OBSERVATIONS OF THE CRAB PULSAR BETWEEN 25 AND 100 GeV WITH THE MAGIC I TELESCOPE
OBSERVATIONS OF THE CRAB PULSAR BETWEEN 25 AND 100 GeV WITH THE MAGIC I TELESCOPE
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DOI：
10.1088/0004-637x/742/1/43
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发表时间：
2011-08
期刊：
影响因子：
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通讯作者：
M. C. J. Aleksi'c;E. Alvarez;L. A. Antonelli;P. Antoranz;M. Asensio;M. Backes;J. Barrio;D. Bastieri;J. Gonz'alez;W. Bednarek;A. Berdyugin;K. Berger;E. Bernardini;A. Biland;O. Blanch;R. Bock;A. Boller;G. Bonnoli;D. Tridon;I. Braun;T. Bretz;A. Cañellas;E. Carmona;A. Carosi;P. Colin;E. Colombo;J. Contreras;J. Cortina;L. Cossio;S. Covino;F. Dazzi;A. Angelis;G. Caneva;E. C. D. Pozo;B. Lotto;C. Mendez;A. Ortega;M. Doert;A. Domínguez;D. Prester;D. Dorner;M. Doro;D. Eisenacher;D. Elsaesser;D. Ferenc;M. V. Fonseca;L. Font;C. Fruck;R. L'opez;M. Garczarczyk;D. Garrido;G. Giavitto;N. Godinovi'c;D. Hadasch;D. Hafner;A. Herrero;D. Hildebrand;D. Hohne-Monch;J. Hose;D. Hrupec;T. Jogler;H. Kellermann;S. Klepser;T. Krahenbuhl;J. Krause;J. Kushida;A. Barbera;D. Lelas;E. Leonardo;E. Lindfors;S. Lombardi;M. L'opez;A. L'opez-Oramas;E. Lorenz;M. Makariev;G. Maneva;N. Mankuzhiyil;K. Mannheim;L. Maraschi;B. Marcote;M. Mariotti;M. Mart'inez;D. Mazin;M. Meucci;J. Miranda;R. Mirzoyan;J. Mold'on;A. Moralejo;P. Munar-Adrover;D. Nieto;K. Nilsson;R. Orito;N. Otte;I. Oya;D. Paneque;R. Paoletti;S. Pardo;J. Paredes;S. Partini;M. Pérez-Torres;M. Persic;L. Peruzzo;M. Pilia;J. Pochon;F. Prada;P. Moroni;E. Prandini;I. Gimenez;I. Puljak;I. Reichardt;R. Reinthal;W. Rhode;M. Rib'o;J. Rico;M. Rissi;S. Rugamer;A. Saggion;K. Saito;T. Saito;M. Salvati;K. Satalecka;V. Scalzotto;V. Scapin;C. Schultz;T. Schweizer;M. Shayduk;S. Shore;A. Sillanpaa;J. Sitarek;I. Šnidarić;D. Sobczynska;F. Spanier;S. Spiro;V. Stamatescu;A. Stamerra;B. Steinke;J. Storz;N. Strah;T. Suri'c;L. Takalo;H. Takami;F. Tavecchio;P. Temnikov;T. Terzi'c;D. Tescaro;M. Teshima;O. Tibolla;D. Torres;A. Treves;M. Uellenbeck;H. Vankov;P. Vogler;R. Wagner;Q. Weitzel;V. Zabalza;F. Zandanel;R. Zanin;K. Hirotani
中科院分区：
文献类型：
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作者：
M. C. J. Aleksi'c;E. Alvarez;L. A. Antonelli;P. Antoranz;M. Asensio;M. Backes;J. Barrio;D. Bastieri;J. Gonz'alez;W. Bednarek;A. Berdyugin;K. Berger;E. Bernardini;A. Biland;O. Blanch;R. Bock;A. Boller;G. Bonnoli;D. Tridon;I. Braun;T. Bretz;A. Cañellas;E. Carmona;A. Carosi;P. Colin;E. Colombo;J. Contreras;J. Cortina;L. Cossio;S. Covino;F. Dazzi;A. Angelis;G. Caneva;E. C. D. Pozo;B. Lotto;C. Mendez;A. Ortega;M. Doert;A. Domínguez;D. Prester;D. Dorner;M. Doro;D. Eisenacher;D. Elsaesser;D. Ferenc;M. V. Fonseca;L. Font;C. Fruck;R. L'opez;M. Garczarczyk;D. Garrido;G. Giavitto;N. Godinovi'c;D. Hadasch;D. Hafner;A. Herrero;D. Hildebrand;D. Hohne-Monch;J. Hose;D. Hrupec;T. Jogler;H. Kellermann;S. Klepser;T. Krahenbuhl;J. Krause;J. Kushida;A. Barbera;D. Lelas;E. Leonardo;E. Lindfors;S. Lombardi;M. L'opez;A. L'opez-Oramas;E. Lorenz;M. Makariev;G. Maneva;N. Mankuzhiyil;K. Mannheim;L. Maraschi;B. Marcote;M. Mariotti;M. Mart'inez;D. Mazin;M. Meucci;J. Miranda;R. Mirzoyan;J. Mold'on;A. Moralejo;P. Munar-Adrover;D. Nieto;K. Nilsson;R. Orito;N. Otte;I. Oya;D. Paneque;R. Paoletti;S. Pardo;J. Paredes;S. Partini;M. Pérez-Torres;M. Persic;L. Peruzzo;M. Pilia;J. Pochon;F. Prada;P. Moroni;E. Prandini;I. Gimenez;I. Puljak;I. Reichardt;R. Reinthal;W. Rhode;M. Rib'o;J. Rico;M. Rissi;S. Rugamer;A. Saggion;K. Saito;T. Saito;M. Salvati;K. Satalecka;V. Scalzotto;V. Scapin;C. Schultz;T. Schweizer;M. Shayduk;S. Shore;A. Sillanpaa;J. Sitarek;I. Šnidarić;D. Sobczynska;F. Spanier;S. Spiro;V. Stamatescu;A. Stamerra;B. Steinke;J. Storz;N. Strah;T. Suri'c;L. Takalo;H. Takami;F. Tavecchio;P. Temnikov;T. Terzi'c;D. Tescaro;M. Teshima;O. Tibolla;D. Torres;A. Treves;M. Uellenbeck;H. Vankov;P. Vogler;R. Wagner;Q. Weitzel;V. Zabalza;F. Zandanel;R. Zanin;K. Hirotani
本文报道了MAGIC I望远镜对蟹状星云脉冲星（PSR B 0532 +21）25 GeV以上γ射线的观测结果。使用了2007/2008年和2008/2009年冬季观测的两组数据。为了讨论从100 MeV到100 GeV的光谱形状，还分析了一年的公共费米大面积望远镜（Fermi-LAT）数据，以补充MAGIC数据。用费米-LAT数据确定的指数截止谱的外推与MAGIC测量不一致，这需要修改标准脉冲星发射模型。在25至100 GeV的能量范围内，P1相（主脉冲的位置在-0.06到0.04之间）和P2相（间脉冲的位置在0.32到0.43之间）的辐射可以用幂律来描述，其谱指数分别为-3.1 ± 1.0stat ± 0.3syst和-3.5 ± 0.5stat ± 0.3syst。假设脉冲形状为非对称洛仑兹函数，主脉冲和间脉冲的峰值位置估计在相位−0.009 ± 0.007和0.393 ± 0.009，而半峰全宽分别为0.025 ± 0.008和0.053 ± 0.015。
We report on the observation of γ-rays above 25 GeV from the Crab pulsar (PSR B0532+21) using the MAGIC I telescope. Two data sets from observations during the winter period 2007/2008 and 2008/2009 are used. In order to discuss the spectral shape from 100 MeV to 100 GeV, one year of public Fermi Large Area Telescope (Fermi-LAT) data are also analyzed to complement the MAGIC data. The extrapolation of the exponential cutoff spectrum determined with the Fermi-LAT data is inconsistent with MAGIC measurements, which requires a modification of the standard pulsar emission models. In the energy region between 25 and 100 GeV, the emission in the P1 phase (from −0.06 to 0.04, location of the main pulse) and the P2 phase (from 0.32 to 0.43, location of the interpulse) can be described by power laws with spectral indices of −3.1 ± 1.0stat ± 0.3syst and −3.5 ± 0.5stat ± 0.3syst, respectively. Assuming an asymmetric Lorentzian for the pulse shape, the peak positions of the main pulse and the interpulse are estimated to be at phases −0.009 ± 0.007 and 0.393 ± 0.009, while the full widths at half-maximum are 0.025 ± 0.008 and 0.053 ± 0.015, respectively.