MAGIC very large zenith angle observations of the Crab Nebula up to 100 TeV
MAGIC very large zenith angle observations of the Crab Nebula up to 100 TeV
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DOI：
10.1051/0004-6361/201936899
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发表时间：
2020-01
影响因子：
6.5
通讯作者：
M. Acciari;S. Ansoldi;L. A. Antonelli;A. A. Engels-A.;D. Baack;A. Babi'c;B. Banerjee;U. D. Almeida;J. Barrio;J. Gonz'alez;W. Bednarek;L. Bellizzi;E. Bernardini;A. Berti;J. Besenrieder;W. Bhattacharyya;C. Bigongiari;A. Biland;O. Blanch;G. Bonnoli;vZ. Bovsnjak;G. Busetto;R. Carosi;G. Ceribella;Y. Chai;A. Chilingaryan;S. Cikota;S. M. Colak;U. Colin;E. Colombo;J. Contreras;J. Cortina;S. Covino;V. D’Elia;P. D. Vela;F. Dazzi;A. Angelis;B. Lotto;M. Delfino;J. Delgado;D. Depaoli;F. D. Pierro;L. Venere;E. Espineira;D. Prester;A. Donini;D. Dorner;M. Doro;D. Elsaesser;V. Ramazani;A. Fattorini;G. Ferrara;D. Fidalgo;L. Foffano;M. V. Fonseca;L. Font;C. Fruck;S. Fukami;R. L'opez;M. Garczarczyk;S. Gasparyan;M. Gaug;N. Giglietto;F. Giordano;N. Godinovi'c;D. Green;D. Guberman;D. Hadasch;A. Hahn;J. Herrera;J. Hoang;D. Hrupec;M. Hutten;T. Inada;S. Inoue;K. Ishio;Y. Iwamura;L. Jouvin;D. Kerszberg;H. Kubo;J. Kushida;A. Lamastra;D. Lelas;F. Leone;E. Lindfors;S. Lombardi;F. Longo;M. L'opez;R. L'opez-Coto;A. L'opez-Oramas;S. Loporchio;B. Fraga;C. Maggio;P. Majumdar;M. Makariev;M. Mallamaci;G. Maneva;M. Manganaro;K. Mannheim;L. Maraschi;M. Mariotti;M. Mart'inez;D. Mazin;S. Mi'canovi'c;D. Miceli;M. Minev;J. Miranda;R. Mirzoyan;E. Molina;A. Moralejo;D. Morcuende;V. Moreno;E. Moretti;P. Munar-Adrover;V. Neustroev;C. Nigro;K. Nilsson;D. Ninci;K. Nishijima;K. Noda;L. Nogu'es;S. Nozaki;S. Paiano;J. Palacio;M. Palatiello;D. Paneque;R. Paoletti;J. Paredes;P. Peñil;Michele Peresano;M. Persic;P. Moroni;E. Prandini;I. Puljak;W. Rhode;M. Rib'o;J. Rico;C. Righi;A. Rugliancich;L. Saha;N. Sahakyan;T. Saito;S. Sakurai;K. Satalecka;K. Schmidt;T. Schweizer;J. Sitarek;I. vSnidari'c;D. Sobczynska;A. Somero;A. Stamerra;D. Strom;M. Strzys;Y. Suda;T. Suri'c;M. Takahashi;F. Tavecchio;P. Temnikov;T. Terzi'c;M. Teshima;N. Torres-Albà;L. Tosti;V. Vagelli;J. Scherpenberg;G. Vanzo;M. Acosta;C. Vigorito;V. Vitale;I. Vovk;M. Will;D. Zari'c
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文献类型：
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作者：
M. Acciari;S. Ansoldi;L. A. Antonelli;A. A. Engels-A.;D. Baack;A. Babi'c;B. Banerjee;U. D. Almeida;J. Barrio;J. Gonz'alez;W. Bednarek;L. Bellizzi;E. Bernardini;A. Berti;J. Besenrieder;W. Bhattacharyya;C. Bigongiari;A. Biland;O. Blanch;G. Bonnoli;vZ. Bovsnjak;G. Busetto;R. Carosi;G. Ceribella;Y. Chai;A. Chilingaryan;S. Cikota;S. M. Colak;U. Colin;E. Colombo;J. Contreras;J. Cortina;S. Covino;V. D’Elia;P. D. Vela;F. Dazzi;A. Angelis;B. Lotto;M. Delfino;J. Delgado;D. Depaoli;F. D. Pierro;L. Venere;E. Espineira;D. Prester;A. Donini;D. Dorner;M. Doro;D. Elsaesser;V. Ramazani;A. Fattorini;G. Ferrara;D. Fidalgo;L. Foffano;M. V. Fonseca;L. Font;C. Fruck;S. Fukami;R. L'opez;M. Garczarczyk;S. Gasparyan;M. Gaug;N. Giglietto;F. Giordano;N. Godinovi'c;D. Green;D. Guberman;D. Hadasch;A. Hahn;J. Herrera;J. Hoang;D. Hrupec;M. Hutten;T. Inada;S. Inoue;K. Ishio;Y. Iwamura;L. Jouvin;D. Kerszberg;H. Kubo;J. Kushida;A. Lamastra;D. Lelas;F. Leone;E. Lindfors;S. Lombardi;F. Longo;M. L'opez;R. L'opez-Coto;A. L'opez-Oramas;S. Loporchio;B. Fraga;C. Maggio;P. Majumdar;M. Makariev;M. Mallamaci;G. Maneva;M. Manganaro;K. Mannheim;L. Maraschi;M. Mariotti;M. Mart'inez;D. Mazin;S. Mi'canovi'c;D. Miceli;M. Minev;J. Miranda;R. Mirzoyan;E. Molina;A. Moralejo;D. Morcuende;V. Moreno;E. Moretti;P. Munar-Adrover;V. Neustroev;C. Nigro;K. Nilsson;D. Ninci;K. Nishijima;K. Noda;L. Nogu'es;S. Nozaki;S. Paiano;J. Palacio;M. Palatiello;D. Paneque;R. Paoletti;J. Paredes;P. Peñil;Michele Peresano;M. Persic;P. Moroni;E. Prandini;I. Puljak;W. Rhode;M. Rib'o;J. Rico;C. Righi;A. Rugliancich;L. Saha;N. Sahakyan;T. Saito;S. Sakurai;K. Satalecka;K. Schmidt;T. Schweizer;J. Sitarek;I. vSnidari'c;D. Sobczynska;A. Somero;A. Stamerra;D. Strom;M. Strzys;Y. Suda;T. Suri'c;M. Takahashi;F. Tavecchio;P. Temnikov;T. Terzi'c;M. Teshima;N. Torres-Albà;L. Tosti;V. Vagelli;J. Scherpenberg;G. Vanzo;M. Acosta;C. Vigorito;V. Vitale;I. Vovk;M. Will;D. Zari'c
目标。我们测量了蟹状星云在~100 TeV能量范围内的γ射线谱能量分布，并在这些高能量下检验了现有轻子发射模型的有效性。方法.我们使用了新的非常大的天顶角观测与MAGIC望远镜系统，以增加收集面积超过10 TeV。我们还开发了一个监测大气传输的辅助程序，以确保对积累的数据进行适当的校准。这采用了在源位置旁边记录恒星场的光学图像，这为透射测量提供了优于10%的精度。结果我们证明，MAGIC非常大的天顶角观测产生的收集面积大于一平方公里。在仅约56小时的观测中，我们探测到蟹状星云高达100 TeV的γ射线发射，从而提供了迄今为止使用成像大气切伦科夫望远镜对该源的最高能量测量。将积累的和存档的MAGIC和Fermi/LAT数据与一些现有的发射模型进行比较，我们发现它们都不能准确描述1 GeV到100 TeV的γ射线信号。
Aims. We measure the Crab Nebula γ-ray spectral energy distribution in the ~100 TeV energy domain and test the validity of existing leptonic emission models at these high energies. Methods. We used the novel very large zenith angle observations with the MAGIC telescope system to increase the collection area above 10 TeV. We also developed an auxiliary procedure of monitoring atmospheric transmission in order to assure proper calibration of the accumulated data. This employs recording optical images of the stellar field next to the source position, which provides a better than 10% accuracy for the transmission measurements. Results. We demonstrate that MAGIC very large zenith angle observations yield a collection area larger than a square kilometer. In only ~ 56 h of observations, we detect the γ-ray emission from the Crab Nebula up to 100 TeV, thus providing the highest energy measurement of this source to date with Imaging Atmospheric Cherenkov Telescopes. Comparing accumulated and archival MAGIC and Fermi/LAT data with some of the existing emission models, we find that none of them provides an accurate description of the 1 GeV to 100 TeV γ-ray signal.