2016年Blazar 1ES 1ES 1ES 1ES 1ES 1ES的宽带表征

论文标题

2016年Blazar 1ES 1ES 1ES 1ES 1ES 1ES的宽带表征

Broadband characterisation of the very intense TeV flares of the blazar 1ES 1959+650 in 2016

论文作者

MAGIC Collaboration, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Baack, D., Babić, A., Banerjee, B., de Almeida, U. Barres, Barrio, J. A., González, J. Becerra, Bednarek, W., Bellizzi, L., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bosnjak, Z., Busetto, G., Carosi, R., Ceribella, G., Chai, Y., Cikota, S., Colak, S. M., Colin, U., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Espiñeira, E. Do Souto, Prester, D. Dominis, Donini, A., Dorner, D., Doro, M., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Fernández-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., Gallozzi, S., López, R. J. García, Garczarczyk, M., Gasparyan, S., Gaug, M., Godinović, N., Green, D., Guberman, D., Hadasch, D., Hahn, A., Herrera, J., Hoang, J., Hrupec, D., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jouvin, L., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Coto, R., López-Oramas, A., Fraga, B. Machado de Oliveira, Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Mićanović, S., Miceli, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Niedzwiecki, A., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Nöthe, M., Nozaki, S., Paiano, S., Palacio, J., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Peñil, P., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Somero, A., Stamerra, A., Strom, D., Strzys, M., Surić, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tsujimoto, S., van Scherpenberg, J., Vanzo, G., Acosta, M. Vazquez, Vovk, I., Will, M., Zarić, D., Collaboration, Fermi-LAT, :, Hayashida, M.

论文摘要

1ES 1959+650是一个明亮的TEV高频式BL LAC对象，具有有趣的功能，例如“孤儿” TEV耀斑和高能策略中的广泛排放，很难使用常规的单区域同步自我自我自我compton（SSC）风景来解释。我们报告了2016年主要的大气伽马成像Cherenkov（Magic）观察结果，以及Fermi大面积望远镜（LAT）和Swift Instruments的多波长数据。魔术观察到1ES 1959+650在2016年的高能（VHE，E> 100 GEV）伽马射线频段中具有不同排放水平的魔术。在长期数据中，随着通量的增加，X射线频谱变得更加困难，并且在VHE频段中也可以看到类似趋势的提示。 2016年6月13日，6月14日和1日，通过魔术测量了蟹状通量的极高的VHE通量，达到了蟹状通量的3倍（观察到自2002年以来最高的通量）。在这些耀斑期间，光谱能分布（SED）的高能峰位于VHE结构域中，延伸至几个TEV。伽马射线（Fermi-Lat和VHE频段）和X射线频带的频谱非常困难。 2016年6月13日和2016年7月1日，消息来源显示了不到一个小时的时间范围内VHE通量的迅速变化。一个简单的单区SSC模型可以在需要多普勒因子中等至高值的耀斑期间描述数据（> = 30-60）。或者，SED的高能量峰可以通过纯种模型来解释，该模型归因于质子合成的辐射，其质子合成辐射具有JET POWER L_ {JET} 〜10^10^{46} ERG/s，并在磁场强度（〜100 g）的高值（〜100 g）和最大Proton Energy（〜D Proton EVER（〜几乎））中。混合的Lepto-Hadronic模型需要喷射功率的超级埃德丁顿值。我们得出的结论是，在2016年极端的爆炸期间，很难从源头中获得可检测到的中微子排放。

1ES 1959+650 is a bright TeV high-frequency-peaked BL Lac object exhibiting interesting features like "orphan" TeV flares and a broad emission in the high-energy regime, that are difficult to interpret using conventional one-zone Synchrotron Self-Compton (SSC) scenarios. We report the results from the Major Atmospheric Gamma Imaging Cherenkov (MAGIC) observations in 2016 along with the multi-wavelength data from the Fermi Large Area Telescope (LAT) and Swift instruments. MAGIC observed 1ES 1959+650 with different emission levels in the very-high-energy (VHE, E >100 GeV) gamma-ray band during 2016. In the long-term data, the X-ray spectrum becomes harder with increasing flux and a hint of a similar trend is also visible in the VHE band. An exceptionally high VHE flux reaching ~ 3 times the Crab Nebula flux was measured by MAGIC on the 13th, 14th of June and 1st July 2016 (the highest flux observed since 2002). During these flares, the high-energy peak of the spectral energy distribution (SED) lies in the VHE domain and extends up to several TeV. The spectrum in the gamma-ray (both Fermi-LAT and VHE bands) and the X-ray bands are quite hard. On 13th June and 1st July 2016, the source showed rapid variations of the VHE flux within timescales of less than an hour. A simple one-zone SSC model can describe the data during the flares requiring moderate to high values of the Doppler factors (>=30-60). Alternatively, the high-energy peak of the SED can be explained by a purely hadronic model attributed to proton-synchrotron radiation with jet power L_{jet}~10^{46} erg/s and under high values of the magnetic field strength (~100 G) and maximum proton energy (~few EeV). Mixed lepto-hadronic models require super-Eddington values of the jet power. We conclude that it is difficult to get detectable neutrino emission from the source during the extreme VHE flaring period of 2016.

下载PDF全文

下载文献需遵守相关版权规定

论文标题