MAGIC TeV gamma-ray observations of Markarian 421 during multiwavelength campaigns in 2006

MAGIC TeV gamma-ray observations of Markarian 421 during multiwavelength campaigns in 2006
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DOI：
10.1051/0004-6361/200913945
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发表时间：
2010-01
期刊：
Astronomy and Astrophysics
影响因子：
6.5
通讯作者：
M. C. J. Aleksi'c;L. A. Antonelli;P. Antoranz;Michael Backes;C. Baixeras;S. Balestra;J. Barrio;D. Bastieri;J. Gonz'alez;W. Bednarek;A. Berdyugin;K. Berger;E. Bernardini;A. Biland;R. Bock;G. Bonnoli;P. Bordas;D. Tridon;V. Bosch-Ramon;D. Bose;I. Braun;T. Bretz;D. Britzger;M. Cámara;E. Carmona;A. Carosi;P. Colin;S. Commichau;J. Contreras;J. Cortina;M. Costado;S. Covino;F. Dazzi;A. Angelis;E. C. D. Pozo;C. Mendez;R. Reyes;B. Lotto;M. D. Maria;F. D. Sabata;M. Doert;A. Domínguez;D. D. Prester-D.;D. Dorner;M. Doro;D. Elsaesser;M. Errando;D. Ferenc;M. V. Fonseca;L. Font;R. L'opez;M. Garczarczyk;M. Gaug;N. Godinovic;D. Hadasch;A. Herrero;D. Hildebrand;D. Hohne-Monch;J. Hose;D. Hrupec;C. Hsu;T. Jogler;S. Klepser;T. Krahenbuhl;D. Kranich;A. Barbera;A. Laille;E. Leonardo;E. Lindfors;S. Lombardi;F. Longo;M. L'opez;E. Lorenz;P. Majumdar;G. Maneva;N. Mankuzhiyil;K. Mannheim;L. Maraschi;M. Mariotti;M. Mart'inez;D. Mazin;M. Meucci;J. Miranda;R. Mirzoyan;H. Miyamoto;J. Mold'on;M. Molés;A. Moralejo;D. Nieto;K. Nilsson;J. Ninković;R. Orito;I. Oya;S. Paiano;R. Paoletti;J. Paredes;S. Partini;M. Pasanen;D. Pascoli;F. Pauss;R. Pegna;M. Pérez-Torres;M. Persic;L. Peruzzo;F. Prada;E. Prandini;N. Puchades;I. Puljak;I. Reichardt;W. Rhode;M. Rib'o;J. Rico;M. Rissi;S. Rugamer;A. Saggion;T. Saito;M. Salvati;M. S'anchez-Conde;K. Satalecka;V. Scalzotto;V. Scapin;C. Schultz;T. Schweizer;M. Shayduk;S. Shore;A. Sierpowska-Bartosik;A. Sillanpaa;J. Sitarek;D. Sobczynska;F. Spanier;S. Spiro;A. Stamerra;B. Steinke;J. Struebig;T. Surić;L. Takalo;F. Tavecchio;P. Temnikov;T. Terzić;D. Tescaro;M. Teshima;D. Torres;H. Vankov;R. Wagner;V. Zabalza;F. Zandanel;R. Z. Ifae;Edifici Cn.;Campus Uab;E-08193 Bellaterra;Spain.;I. I. F. Astrophysics-I.;I. Rome;Italy.;U. Complutense;E. Madrid;Technische Universitat Dortmund;D. Dortmund;H Germany;U. Barcelona;U. Padova;Infn;I-35131 Padova;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-102997450;E-38200 La Laguna;Tenerife;University of L'od'z;PL-90236 Lodz;Poland;T. Observatory;U. Turku;FI-21500 Piikkio;Finland.;D. Elektronen-Synchrotron;D. Zeuthen;E. Zurich;CH-8093 Switzerland;M. F. Physik;D-80805 Munchen;U. Barcelona;E. Barcelona;U. Wurzburg;D-97074 Wurzburg;Dept. Astrofisica;Universidad;E-38200 La Laguna;U. Udine;I. Trieste;I. 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;E. Granada;Croatian Magic Consortium;I. R. Bošković;University of Rijeka;University of Split;HR-10000 Zagreb;Croatia.;U. California;Davis;CA-95616-8677;Usa;U. Siena;I. Pisa;I-53100 Siena;Inst. for Nucl. Research;Nucl. Energy;BG-1784 Sofia;Bulgaria.;INAF-Osservatorio Astronomico;I. Trieste;Icrea;E. Barcelona;U. Pisa;I. Pisa
M. C. J. Aleksi'c;L. A. Antonelli;P. Antoranz;Michael Backes;C. Baixeras;S. Balestra;J. Barrio;D. Bastieri;J. Gonz'alez;W. Bednarek;A. Berdyugin;K. Berger;E. Bernardini;A. Biland;R. Bock;G. Bonnoli;P. Bordas;D. Tridon;V. Bosch-Ramon;D. Bose;I. Braun;T. Bretz;D. Britzger;M. Cámara;E. Carmona;A. Carosi;P. Colin;S. Commichau;J. Contreras;J. Cortina;M. Costado;S. Covino;F. Dazzi;A. Angelis;E. C. D. Pozo;C. Mendez;R. Reyes;B. Lotto;M. D. Maria;F. D. Sabata;M. Doert;A. Domínguez;D. D. Prester-D.;D. Dorner;M. Doro;D. Elsaesser;M. Errando;D. Ferenc;M. V. Fonseca;L. Font;R. L'opez;M. Garczarczyk;M. Gaug;N. Godinovic;D. Hadasch;A. Herrero;D. Hildebrand;D. Hohne-Monch;J. Hose;D. Hrupec;C. Hsu;T. Jogler;S. Klepser;T. Krahenbuhl;D. Kranich;A. Barbera;A. Laille;E. Leonardo;E. Lindfors;S. Lombardi;F. Longo;M. L'opez;E. Lorenz;P. Majumdar;G. Maneva;N. Mankuzhiyil;K. Mannheim;L. Maraschi;M. Mariotti;M. Mart'inez;D. Mazin;M. Meucci;J. Miranda;R. Mirzoyan;H. Miyamoto;J. Mold'on;M. Molés;A. Moralejo;D. Nieto;K. Nilsson;J. Ninković;R. Orito;I. Oya;S. Paiano;R. Paoletti;J. Paredes;S. Partini;M. Pasanen;D. Pascoli;F. Pauss;R. Pegna;M. Pérez-Torres;M. Persic;L. Peruzzo;F. Prada;E. Prandini;N. Puchades;I. Puljak;I. Reichardt;W. Rhode;M. Rib'o;J. Rico;M. Rissi;S. Rugamer;A. Saggion;T. Saito;M. Salvati;M. S'anchez-Conde;K. Satalecka;V. Scalzotto;V. Scapin;C. Schultz;T. Schweizer;M. Shayduk;S. Shore;A. Sierpowska-Bartosik;A. Sillanpaa;J. Sitarek;D. Sobczynska;F. Spanier;S. Spiro;A. Stamerra;B. Steinke;J. Struebig;T. Surić;L. Takalo;F. Tavecchio;P. Temnikov;T. Terzić;D. Tescaro;M. Teshima;D. Torres;H. Vankov;R. Wagner;V. Zabalza;F. Zandanel;R. Z. Ifae;Edifici Cn.;Campus Uab;E-08193 Bellaterra;Spain.;I. I. F. Astrophysics-I.;I. Rome;Italy.;U. Complutense;E. Madrid;Technische Universitat Dortmund;D. Dortmund;H Germany;U. Barcelona;U. Padova;Infn;I-35131 Padova;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-102997450;E-38200 La Laguna;Tenerife;University of L'od'z;PL-90236 Lodz;Poland;T. Observatory;U. Turku;FI-21500 Piikkio;Finland.;D. Elektronen-Synchrotron;D. Zeuthen;E. Zurich;CH-8093 Switzerland;M. F. Physik;D-80805 Munchen;U. Barcelona;E. Barcelona;U. Wurzburg;D-97074 Wurzburg;Dept. Astrofisica;Universidad;E-38200 La Laguna;U. Udine;I. Trieste;I. 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;E. Granada;Croatian Magic Consortium;I. R. Bošković;University of Rijeka;University of Split;HR-10000 Zagreb;Croatia.;U. California;Davis;CA-95616-8677;Usa;U. Siena;I. Pisa;I-53100 Siena;Inst. for Nucl. Research;Nucl. Energy;BG-1784 Sofia;Bulgaria.;INAF-Osservatorio Astronomico;I. Trieste;Icrea;E. Barcelona;U. Pisa;I. Pisa
中科院分区：
物理与天体物理2区
文献类型：
--
作者：
M. C. J. Aleksi'c;L. A. Antonelli;P. Antoranz;Michael Backes;C. Baixeras;S. Balestra;J. Barrio;D. Bastieri;J. Gonz'alez;W. Bednarek;A. Berdyugin;K. Berger;E. Bernardini;A. Biland;R. Bock;G. Bonnoli;P. Bordas;D. Tridon;V. Bosch-Ramon;D. Bose;I. Braun;T. Bretz;D. Britzger;M. Cámara;E. Carmona;A. Carosi;P. Colin;S. Commichau;J. Contreras;J. Cortina;M. Costado;S. Covino;F. Dazzi;A. Angelis;E. C. D. Pozo;C. Mendez;R. Reyes;B. Lotto;M. D. Maria;F. D. Sabata;M. Doert;A. Domínguez;D. D. Prester-D.;D. Dorner;M. Doro;D. Elsaesser;M. Errando;D. Ferenc;M. V. Fonseca;L. Font;R. L'opez;M. Garczarczyk;M. Gaug;N. Godinovic;D. Hadasch;A. Herrero;D. Hildebrand;D. Hohne-Monch;J. Hose;D. Hrupec;C. Hsu;T. Jogler;S. Klepser;T. Krahenbuhl;D. Kranich;A. Barbera;A. Laille;E. Leonardo;E. Lindfors;S. Lombardi;F. Longo;M. L'opez;E. Lorenz;P. Majumdar;G. Maneva;N. Mankuzhiyil;K. Mannheim;L. Maraschi;M. Mariotti;M. Mart'inez;D. Mazin;M. Meucci;J. Miranda;R. Mirzoyan;H. Miyamoto;J. Mold'on;M. Molés;A. Moralejo;D. Nieto;K. Nilsson;J. Ninković;R. Orito;I. Oya;S. Paiano;R. Paoletti;J. Paredes;S. Partini;M. Pasanen;D. Pascoli;F. Pauss;R. Pegna;M. Pérez-Torres;M. Persic;L. Peruzzo;F. Prada;E. Prandini;N. Puchades;I. Puljak;I. Reichardt;W. Rhode;M. Rib'o;J. Rico;M. Rissi;S. Rugamer;A. Saggion;T. Saito;M. Salvati;M. S'anchez-Conde;K. Satalecka;V. Scalzotto;V. Scapin;C. Schultz;T. Schweizer;M. Shayduk;S. Shore;A. Sierpowska-Bartosik;A. Sillanpaa;J. Sitarek;D. Sobczynska;F. Spanier;S. Spiro;A. Stamerra;B. Steinke;J. Struebig;T. Surić;L. Takalo;F. Tavecchio;P. Temnikov;T. Terzić;D. Tescaro;M. Teshima;D. Torres;H. Vankov;R. Wagner;V. Zabalza;F. Zandanel;R. Z. Ifae;Edifici Cn.;Campus Uab;E-08193 Bellaterra;Spain.;I. I. F. Astrophysics-I.;I. Rome;Italy.;U. Complutense;E. Madrid;Technische Universitat Dortmund;D. Dortmund;H Germany;U. Barcelona;U. Padova;Infn;I-35131 Padova;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-102997450;E-38200 La Laguna;Tenerife;University of L'od'z;PL-90236 Lodz;Poland;T. Observatory;U. Turku;FI-21500 Piikkio;Finland.;D. Elektronen-Synchrotron;D. Zeuthen;E. Zurich;CH-8093 Switzerland;M. F. Physik;D-80805 Munchen;U. Barcelona;E. Barcelona;U. Wurzburg;D-97074 Wurzburg;Dept. Astrofisica;Universidad;E-38200 La Laguna;U. Udine;I. Trieste;I. 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;E. Granada;Croatian Magic Consortium;I. R. Bošković;University of Rijeka;University of Split;HR-10000 Zagreb;Croatia.;U. California;Davis;CA-95616-8677;Usa;U. Siena;I. Pisa;I-53100 Siena;Inst. for Nucl. Research;Nucl. Energy;BG-1784 Sofia;Bulgaria.;INAF-Osservatorio Astronomico;I. Trieste;Icrea;E. Barcelona;U. Pisa;I. Pisa

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上下文。耀变体型活动星系核的宽范围光谱覆盖对于理解假定发生在其喷流中的粒子加速机制至关重要。主要大气伽马成像切伦科夫（MAGIC）望远镜参加了三次多波长（MWL）活动，在2006年4月28日和29日以及2006年6月14日的晚上观测了马尔卡良（Mkn） 421。目标。我们分析了2006年4月22日至30日和2006年6月14日9个晚上的MAGIC超高能观测数据。我们用亚日分辨率和逐夜能量光谱推断光曲线。方法。MAGIC通过观察大气中延伸的空气阵雨来探测伽马射线。使用标准MAGIC分析链对获得的风淋室图像进行分析。结果。在所有的观测夜晚都从Mkn 421探测到强烈的伽马射线信号。2006年4月的通量（E > 250 GeV）在（0.92 +/- 0.11）× 10(-10) cm(-2) s(-1) （0.57 Crab单位）和（3.21 +/- 0.15）× 10(-10) cm(-2) s(-1) （2.0 Crab单位）之间逐夜变化。在2006年4月29日晚上，有一个明显的夜间变异性的迹象，时间增加了一倍，为36 +/- 10(stat) min，再次为这个天体建立了快速的通量变异性。所有夜晚的伽马射线能谱都可以推断出来，幂律指数在1.66到2.47之间。我们没有发现光谱指数和单个夜晚的通量状态之间有统计学意义的相关性。在2006年6月的活动中，发现了一个远低于四天后惠普尔10米望远镜测量到的通量。利用对数抛物线型幂律拟合，我们推导出了一些数据集在高能区光谱峰的位置。我们的结果证实了随着通量增加峰值能量上升的迹象，正如轻子加速模型所预期的那样。
Context. Wide-range spectral coverage of blazar-type active galactic nuclei is of paramount importance for understanding the particle acceleration mechanisms assumed to take place in their jets. The Major Atmospheric Gamma Imaging Cerenkov (MAGIC) telescope participated in three multiwavelength (MWL) campaigns, observing the blazar Markarian (Mkn) 421 during the nights of April 28 and 29, 2006, and June 14, 2006. Aims. We analyzed the corresponding MAGIC very-high energy observations during 9 nights from April 22 to 30, 2006 and on June 14, 2006. We inferred light curves with sub-day resolution and night-by-night energy spectra. Methods. MAGIC detects gamma-rays by observing extended air showers in the atmosphere. The obtained air-shower images were analyzed using the standard MAGIC analysis chain. Results. A strong gamma-ray signal was detected from Mkn 421 on all observation nights. The flux (E > 250 GeV) varied on night-by-night basis between (0.92 +/- 0.11) x 10(-10) cm(-2) s(-1) (0.57 Crab units) and (3.21 +/- 0.15) x 10(-10) cm(-2) s(-1) (2.0 Crab units) in April 2006. There is a clear indication for intra-night variability with a doubling time of 36 +/- 10(stat) min on the night of April 29, 2006, establishing once more rapid flux variability for this object. For all individual nights gamma-ray spectra could be inferred, with power-law indices ranging from 1.66 to 2.47. We did not find statistically significant correlations between the spectral index and the flux state for individual nights. During the June 2006 campaign, a flux substantially lower than the one measured by the Whipple 10-m telescope four days later was found. Using a log-parabolic power law fit we deduced for some data sets the location of the spectral peak in the very-high energy regime. Our results confirm the indications of rising peak energy with increasing flux, as expected in leptonic acceleration models.