, Lei Qian, Li-Ping Xin, Xinwen Shu, Lei Hu, Jian‐Yan Wei, Yihan Wang, Yongkun Zhang, Yuxiang Huang, Xiaofan Zhao, Songbo Zhang, V. Burwitz, Xue-Feng Wu, J. Y. Hu, Zhiming Cai, Hua Feng, Ye Li, Jing Wang, Bing Zhang, Juan Zhang, Yong Zhang, Xiaoling Zhang, Wei Cui, Mo Zhang, Wenda Zhang, Hongfei Zhang, Yingxi Zuo, Yuan Liu, Hairen Wang, Peng Jiang, Ming Liang, Xuan Yang, Jian Wang, Jinlong Tang, Feng Li, Bin Li, Dawei Han, Hua Yao, Péter Friedrich, Dazhi Yao, Shengli Sun, Y. F. Liang, Haibo Liu
article en

Abstract

Abstract 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 Objects Monitor/Visible Telescope (SVOM/VT). The 13.08 hr 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 multiepoch 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″). A subsequent Chandra observation revealed this source to be offset by 7″ from the FRB position and established a 0.5–10 keV flux upper limit of 7.6 × 10 −15 erg cm −2 s −1 at the FRB position, corresponding to ∼10 39 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 nonrepeating FRB, disfavoring ultraluminous X-ray sources 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.

The Astrophysical JournalVol. 995(1)
University of Science and Technology of China (CN), Commonwealth Scientific and Industrial Research Organisation (AU), Australia Telescope National Facility (AU), Institute of Space Sciences (ES), University of Nevada, Las Vegas (US), University of Wisconsin–Madison (US), Guizhou University (CN), Chinese Academy of Sciences (CN), National Institutes of Natural Sciences (JP), Beijing Normal University (CN), Shanghai Astronomical Observatory (CN), Yunnan Observatories (CN), Miller College (US), Purple Mountain Observatory (CN), Shanghai Micro Satellite Engineering Center (CN), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), Institute of Optics and Electronics, Chinese Academy of Sciences (CN), Astronomy Australia (AU), Shanghai Institute of Technical Physics (CN), Institute of High Energy Physics (CN), Ministry of Education (TW), NSF NOIRLab (US), Space Engineering University (CN), National Astronomical Observatory of Japan (JP), National Astronomical Observatories (CN), University of Chinese Academy of Sciences (CN), Innovation Academy for Microsatellites of Chinese Academy of Sciences, Anhui Normal University (CN), Carnegie Mellon University (US), University of Hong Kong (HK), University of California, Berkeley (US)
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