Triggering the Untriggered: The First Einstein Probe-Detected Gamma-Ray Burst 240219A and Its Implications
The Einstein Probe (EP) achieved its first detection and localization of a bright X-ray flare, EP240219a, on 2024 February 19, during its commissioning phase. Subsequent targeted searches triggered by the EP240219a alert identified a faint, untriggered gamma-ray burst (GRB) in the archived data of F...
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| creator | Yi-Han, Iris Yin Bin-Bin, Zhang Yang, Jun Sun, Hui Zhang, Chen Yi-Xuan Shao You-Dong, Hu Zi-Pei Zhu Xu, Dong Li, An Gao, He Xue-Feng, Wu Zhang, Bing Castro-Tirado, Alberto Javier Pandey, Shashi B Rau, Arne Lei, Weihua Xie, Wei Ghirlanda, Giancarlo Piro, Luigi O'Brien, Paul Troja, Eleonora Jonker, Peter Yun-Wei, Yu An, Jie Chen, Run-Chao Yi-Jing, Chen Xiao-Fei, Dong Eyles-Ferris, Rob Zhou, Fan Shao-Yu, Fu Fynbo, Johan P U Gao, Xing Yong-Feng, Huang Shuai-Qing Jiang Ya-Hui, Jiang Julakanti, Yashaswi Kuulkers, Erik Qing-Hui Lao Li, Dongyue Zhi-Xing Ling Liu, Xing Liu, Yuan Jia-Yu, Mou Pan, Xin Varun Wei, Daming Wu, Qinyu Yadav, Muskan Yu-Han, Yang Yuan, Weimin Zhang, Shuang-Nan |
| description | The Einstein Probe (EP) achieved its first detection and localization of a bright X-ray flare, EP240219a, on 2024 February 19, during its commissioning phase. Subsequent targeted searches triggered by the EP240219a alert identified a faint, untriggered gamma-ray burst (GRB) in the archived data of Fermi Gamma-ray Burst Monitor (GBM), Swift Burst Alert Telescope (BAT), and Insight-HXMT/HE. The EP Wide-field X-ray Telescope (WXT) light curve reveals a long duration of approximately 160 s with a slow decay, whereas the Fermi/GBM light curve shows a total duration of approximately 70 s. The peak in the Fermi/GBM light curve occurs slightly later with respect to the peak seen in the EP/WXT light curve. Our spectral analysis shows that a single cutoff power-law (PL) model effectively describes the joint EP/WXT--Fermi/GBM spectra in general, indicating coherent broad emission typical of GRBs. The model yielded a photon index of \(\sim -1.70 \pm 0.05\) and a peak energy of \(\sim 257 \pm 134\) keV. After detection of GRB 240219A, long-term observations identified several candidates in optical and radio wavelengths, none of which was confirmed as the afterglow counterpart during subsequent optical and near-infrared follow-ups. The analysis of GRB 240219A classifies it as an X-ray rich GRB (XRR) with a high peak energy, presenting both challenges and opportunities for studying the physical origins of X-ray flashes, XRRs, and classical GRBs. Furthermore, linking the cutoff PL component to nonthermal synchrotron radiation suggests that the burst is driven by a Poynting flux-dominated outflow. |
| doi_str_mv | 10.48550/arxiv.2407.10156 |
| format | Article |
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Subsequent targeted searches triggered by the EP240219a alert identified a faint, untriggered gamma-ray burst (GRB) in the archived data of Fermi Gamma-ray Burst Monitor (GBM), Swift Burst Alert Telescope (BAT), and Insight-HXMT/HE. The EP Wide-field X-ray Telescope (WXT) light curve reveals a long duration of approximately 160 s with a slow decay, whereas the Fermi/GBM light curve shows a total duration of approximately 70 s. The peak in the Fermi/GBM light curve occurs slightly later with respect to the peak seen in the EP/WXT light curve. Our spectral analysis shows that a single cutoff power-law (PL) model effectively describes the joint EP/WXT--Fermi/GBM spectra in general, indicating coherent broad emission typical of GRBs. The model yielded a photon index of \(\sim -1.70 \pm 0.05\) and a peak energy of \(\sim 257 \pm 134\) keV. After detection of GRB 240219A, long-term observations identified several candidates in optical and radio wavelengths, none of which was confirmed as the afterglow counterpart during subsequent optical and near-infrared follow-ups. The analysis of GRB 240219A classifies it as an X-ray rich GRB (XRR) with a high peak energy, presenting both challenges and opportunities for studying the physical origins of X-ray flashes, XRRs, and classical GRBs. Furthermore, linking the cutoff PL component to nonthermal synchrotron radiation suggests that the burst is driven by a Poynting flux-dominated outflow.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2407.10156</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Afterglows ; Emission spectra ; Gamma ray bursts ; Gamma rays ; Infrared analysis ; Light curve ; Physics - High Energy Astrophysical Phenomena ; Pluto ; Power law ; Spectrum analysis ; Synchrotron radiation ; X ray flashes</subject><ispartof>arXiv.org, 2024-11</ispartof><rights>2024. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,784,885,27925</link.rule.ids><backlink>$$Uhttps://doi.org/10.3847/2041-8213/ad8652$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.2407.10156$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Yi-Han, Iris Yin</creatorcontrib><creatorcontrib>Bin-Bin, Zhang</creatorcontrib><creatorcontrib>Yang, Jun</creatorcontrib><creatorcontrib>Sun, Hui</creatorcontrib><creatorcontrib>Zhang, Chen</creatorcontrib><creatorcontrib>Yi-Xuan Shao</creatorcontrib><creatorcontrib>You-Dong, Hu</creatorcontrib><creatorcontrib>Zi-Pei Zhu</creatorcontrib><creatorcontrib>Xu, Dong</creatorcontrib><creatorcontrib>Li, An</creatorcontrib><creatorcontrib>Gao, He</creatorcontrib><creatorcontrib>Xue-Feng, Wu</creatorcontrib><creatorcontrib>Zhang, Bing</creatorcontrib><creatorcontrib>Castro-Tirado, Alberto Javier</creatorcontrib><creatorcontrib>Pandey, Shashi B</creatorcontrib><creatorcontrib>Rau, Arne</creatorcontrib><creatorcontrib>Lei, Weihua</creatorcontrib><creatorcontrib>Xie, Wei</creatorcontrib><creatorcontrib>Ghirlanda, Giancarlo</creatorcontrib><creatorcontrib>Piro, Luigi</creatorcontrib><creatorcontrib>O'Brien, Paul</creatorcontrib><creatorcontrib>Troja, Eleonora</creatorcontrib><creatorcontrib>Jonker, Peter</creatorcontrib><creatorcontrib>Yun-Wei, Yu</creatorcontrib><creatorcontrib>An, Jie</creatorcontrib><creatorcontrib>Chen, Run-Chao</creatorcontrib><creatorcontrib>Yi-Jing, Chen</creatorcontrib><creatorcontrib>Xiao-Fei, Dong</creatorcontrib><creatorcontrib>Eyles-Ferris, Rob</creatorcontrib><creatorcontrib>Zhou, Fan</creatorcontrib><creatorcontrib>Shao-Yu, Fu</creatorcontrib><creatorcontrib>Fynbo, Johan P U</creatorcontrib><creatorcontrib>Gao, Xing</creatorcontrib><creatorcontrib>Yong-Feng, Huang</creatorcontrib><creatorcontrib>Shuai-Qing Jiang</creatorcontrib><creatorcontrib>Ya-Hui, Jiang</creatorcontrib><creatorcontrib>Julakanti, Yashaswi</creatorcontrib><creatorcontrib>Kuulkers, Erik</creatorcontrib><creatorcontrib>Qing-Hui Lao</creatorcontrib><creatorcontrib>Li, Dongyue</creatorcontrib><creatorcontrib>Zhi-Xing Ling</creatorcontrib><creatorcontrib>Liu, Xing</creatorcontrib><creatorcontrib>Liu, Yuan</creatorcontrib><creatorcontrib>Jia-Yu, Mou</creatorcontrib><creatorcontrib>Pan, Xin</creatorcontrib><creatorcontrib>Varun</creatorcontrib><creatorcontrib>Wei, Daming</creatorcontrib><creatorcontrib>Wu, Qinyu</creatorcontrib><creatorcontrib>Yadav, Muskan</creatorcontrib><creatorcontrib>Yu-Han, Yang</creatorcontrib><creatorcontrib>Yuan, Weimin</creatorcontrib><creatorcontrib>Zhang, Shuang-Nan</creatorcontrib><title>Triggering the Untriggered: The First Einstein Probe-Detected Gamma-Ray Burst 240219A and Its Implications</title><title>arXiv.org</title><description>The Einstein Probe (EP) achieved its first detection and localization of a bright X-ray flare, EP240219a, on 2024 February 19, during its commissioning phase. Subsequent targeted searches triggered by the EP240219a alert identified a faint, untriggered gamma-ray burst (GRB) in the archived data of Fermi Gamma-ray Burst Monitor (GBM), Swift Burst Alert Telescope (BAT), and Insight-HXMT/HE. The EP Wide-field X-ray Telescope (WXT) light curve reveals a long duration of approximately 160 s with a slow decay, whereas the Fermi/GBM light curve shows a total duration of approximately 70 s. The peak in the Fermi/GBM light curve occurs slightly later with respect to the peak seen in the EP/WXT light curve. Our spectral analysis shows that a single cutoff power-law (PL) model effectively describes the joint EP/WXT--Fermi/GBM spectra in general, indicating coherent broad emission typical of GRBs. The model yielded a photon index of \(\sim -1.70 \pm 0.05\) and a peak energy of \(\sim 257 \pm 134\) keV. After detection of GRB 240219A, long-term observations identified several candidates in optical and radio wavelengths, none of which was confirmed as the afterglow counterpart during subsequent optical and near-infrared follow-ups. The analysis of GRB 240219A classifies it as an X-ray rich GRB (XRR) with a high peak energy, presenting both challenges and opportunities for studying the physical origins of X-ray flashes, XRRs, and classical GRBs. Furthermore, linking the cutoff PL component to nonthermal synchrotron radiation suggests that the burst is driven by a Poynting flux-dominated outflow.</description><subject>Afterglows</subject><subject>Emission spectra</subject><subject>Gamma ray bursts</subject><subject>Gamma rays</subject><subject>Infrared analysis</subject><subject>Light curve</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Pluto</subject><subject>Power law</subject><subject>Spectrum analysis</subject><subject>Synchrotron radiation</subject><subject>X ray flashes</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotkE1PAjEURRsTEwnyA1zZxPVgv960uEMEJCHRKK4nnWkHS5gOtsXAv3cAVze5OXnv5iB0R8lQKADyqMPB_Q6ZIHJICYX8CvUY5zRTgrEbNIhxQwhhuWQAvIc2q-DWaxucX-P0bfGXT5fCmie86oqZCzHhqfMxWefxe2hLm73YZKtkDZ7rptHZhz7i5_2J694yOhpj7Q1epIgXzW7rKp1c6-Mtuq71NtrBf_bR52y6mrxmy7f5YjJeZhqYyACErXOpqJaSjsAaI7muczCloIYDJyBqSSpa1rwEokDpKifKSD3iTHHG--j-cvXsodgF1-hwLE4-irOPjni4ELvQ_uxtTMWm3QffTSo4UVQIyrjgf1ymYRk</recordid><startdate>20241111</startdate><enddate>20241111</enddate><creator>Yi-Han, Iris Yin</creator><creator>Bin-Bin, Zhang</creator><creator>Yang, Jun</creator><creator>Sun, Hui</creator><creator>Zhang, Chen</creator><creator>Yi-Xuan Shao</creator><creator>You-Dong, 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Gamma-Ray Burst 240219A and Its Implications</title><author>Yi-Han, Iris Yin ; Bin-Bin, Zhang ; Yang, Jun ; Sun, Hui ; Zhang, Chen ; Yi-Xuan Shao ; You-Dong, Hu ; Zi-Pei Zhu ; Xu, Dong ; Li, An ; Gao, He ; Xue-Feng, Wu ; Zhang, Bing ; Castro-Tirado, Alberto Javier ; Pandey, Shashi B ; Rau, Arne ; Lei, Weihua ; Xie, Wei ; Ghirlanda, Giancarlo ; Piro, Luigi ; O'Brien, Paul ; Troja, Eleonora ; Jonker, Peter ; Yun-Wei, Yu ; An, Jie ; Chen, Run-Chao ; Yi-Jing, Chen ; Xiao-Fei, Dong ; Eyles-Ferris, Rob ; Zhou, Fan ; Shao-Yu, Fu ; Fynbo, Johan P U ; Gao, Xing ; Yong-Feng, Huang ; Shuai-Qing Jiang ; Ya-Hui, Jiang ; Julakanti, Yashaswi ; Kuulkers, Erik ; Qing-Hui Lao ; Li, Dongyue ; Zhi-Xing Ling ; Liu, Xing ; Liu, Yuan ; Jia-Yu, Mou ; Pan, Xin ; Varun ; Wei, Daming ; Wu, Qinyu ; Yadav, Muskan ; Yu-Han, Yang ; Yuan, Weimin ; Zhang, 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Xing</au><au>Yong-Feng, Huang</au><au>Shuai-Qing Jiang</au><au>Ya-Hui, Jiang</au><au>Julakanti, Yashaswi</au><au>Kuulkers, Erik</au><au>Qing-Hui Lao</au><au>Li, Dongyue</au><au>Zhi-Xing Ling</au><au>Liu, Xing</au><au>Liu, Yuan</au><au>Jia-Yu, Mou</au><au>Pan, Xin</au><au>Varun</au><au>Wei, Daming</au><au>Wu, Qinyu</au><au>Yadav, Muskan</au><au>Yu-Han, Yang</au><au>Yuan, Weimin</au><au>Zhang, Shuang-Nan</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Triggering the Untriggered: The First Einstein Probe-Detected Gamma-Ray Burst 240219A and Its Implications</atitle><jtitle>arXiv.org</jtitle><date>2024-11-11</date><risdate>2024</risdate><eissn>2331-8422</eissn><abstract>The Einstein Probe (EP) achieved its first detection and localization of a bright X-ray flare, EP240219a, on 2024 February 19, during its commissioning phase. Subsequent targeted searches triggered by the EP240219a alert identified a faint, untriggered gamma-ray burst (GRB) in the archived data of Fermi Gamma-ray Burst Monitor (GBM), Swift Burst Alert Telescope (BAT), and Insight-HXMT/HE. The EP Wide-field X-ray Telescope (WXT) light curve reveals a long duration of approximately 160 s with a slow decay, whereas the Fermi/GBM light curve shows a total duration of approximately 70 s. The peak in the Fermi/GBM light curve occurs slightly later with respect to the peak seen in the EP/WXT light curve. Our spectral analysis shows that a single cutoff power-law (PL) model effectively describes the joint EP/WXT--Fermi/GBM spectra in general, indicating coherent broad emission typical of GRBs. The model yielded a photon index of \(\sim -1.70 \pm 0.05\) and a peak energy of \(\sim 257 \pm 134\) keV. After detection of GRB 240219A, long-term observations identified several candidates in optical and radio wavelengths, none of which was confirmed as the afterglow counterpart during subsequent optical and near-infrared follow-ups. The analysis of GRB 240219A classifies it as an X-ray rich GRB (XRR) with a high peak energy, presenting both challenges and opportunities for studying the physical origins of X-ray flashes, XRRs, and classical GRBs. Furthermore, linking the cutoff PL component to nonthermal synchrotron radiation suggests that the burst is driven by a Poynting flux-dominated outflow.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2407.10156</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2024-11 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_2407_10156 |
| source | arXiv.org; Free E- Journals |
| subjects | Afterglows Emission spectra Gamma ray bursts Gamma rays Infrared analysis Light curve Physics - High Energy Astrophysical Phenomena Pluto Power law Spectrum analysis Synchrotron radiation X ray flashes |
| title | Triggering the Untriggered: The First Einstein Probe-Detected Gamma-Ray Burst 240219A and Its Implications |
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