Detection of very-high energy γ -ray emission from NGC 1275 by the MAGIC telescopes

Detection of very-high energy γ -ray emission from NGC 1275 by the MAGIC telescopes
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DOI：
10.1051/0004-6361/201118668
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发表时间：
2012
期刊：
Science and Technology of Advanced Materials
影响因子：
5.5
通讯作者：
M. C. J. Aleksi'c;E. Alvarez;L. A. Antonelli;P. Antoranz;M. Asensio;Michael Backes;U. D. Almeida;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. D. Prester-D.;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;S. Gozzini;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;N. Lewandowska;E. Lindfors;S. Lombardi;M. L'opez;R. L'opez-Coto;A. L'opez-Oramas;E. Lorenz;M. Makariev;G. Maneva;N. Mankuzhiyil;K. Mannheim;L. Maraschi;M. Mariotti;M. Mart'inez;D. Mazin;M. Meucci;J. Miranda;R. Mirzoyan;J. Mold'on;A. Moralejo;P. Munar-Adrover;A. Niedźwiecki;D. Nieto;K. Nilsson;N. Nowak;R. Orito;S. Paiano;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;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;S. Sun;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;C. Pfrommer;A. P. Ifae;Edifici Cn.;Campus Uab;Bellaterra;Spain.;U. Complutense;Madrid;I. I. F. Astrophysics-I.;Romé;Italy.;U. Siena;I. Pisa;Siena;Technische Universitat Dortmund;Dortmund;H Germany;M. F. Physik;Munchen;U. Padova;Infn;Padova;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-102997450;La Laguna;Tenerife;D. Astrof'isica;U. L. Laguna;University of L'od'z;Lodz;Poland;T. Observatory;U. Turku;Piikkio;Finland.;D. Elektronen-Synchrotron;Zeuthen;E. Zurich;Zurich;Switzerland.;U. Wurzburg;Wurzburg;U. Barcelona;Barcelona;U. Udine;I. Trieste;Udine;Institut de Ci'encies de l'Espai-Institut-de-Ci'encies-de-l'Espai-123080358;Inst. de Astrof'isica de Andaluc'ia-Inst.-de-Astrof'isica-de-Andaluc'ia-102813830;Granada;Croatian Magic Consortium;Rudjer Boskovic Institute;University of Rijeka;University of Split;Zagreb;Croatia.;U. Barcelona;Inst. for Nucl. Research;Nucl. Energy;Sofía;Bulgaria.;INAF-Osservatorio Astronomico;Trieste;Universita' dell'Insubria;Como;U. Pisa;Pisa;Icrea;N. C. E. P. F. D. Lausanne;Lausanne;supported by Infn Padova;Now at Centro de Investigaciones Energ'eticas;Medioambientales y Tecnol'ogicas;N. Eso;Hits;Heidelberg;U. Barbara;Santa Barbara;Ca;Usa
M. C. J. Aleksi'c;E. Alvarez;L. A. Antonelli;P. Antoranz;M. Asensio;Michael Backes;U. D. Almeida;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. D. Prester-D.;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;S. Gozzini;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;N. Lewandowska;E. Lindfors;S. Lombardi;M. L'opez;R. L'opez-Coto;A. L'opez-Oramas;E. Lorenz;M. Makariev;G. Maneva;N. Mankuzhiyil;K. Mannheim;L. Maraschi;M. Mariotti;M. Mart'inez;D. Mazin;M. Meucci;J. Miranda;R. Mirzoyan;J. Mold'on;A. Moralejo;P. Munar-Adrover;A. Niedźwiecki;D. Nieto;K. Nilsson;N. Nowak;R. Orito;S. Paiano;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;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;S. Sun;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;C. Pfrommer;A. P. Ifae;Edifici Cn.;Campus Uab;Bellaterra;Spain.;U. Complutense;Madrid;I. I. F. Astrophysics-I.;Romé;Italy.;U. Siena;I. Pisa;Siena;Technische Universitat Dortmund;Dortmund;H Germany;M. F. Physik;Munchen;U. Padova;Infn;Padova;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-102997450;La Laguna;Tenerife;D. Astrof'isica;U. L. Laguna;University of L'od'z;Lodz;Poland;T. Observatory;U. Turku;Piikkio;Finland.;D. Elektronen-Synchrotron;Zeuthen;E. Zurich;Zurich;Switzerland.;U. Wurzburg;Wurzburg;U. Barcelona;Barcelona;U. Udine;I. Trieste;Udine;Institut de Ci'encies de l'Espai-Institut-de-Ci'encies-de-l'Espai-123080358;Inst. de Astrof'isica de Andaluc'ia-Inst.-de-Astrof'isica-de-Andaluc'ia-102813830;Granada;Croatian Magic Consortium;Rudjer Boskovic Institute;University of Rijeka;University of Split;Zagreb;Croatia.;U. Barcelona;Inst. for Nucl. Research;Nucl. Energy;Sofía;Bulgaria.;INAF-Osservatorio Astronomico;Trieste;Universita' dell'Insubria;Como;U. Pisa;Pisa;Icrea;N. C. E. P. F. D. Lausanne;Lausanne;supported by Infn Padova;Now at Centro de Investigaciones Energ'eticas;Medioambientales y Tecnol'ogicas;N. Eso;Hits;Heidelberg;U. Barbara;Santa Barbara;Ca;Usa
中科院分区：
材料科学2区
文献类型：
--
作者：
M. C. J. Aleksi'c;E. Alvarez;L. A. Antonelli;P. Antoranz;M. Asensio;Michael Backes;U. D. Almeida;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. D. Prester-D.;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;S. Gozzini;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;N. Lewandowska;E. Lindfors;S. Lombardi;M. L'opez;R. L'opez-Coto;A. L'opez-Oramas;E. Lorenz;M. Makariev;G. Maneva;N. Mankuzhiyil;K. Mannheim;L. Maraschi;M. Mariotti;M. Mart'inez;D. Mazin;M. Meucci;J. Miranda;R. Mirzoyan;J. Mold'on;A. Moralejo;P. Munar-Adrover;A. Niedźwiecki;D. Nieto;K. Nilsson;N. Nowak;R. Orito;S. Paiano;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;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;S. Sun;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;C. Pfrommer;A. P. Ifae;Edifici Cn.;Campus Uab;Bellaterra;Spain.;U. Complutense;Madrid;I. I. F. Astrophysics-I.;Romé;Italy.;U. Siena;I. Pisa;Siena;Technische Universitat Dortmund;Dortmund;H Germany;M. F. Physik;Munchen;U. Padova;Infn;Padova;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-102997450;La Laguna;Tenerife;D. Astrof'isica;U. L. Laguna;University of L'od'z;Lodz;Poland;T. Observatory;U. Turku;Piikkio;Finland.;D. Elektronen-Synchrotron;Zeuthen;E. Zurich;Zurich;Switzerland.;U. Wurzburg;Wurzburg;U. Barcelona;Barcelona;U. Udine;I. Trieste;Udine;Institut de Ci'encies de l'Espai-Institut-de-Ci'encies-de-l'Espai-123080358;Inst. de Astrof'isica de Andaluc'ia-Inst.-de-Astrof'isica-de-Andaluc'ia-102813830;Granada;Croatian Magic Consortium;Rudjer Boskovic Institute;University of Rijeka;University of Split;Zagreb;Croatia.;U. Barcelona;Inst. for Nucl. Research;Nucl. Energy;Sofía;Bulgaria.;INAF-Osservatorio Astronomico;Trieste;Universita' dell'Insubria;Como;U. Pisa;Pisa;Icrea;N. C. E. P. F. D. Lausanne;Lausanne;supported by Infn Padova;Now at Centro de Investigaciones Energ'eticas;Medioambientales y Tecnol'ogicas;N. Eso;Hits;Heidelberg;U. Barbara;Santa Barbara;Ca;Usa

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本文报道了英仙座星系团中央射电星系NGC 1275的甚高能（VHE，E > 100 GeV）γ射线辐射的探测结果。MAGIC望远镜探测到了这个源，统计意义为6。在2010年8月至2011年2月进行的46小时立体观测中，6 σ超过100 GeV。在70 GeV和500 GeV之间测量到的能谱可以用幂律来描述，其陡峭的谱指数为Γ = − 4。1 ± 0。7 stat ± 0 . 3系统，100 GeV以上的平均X射线为F γ =（1 . 3 ± 0。2静态± 0。3系统）× 10 − 11 cm − 2 s − 1。这些结果与费米-LAT在前两年观测中测得的100 MeV以上的幂律谱相结合，谱指数为Γ（cid：3）− 2。1，强烈表明在NGC 1275光谱中存在数十GeV的断裂或截止。100 GeV以上的源的光变曲线在一个月的时间尺度上没有显示出变化的迹象。最后，我们报告的非检测在目前的数据的射电星系IC 310，以前发现的费米-LAT和MAGIC。导出的双曲上限FU。L .γ（> 300 GeV）= 1。2 × 10 − 12 cm − 2 s − 1比MAGIC在2009年10月至2010年2月间测得的平均λ ux低103倍，从而证实了VHE源的年时间尺度变化。
We report on the detection of very-high energy (VHE, E > 100 GeV) γ -ray emission from NGC 1275, the central radio galaxy of the Perseus cluster of galaxies. The source has been detected by the MAGIC telescopes with a statistical significance of 6 . 6 σ above 100 GeV in 46 h of stereo observations carried out between August 2010 and February 2011. The measured di ff erential energy spectrum between 70 GeV and 500 GeV can be described by a power law with a steep spectral index of Γ = − 4 . 1 ± 0 . 7 stat ± 0 . 3 syst , and the average flux above 100 GeV is F γ = (1 . 3 ± 0 . 2 stat ± 0 . 3 syst ) × 10 − 11 cm − 2 s − 1 . These results, combined with the power-law spectrum measured in the first two years of observations by the Fermi -LAT above 100 MeV, with a spectral index of Γ (cid:3) − 2 . 1, strongly suggest the presence of a break or cut-o ff around tens of GeV in the NGC 1275 spectrum. The light curve of the source above 100 GeV does not show hints of variability on a month time scale. Finally, we report on the nondetection in the present data of the radio galaxy IC 310, previously discovered by the Fermi -LAT and MAGIC. The derived flux upper limit F U . L . γ ( > 300 GeV) = 1 . 2 × 10 − 12 cm − 2 s − 1 is a factor ∼ 3 lower than the mean flux measured by MAGIC between October 2009 and February 2010, thus confirming the year time-scale variability of the source at VHE.