MAGIC 测得的 NGC 1275 在 2016-2017 年的伽马射线耀发活动
高能天体物理现象
2018-09-26 v1
摘要
我们报告利用 MAGIC 望远镜在甚高能（VHE，E 100 GeV）伽马射线波段探测到 Fanaroff-Riley I 型射电星系 NGC 1275 的耀发活动。观测于 2016 年 9 月至 2017 年 2 月作为监测项目的一部分进行。最明亮的爆发发生在 2016 年 12 月 31 日至 2017 年 1 月 1 日夜间，其高于 100 GeV 的通量约为蟹状星云通量（C.U.）的 倍（比 2009 至 2011 年间两次观测活动所测平均通量高五十倍）。测得逐日光变曲线存在显著变率，最短通量倍增时间尺度为 分钟。MAGIC 数据在最强耀发态与 Fermi-LAT around 2017 年 1 月 1 日前后同步数据的合并能谱遵循带指数截断的幂律，截断能量为 GeV。同时给出了用 KVA 望远镜在 R 波段获得的同步光学通量密度测量，并研究了光学与伽马射线辐射之间的相关性。由于可能的内部对产生，快速通量变率将多普勒因子限制为与射电波段观测到的大视角不一致的值。我们研究了用于解释快速伽马射线变率的不同情形，即来自：磁层间隙、在喷流中传播的相对论性团块（迷你喷流）或进入喷流的外部云（或恒星）的辐射。我们发现，在此观测到的光度唯一合理的模型是，仅当穿过多普勒黑洞的磁场从其与吸积流气体压力平衡的值增强时，才在中心黑洞周围的磁层间隙中产生伽马射线。
引用
@article{arxiv.1806.01559,
title = {Gamma-ray flaring activity of NGC 1275 in 2016-2017 measured by MAGIC},
author = {MAGIC collaboration and S. Ansoldi and L. A. Antonelli and C. Arcaro and D. Baack and A. Babić and B. Banerjee and P. Bangale and U. Barres de Almeida and J. A. Barrio and J. Becerra González and W. Bednarek and E. Bernardini and R. Ch. Berse and A. Berti and W. Bhattacharyya and C. Bigongiari and A. Biland and O. Blanch and G. Bonnoli and R. Carosi and G. Ceribella and A. Chatterjee and S. M. Colak and P. Colin and E. Colombo and J. L. Contreras and J. Cortina and S. Covino and P. Cumani and V. D'Elia and P. Da Vela and F. Dazzi and A. De Angelis and B. De Lotto and M. Delfino and J. Delgado and F. Di Pierro and A. Domínguez and D. Dominis Prester and D. Dorner and M. Doro and S. Einecke and D. Elsaesser and V. Fallah Ramazani and A. Fattorini and A. Fernández-Barral and G. Ferrara and D. Fidalgo and L. Foffano and M. V. Fonseca and L. Font and C. Fruck and D. Galindo and S. Gallozzi and R. J. García López and M. Garczarczyk and M. Gaug and P. Giammaria and N. Godinović and D. Gora and D. Guberman and D. Hadasch and A. Hahn and T. Hassan and M. Hayashida and J. Herrera and J. Hoang and J. Hose and D. Hrupec and K. Ishio and Y. Konno and H. Kubo and J. Kushida and A. Lamastra and D. Lelas and F. Leone and E. Lindfors and S. Lombardi and F. Longo and M. López and C. Maggio and P. Majumdar and M. Makariev and G. Maneva and M. Manganaro and K. Mannheim and L. Maraschi and M. Mariotti and M. Martínez and S. Masuda and D. Mazin and K. Mielke and M. Minev and J. M. Miranda and R. Mirzoyan and A. Moralejo and V. Moreno and E. Moretti and T. Nagayoshi and V. Neustroev and A. Niedzwiecki and M. Nievas Rosillo and C. Nigro and K. Nilsson and D. Ninci and K. Nishijima and K. Noda and L. Nogués and S. Paiano and J. Palacio and D. Paneque and R. Paoletti and J. M. Paredes and G. Pedaletti and P. Peñil and M. Peresano and M. Persic and K. Pfrang and P. G. Prada Moroni and E. Prandini and I. Puljak and J. R. Garcia and I. Reichardt and W. Rhode and M. Ribó and J. Rico and C. Righi and A. Rugliancich and L. Saha and T. Saito and K. Satalecka and T. Schweizer and J. Sitarek and I. Šnidarić and D. Sobczynska and A. Stamerra and M. Strzys and T. Surić and M. Takahashi and F. Tavecchio and P. Temnikov and T. Terzić and M. Teshima and N. Torres-Albà and S. Tsujimoto and G. Vanzo and M. Vazquez Acosta and I. Vovk and J. E. Ward and M. Will and D. Zarić and D. Glawion and L. O. Takalo and J. Jormanainen},
journal= {arXiv preprint arXiv:1806.01559},
year = {2018}
}
备注
accepted for publications in Astronomy and Astrophysics