MAGIC Collaboration, J. Aleksić, H. Anderhub, L. A. Antonelli, P. Antoranz, M. Backes, C. Baixeras, S. Balestra, J. A. Barrio, D. Bastieri, J. Becerra González,… 展开作者
MAGIC Collaboration, J. Aleksić, H. Anderhub, L. A. Antonelli, P. Antoranz, M. Backes, C. Baixeras, S. Balestra, J. A. Barrio, D. Bastieri, J. Becerra González, J. K. Becker, W. Bednarek, A. Berdyugin, K. Berger, E. Bernardini, A. Biland, R. K. Bock, G. Bonnoli, P. Bordas, D. Borla Tridon, V. Bosch-Ramon, D. Bose, I. Braun, T. Bretz, D. Britzger, M. Camara, E. Carmona, A. Carosi, P. Colin, S. Commichau, J. L. Contreras, J. Cortina, M. T. Costado, S. Covino, F. Dazzi, A. De Angelis, E. de Cea del Pozo, R. De los Reyes, B. De Lotto, M. De Maria, F. De Sabata, C. Delgado Mendez, M. Doert, A. Domínguez, D. Dominis Prester, D. Dorner, M. Doro, D. Elsaesser, M. Errando, D. Ferenc, E. Fernández, R. Firpo, M. V. Fonseca, L. Font, N. Galante, R. J. García López, M. Garczarczyk, M. Gaug, N. Godinovic, F. Goebel, D. Hadasch, A. Herrero, D. Hildebrand, D. Höhne-Mönch, J. Hose, D. Hrupec, C. C. Hsu, T. Jogler, S. Klepser, T. Krähenbühl, D. Kranich, A. La Barbera, A. Laille, E. Leonardo, E. Lindfors, S. Lombardi, F. Longo, M. López, E. Lorenz, P. Majumdar, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, M. Mariotti, M. Martínez, D. Mazin, M. Meucci, J. M. Miranda, R. Mirzoyan, H. Miyamoto, J. Moldón, M. Moles, A. Moralejo, D. Nieto, K. Nilsson, J. Ninkovic, R. Orito, I. Oya, R. Paoletti, J. M. Paredes, M. Pasanen, D. Pascoli, F. Pauss, R. G. Pegna, M. A. Perez-Torres, M. Persic, L. Peruzzo, F. Prada, E. Prandini, N. Puchades, I. Puljak, I. Reichardt, W. Rhode, M. Ribó, J. Rico, M. Rissi, S. Rügamer, A. Saggion, T. Y. Saito, M. Salvati, M. Sánchez-Conde, K. Satalecka, V. Scalzotto, V. Scapin, T. Schweizer, M. Shayduk, S. N. Shore, A. Sierpowska-Bartosik, A. Sillanpää, J. Sitarek, D. Sobczynska, F. Spanier, S. Spiro, A. Stamerra, B. Steinke, N. Strah, J. C. Struebig, T. Suric, L. Takalo, F. Tavecchio, P. Temnikov, D. Tescaro, M. Teshima, D. F. Torres, N. Turini, H. Vankov, R. M. Wagner, V. Zabalza, F. Zandanel, R. Zanin, J. Zapatero, A. de Ugarte-Postigo
备注：
6 pages, 1 figure. Astronomy & Astrophysics, in press. Revision affects only the author list.
Context: Gamma-ray bursts are cosmological sources emitting radiation from the gamma-rays to the radio band. Substantial observational efforts have been devoted to the study of gamma-ray bursts during the prompt phase, i.e. the initial burst of high-energy radiation, and during the long-lasting afterglows. In spite of many successes in interpreting these phenomena, there are still several open key questions about the fundamental emission processes, their energetics and the environment. Aim: Independently of specific gamma-ray burst theoretical recipes, spectra in the GeV/TeV range are predicted to be remarkably simple, being satisfactorily modeled with power-laws, and therefore offer a very valuable tool to probe the extragalactic background light distribution. Furthermore, the simple detection of a component at very-high energies, i.e. at $\sim 100$\,GeV, would solve the ambiguity about the importance of various possible emission processes, which provide barely distinguishable scenarios at lower energies. Methods: We used the results of the MAGIC telescope observation of the moderate resdhift ($z\sim0.76$) \object{GRB\,080430} at energies above about 80\,GeV, to evaluate the perspective for late-afterglow observations with ground based GeV/TeV telescopes. Results: We obtained an upper limit of $F_{\rm 95%\,CL} = 5.5 \times 10^{-11}$\,erg\,cm$^{-2}$\,s$^{-1}$ for the very-high energy emission of \object{GRB\,080430}, which cannot set further constraints on the theoretical scenarios proposed for this object also due to the difficulties in modeling the low-energy afterglow. Nonetheless, our observations show that Cherenkov telescopes have already reached the required sensitivity to detect the GeV/TeV emission of GRBs at moderate redshift ($z \lesssim 0.8$), provided the observations are carried out at early times, close to the onset of their afterglow phase.
VLBI and Archival VLA and WSRT Observations of the GRB 030329 Radio Afterglow
我们介绍VLBI和档案卡尔G。Jansky甚大阵列（VLA）和Westerbork综合射电望远镜（WSRT）对2003年3月29日伽马射线暴（GRB 030329）的射电余辉的观测，在爆发后672至2032天之间进行。EVLA和WSRT的数据表明，在5 GHz的通量简单的幂律衰减，没有任何明显的迹象，从反喷流的再亮。我们报告了一个未解决的来源，在2032天的大小$1.18\pm0.13$ mas，我们使用结合膨胀率的爆发，认为存在一个统一的，ISM样环爆介质。我们发展了一种半解析的方法来模拟伽马射线暴的余辉，并将其应用到5 GHz的光变曲线进行爆发量热。自行受到$< 0.067$ mas yr $^{-1}$的限制，支持伽马射线暴的标准余辉模型。
Photometric and late-time spectropolarimetric observations of GRB 250129A afterglow
University of Johannesburg（约翰内斯堡大学）；The George Washington University（乔治华盛顿大学）；National Institute for Theoretical and Computational Sciences (NITheCS)（国家理论与计算科学研究所）；University of the Free State（自由州大学）；Aryabhatta Research Institute of Observational Sciences（阿亚巴塔观测科学研究所）；University of Cape Town（开普敦大学）；South African Astronomical Observatory（南非天文台）
Overview of the results from extra-galactic observations with the MAGIC telescopes
活动星系核的非热喷流辐射在频率范围内有几个数量级。因此，观测方法需要多波长（MWL）活动，收集无线电，光学，紫外线，X射线，高能直到甚高能（VHE）伽马射线波段的数据。MAGIC是加那利群岛拉帕尔马Roque de los Muchachos天文台的一个由两台17米直径望远镜组成的系统，积极参与并组织MWL对已知和新发现的VHE源的观测。在这些会议记录中，我们报告了MAGIC河外观测的最新结果，该结果在时间变率研究和喷流排放模型方面获得了新的见解。
MAGIC是从地面探测50 GeV - 50 TeV能量范围内银河伽马射线天空的主要仪器之一。它由两个17米直径的成像大气切伦科夫望远镜组成，位于加那利群岛拉帕尔马的Roque de los Muchachos天文台。由于其出色的灵敏度，MAGIC对不同类型的银河系天体进行了相关研究。其中包括TeV能量的蟹状星云脉冲星、超新星遗迹仙后座A的光谱截止、LSI +61 303双星系统的超轨道变率、微类星体的搜寻、银河系中心的多年观测以及对未知HAWC源的后续研究。在许多情况下，这些观测结果挑战了我们对潜在发射机制的理解。在这里，我们回顾了MAGIC对这些星系源观测的最新结果。
MAGIC Telescopes observation of the BL Lac objects 1ES 1215+303 and 1ES 1218+304
两个BL Lac天体1 ES 1215+303和1 ES 1218+304，相隔0.8度，在2010-2011年用MAGIC切伦科夫望远镜观测到。2011年1月的观测结果是第一次探测到1 ES 1215+303（也称为ON-325）超过100 GeV，它在2010年10月被费米-LAT合作组织标记为有希望的甚高能（VHE，E > 100 GeV）伽马射线源候选者。2011年1月的观测是由Tuorla blazar监测计划报告的光源的高光学状态触发的。与2010年数据的比较表明，1 ES 1215+303也在VHE伽马射线中闪耀。此外，机会目标（ToO）的X射线观测表明，通量几乎是以前观测（2009年12月）的两倍。相反，1 ES 1218+304是一个众所周知的VHE伽马射线发射器，位于同一视场，然后与MAGIC同时观察。在这方面的贡献，我们提出了这两个VHE伽玛射线发射活动星系核的MAGIC观测的初步结果。
