Multiwavelength Analysis of GRB 250101A: From Gamma-Ray Prompt Emission to Optical Afterglow
The interaction between the relativistic jet and the circumburst medium produces a multiwavelength afterglow of a gamma-ray burst (GRBs). In this work, we present multiwavelength properties of GRB 250101A based on the observations of Swift, Fermi, and Mephisto. The spectral analysis of Swift/Swift B...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/adea3d |
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| author | Guowang Du Yehao Cheng Yuan-Pei Yang Jun Yang Jinghua Zhang Dan Zhu Yu Pan Yuan Fang Xingzhu Zou Brajesh Kumar Helong Guo Xufeng Zhu Yangwei Zhang Fanchuan Kong Chenxi Shang Xinlei Chen Xiangkun Liu Xiaowei Liu |
| author_facet | Guowang Du Yehao Cheng Yuan-Pei Yang Jun Yang Jinghua Zhang Dan Zhu Yu Pan Yuan Fang Xingzhu Zou Brajesh Kumar Helong Guo Xufeng Zhu Yangwei Zhang Fanchuan Kong Chenxi Shang Xinlei Chen Xiangkun Liu Xiaowei Liu |
| author_sort | Guowang Du |
| collection | DOAJ |
| description | The interaction between the relativistic jet and the circumburst medium produces a multiwavelength afterglow of a gamma-ray burst (GRBs). In this work, we present multiwavelength properties of GRB 250101A based on the observations of Swift, Fermi, and Mephisto. The spectral analysis of Swift/Swift Burst Alert Telescope (BAT) and Fermi/Gamma-ray Burst Monitor (GBM) reveals a soft prompt spectrum with a low-energy photon index of −1.18 and a peak energy of 33 keV, and the isotropic energy is 1.4 × 10 ^52 erg. The prompt emission of GRB 250101A aligns with Type II GRBs in the Amati relation. Meanwhile, our analysis indicates that GRB 250101A is an X-ray-rich or X-ray-dominated GRB, with intrinsic properties suggesting that it is relatively softer than most classical GRBs. Optical observation with Mephisto, beginning 197 s post-trigger, shows a single power-law decay in uvgriz bands, with F _ν _,obs ∝ t ^−0.76 ν ^−1.21 . The observed spectral index significantly exceeds theoretical predictions under standard afterglow models, suggesting a color excess of ∼0.216 mag. However, combining X-ray and optical afterglow, we find that GRB 250101A is more likely a “normal burst” rather than an “optical-dark burst,” and the dust extinction effect plays an important role in the optical blue bands. Furthermore, there is a structural change at T _0 + 2924 s in the optical light curve, indicating a density drop of ∼50% in the interstellar medium at a distance of ∼0.13 pc. Our analysis shows that this GRB clearly shows some unique characteristics in its observed X-ray-rich prompt emission as well as the circumburst environment, implying a special progenitor. |
| format | Article |
| id | doaj-art-cd78e9f7eef44a0784b095e489e09f67 |
| institution | DOAJ |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-cd78e9f7eef44a0784b095e489e09f672025-08-20T02:47:37ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198911910.3847/1538-4357/adea3dMultiwavelength Analysis of GRB 250101A: From Gamma-Ray Prompt Emission to Optical AfterglowGuowang Du0https://orcid.org/0000-0002-8109-7152Yehao Cheng1https://orcid.org/0000-0001-8278-2955Yuan-Pei Yang2https://orcid.org/0000-0001-6374-8313Jun Yang3https://orcid.org/0000-0002-5485-5042Jinghua Zhang4https://orcid.org/0000-0002-2510-6931Dan Zhu5https://orcid.org/0009-0008-5929-6658Yu Pan6https://orcid.org/0009-0002-7625-2653Yuan Fang7https://orcid.org/0009-0006-1010-1325Xingzhu Zou8https://orcid.org/0009-0006-5847-9271Brajesh Kumar9https://orcid.org/0000-0001-7225-2475Helong Guo10https://orcid.org/0000-0001-5737-6445Xufeng Zhu11https://orcid.org/0009-0003-6936-7548Yangwei Zhang12https://orcid.org/0009-0000-7791-8192Fanchuan Kong13https://orcid.org/0009-0009-9343-090XChenxi Shang14https://orcid.org/0009-0002-9069-8774Xinlei Chen15https://orcid.org/0009-0000-4068-1320Xiangkun Liu16https://orcid.org/0000-0003-0394-1298Xiaowei Liu17https://orcid.org/0000-0003-1295-2909South-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSchool of Astronomy and Space Science, Nanjing University , Nanjing 210093, People’s Republic of China ; jyang@smail.nju.edu.cn; Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University) , Ministry of Education, People’s Republic of ChinaSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnSouth-Western Institute for Astronomy Research, Key Laboratory of Survey Science of Yunnan Province, Yunnan University , Kunming, Yunnan 650504, People’s Republic of China ; ypyang@ynu.edu.cn, zhang_jh@ynu.edu.cn, x.liu@ynu.edu.cnThe interaction between the relativistic jet and the circumburst medium produces a multiwavelength afterglow of a gamma-ray burst (GRBs). In this work, we present multiwavelength properties of GRB 250101A based on the observations of Swift, Fermi, and Mephisto. The spectral analysis of Swift/Swift Burst Alert Telescope (BAT) and Fermi/Gamma-ray Burst Monitor (GBM) reveals a soft prompt spectrum with a low-energy photon index of −1.18 and a peak energy of 33 keV, and the isotropic energy is 1.4 × 10 ^52 erg. The prompt emission of GRB 250101A aligns with Type II GRBs in the Amati relation. Meanwhile, our analysis indicates that GRB 250101A is an X-ray-rich or X-ray-dominated GRB, with intrinsic properties suggesting that it is relatively softer than most classical GRBs. Optical observation with Mephisto, beginning 197 s post-trigger, shows a single power-law decay in uvgriz bands, with F _ν _,obs ∝ t ^−0.76 ν ^−1.21 . The observed spectral index significantly exceeds theoretical predictions under standard afterglow models, suggesting a color excess of ∼0.216 mag. However, combining X-ray and optical afterglow, we find that GRB 250101A is more likely a “normal burst” rather than an “optical-dark burst,” and the dust extinction effect plays an important role in the optical blue bands. Furthermore, there is a structural change at T _0 + 2924 s in the optical light curve, indicating a density drop of ∼50% in the interstellar medium at a distance of ∼0.13 pc. Our analysis shows that this GRB clearly shows some unique characteristics in its observed X-ray-rich prompt emission as well as the circumburst environment, implying a special progenitor.https://doi.org/10.3847/1538-4357/adea3dGamma-ray burstsLight curvesOptical astronomy |
| spellingShingle | Guowang Du Yehao Cheng Yuan-Pei Yang Jun Yang Jinghua Zhang Dan Zhu Yu Pan Yuan Fang Xingzhu Zou Brajesh Kumar Helong Guo Xufeng Zhu Yangwei Zhang Fanchuan Kong Chenxi Shang Xinlei Chen Xiangkun Liu Xiaowei Liu Multiwavelength Analysis of GRB 250101A: From Gamma-Ray Prompt Emission to Optical Afterglow The Astrophysical Journal Gamma-ray bursts Light curves Optical astronomy |
| title | Multiwavelength Analysis of GRB 250101A: From Gamma-Ray Prompt Emission to Optical Afterglow |
| title_full | Multiwavelength Analysis of GRB 250101A: From Gamma-Ray Prompt Emission to Optical Afterglow |
| title_fullStr | Multiwavelength Analysis of GRB 250101A: From Gamma-Ray Prompt Emission to Optical Afterglow |
| title_full_unstemmed | Multiwavelength Analysis of GRB 250101A: From Gamma-Ray Prompt Emission to Optical Afterglow |
| title_short | Multiwavelength Analysis of GRB 250101A: From Gamma-Ray Prompt Emission to Optical Afterglow |
| title_sort | multiwavelength analysis of grb 250101a from gamma ray prompt emission to optical afterglow |
| topic | Gamma-ray bursts Light curves Optical astronomy |
| url | https://doi.org/10.3847/1538-4357/adea3d |
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