H.E.S.S. Follow-up Observations of GRB 221009A
H.E.S.S. Follow-up Observations of GRB 221009A
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DOI：
10.3847/2041-8213/acc405
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发表时间：
2023-03
期刊：
影响因子：
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通讯作者：
H. C. F. Aharonian;F. Benkhali;J. Aschersleben;H. Ashkar;Michael Backes;A. Baktash;V. B. Martins;R. Batzofin;Y. Becherini;D. Berge;K. Bernlohr;B. Bi;M. Bottcher;C. Boisson;J. Bolmont;M. D. B. Lavergne;J. Borowska;M. Bouyahiaoui;F. Bradascio;M. Breuhaus;R. Brose;F. Brun;B. Bruno;T. Bulik;C. Burger-Scheidlin;S. Caroff;S. Casanova;J. Celić;M. Cerruti;T. Chand;S. Chandra;A. Chen;J. Chibueze;O. Chibueze;G. Cotter;S. Dai;J. D. Mbarubucyeye;J. Devin;A. Djannati-Atai;A. Dmytriiev;V. Doroshenko;K. Egberts;S. Einecke;J. Ernenwein;S. Fegan;G. F. D. Clairfontaine;M. Filipović;G. Fontaine;M. Fussling;S. Funk;S. Gabici;S. Ghafourizadeh;G. Giavitto;D. Glawion;J. Glicenstein;P. Goswami;G. Grolleron;Morna Hinton;T. Holch;M. Holler;D. Horns;Zhiqiu Huang;M. Jamrozy;F. Jankowsky;V. Joshi;I. Jung-Richardt;E. Kasai;K. Katarzy'nski;R. Khatoon;B. Kh'elifi;W. Klu'zniak;N. Komin;R. Konno;K. Kosack;D. Kostunin;R. G. Lang;S. L. Stum;F. Leitl;A. Lemière;M. Lemoine-Goumard;J. Lenain;F. Leuschner;T. Lohse;I. Lypova;J. Mackey;D. Malyshev;V. Marandon;P. Marchegiani;A. Marcowith;G. Mart'i-Devesa;R. Marx;M. Meyer;A. Mitchell;L. Mohrmann;A. Montanari;E. Moulin;T. Murach;K. Nakashima;M. Naurois;J. Niemiec;A. Noel;P. O’Brien;S. Ohm;L. Olivera-Nieto;E. Wilhelmi;M. Ostrowski;S. Panny;M. Panter;R. Parsons;G. Peron;D. Prokhorov;H. Prokoph;G. Puhlhofer;M. Punch;A. Quirrenbach;P. Reichherzer;A. Reimer;O. Reimer;H. Ren;M. Renaud;B. Reville;F. Rieger;G. Rowell;B. Rudak;E. Ruiz-Velasco;V. Sahakian;H. Salzmann;A. Santangelo;M. Sasaki;J. Schafer;F. Schussler;H. Schutte;U. Schwanke;J. Shapopi;A. Specovius;S. Spencer;L. Stawarz;R. Steenkamp;S. Steinmassl;C. Steppa;I. Sushch;H. Suzuki;T. Takahashi;T. Tanaka;R. Terrier;N. Tsuji;Y. Uchiyama;M. Vecchi;C. Venter;J. Vink;S. Wagner;R. White;A. Wierzcholska;Y. Wong;M. Zacharias;D. Zargaryan;A. Zdziarski;A. Zech;S. Zhu;N. Żywucka
中科院分区：
文献类型：
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作者：
H. C. F. Aharonian;F. Benkhali;J. Aschersleben;H. Ashkar;Michael Backes;A. Baktash;V. B. Martins;R. Batzofin;Y. Becherini;D. Berge;K. Bernlohr;B. Bi;M. Bottcher;C. Boisson;J. Bolmont;M. D. B. Lavergne;J. Borowska;M. Bouyahiaoui;F. Bradascio;M. Breuhaus;R. Brose;F. Brun;B. Bruno;T. Bulik;C. Burger-Scheidlin;S. Caroff;S. Casanova;J. Celić;M. Cerruti;T. Chand;S. Chandra;A. Chen;J. Chibueze;O. Chibueze;G. Cotter;S. Dai;J. D. Mbarubucyeye;J. Devin;A. Djannati-Atai;A. Dmytriiev;V. Doroshenko;K. Egberts;S. Einecke;J. Ernenwein;S. Fegan;G. F. D. Clairfontaine;M. Filipović;G. Fontaine;M. Fussling;S. Funk;S. Gabici;S. Ghafourizadeh;G. Giavitto;D. Glawion;J. Glicenstein;P. Goswami;G. Grolleron;Morna Hinton;T. Holch;M. Holler;D. Horns;Zhiqiu Huang;M. Jamrozy;F. Jankowsky;V. Joshi;I. Jung-Richardt;E. Kasai;K. Katarzy'nski;R. Khatoon;B. Kh'elifi;W. Klu'zniak;N. Komin;R. Konno;K. Kosack;D. Kostunin;R. G. Lang;S. L. Stum;F. Leitl;A. Lemière;M. Lemoine-Goumard;J. Lenain;F. Leuschner;T. Lohse;I. Lypova;J. Mackey;D. Malyshev;V. Marandon;P. Marchegiani;A. Marcowith;G. Mart'i-Devesa;R. Marx;M. Meyer;A. Mitchell;L. Mohrmann;A. Montanari;E. Moulin;T. Murach;K. Nakashima;M. Naurois;J. Niemiec;A. Noel;P. O’Brien;S. Ohm;L. Olivera-Nieto;E. Wilhelmi;M. Ostrowski;S. Panny;M. Panter;R. Parsons;G. Peron;D. Prokhorov;H. Prokoph;G. Puhlhofer;M. Punch;A. Quirrenbach;P. Reichherzer;A. Reimer;O. Reimer;H. Ren;M. Renaud;B. Reville;F. Rieger;G. Rowell;B. Rudak;E. Ruiz-Velasco;V. Sahakian;H. Salzmann;A. Santangelo;M. Sasaki;J. Schafer;F. Schussler;H. Schutte;U. Schwanke;J. Shapopi;A. Specovius;S. Spencer;L. Stawarz;R. Steenkamp;S. Steinmassl;C. Steppa;I. Sushch;H. Suzuki;T. Takahashi;T. Tanaka;R. Terrier;N. Tsuji;Y. Uchiyama;M. Vecchi;C. Venter;J. Vink;S. Wagner;R. White;A. Wierzcholska;Y. Wong;M. Zacharias;D. Zargaryan;A. Zdziarski;A. Zech;S. Zhu;N. Żywucka
GRB 221009 A是迄今为止发现的最明亮的伽马射线暴。为了探测甚高能（VHE; >100 GeV）发射，高能立体系统（H.E.S.S.）在触发事件后53小时开始观测，此时月光的亮度不再妨碍观测。我们使用H.E.S.S.导出微分和积分上限。在应用大气校正之后，从最初的伽玛射线暴探测之后的第三、第四和第九个夜晚获得的数据。综合观测得到的积分能流上限为ΦUL95%=9.7×10− 12 ergcm −2s−1，高于E thr = 650 GeV。从H.E.S.S.观测补充了现有的多波长数据。射电到X射线的数据与单电子群的同步辐射一致，其光谱能量分布的峰值出现在X射线波段之上。与VHE明亮的GRB 190829 A相比，GRB 221009 A的上限意味着余辉中的伽马射线与X射线通量比较小。即使没有探测到，高能量发射系统。因此，上限有助于GRB 221009 A的多波长图像，有效地排除了IC占主导地位的情况。
GRB 221009A is the brightest gamma-ray burst (GRB) ever detected. To probe the very-high-energy (VHE; >100 GeV) emission, the High Energy Stereoscopic System (H.E.S.S.) began observations 53 hr after the triggering event, when the brightness of the moonlight no longer precluded observations. We derive differential and integral upper limits using H.E.S.S. data from the third, fourth, and ninth nights after the initial GRB detection, after applying atmospheric corrections. The combined observations yield an integral energy flux upper limit of ΦUL95%=9.7×10−12ergcm−2s−1 above E thr = 650 GeV. The constraints derived from the H.E.S.S. observations complement the available multiwavelength data. The radio to X-ray data are consistent with synchrotron emission from a single electron population, with the peak in the spectral energy distribution occurring above the X-ray band. Compared to the VHE-bright GRB 190829A, the upper limits for GRB 221009A imply a smaller gamma-ray to X-ray flux ratio in the afterglow. Even in the absence of a detection, the H.E.S.S. upper limits thus contribute to the multiwavelength picture of GRB 221009A, effectively ruling out an IC-dominated scenario.