Journal Article

Multiwavelength Observations of the Apparently Nonrepeating FRB 20250316A

Li, Dong-Yue, Liu, Hua-Qiu, Sun, Chun, Hu, Jing-Wei, Xin, Li-Ping, Huang, Yu-Xiang, Han, Da-Wei, Hu, Lei, Zhang, Juan, Friedrich, Peter, Liang, Yi-Fang, Cai, Zhi-Ming, Liang, Ming, Zhang, Yong-He, Yao, Da-Zhi, Tao, Lian, Chen, Yong, Yao, Zhu-Heng, Yuan, Weimin, Zheng, Xian-Zhong, Zuo, Ying-Xi, Sun, Tian-Rui, Zhu, Yu-Hao, Zhang, Bing, Zhang, Wen-Da, Wu, Xue-Feng, Rau, Arne, Wan, Zhen, Li, Ye, Feng, Hua, Liu, Yuan, Xu, Yun-Fei, Shu, Xin-Wen, Li, Cheng-Kui, Zhang, Mo, Zhang, Xiao-Ling, Wang, Yi-Han, Hua, Yan-Long, Geng, Jin-Jun, Niu, Jia-Rui, An, Tao, Yang, Xuan, Cheng, Hua-Qing, Xue, Yongquan, Zhang, Song-Bo, Burwitz, Vadim, Wang, Hai-Ren, Sun, Hui, Cao, Jin-Huang, Jiang, Peng, Qian, Lei, Jin, Chi-Chuan, Yao, Yuhan, Jiang, Ji-An, Liu, Hao, Wang, Jian, Liu, He-Yang, Zhu, Wei-Wei, Rea, Nanda, Li, Feng, Jia, Shu-Mei, Wang, Jing, Meidinger, Norbert, Zhang, Jia-Heng, Zhao, Xiao-Fan, Wei, Jian-Yan, Li, Bin, Zhang, Hong-Fei, Zhao, Wen, Pan, Zhi-Chen, Zhang, Yong-Kun, Pan, Hai-Wu, Tang, Jin-Long, Cui, Wei-Wei, Sun, Sheng-Li

2025

Overview

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 ∼1039 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.

• Publisher: IOP Publishing
• Subject: Afterglows / Angular resolution / Emission / Energy distribution / Galaxies / Magnetars / Radio bursts / Radio telescopes / Space telescopes / Telescopes / X ray sources / X ray telescopes / X-ray astronomy / X-ray bursts / X-ray emissions / X-rays