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首页> 外文会议>Session of the Sant Cugat Forum on Astrophysics >Cosmic Ray Acceleration in W51C Observed with the MAGIC Telescopes
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Cosmic Ray Acceleration in W51C Observed with the MAGIC Telescopes

机译：用魔术望远镜观察W51C中的宇宙射线加速度

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We present the observations of the W51 complex with the MAGIC telescopes. After collecting more than 50 h of good quality data, we are able to measure the energy spectrum between 75 GeV and 5.5 TeV, and to lit it with a single power law with an index of 2.58 ± 0.07_(stat) ± 0.22_(syst). We look for underlying structures by means of detailed morphological studies that allow us to locate the majority of the emission around the interaction point between W51C and W51B, where shocked molecular and atomic gas is found. We also find a feature extending towards the pulsar wind nebula candidate CXO .1192318.5 + 140305. The possible contribution of this pulsar wind nebula candidate, assuming a point-like source adds up to 20% of the overall emission. The broad band spectral energy distribution of the whole gamma-ray source can be explained with a simple hadronic model that implies proton acceleration at least up to 100TeV. The outcome of the modeling, together with the morphology of the source, suggests that we indeed observe ongoing acceleration of ions in the interaction zone between supernova remnant and cloud.
机译：我们向魔术望远镜展示了W51复合物的观察。收集超过50小时的高质量数据后，我们能够测量75 GEV和5.5 TEV之间的能谱，并用单一的电源律点亮，指数为2.58±0.07_（统计）±0.22_（系统）。我们通过详细的形态学研究寻找潜在的结构，使我们能够找到W51C和W51B之间的相互作用点周围的大部分发射，其中发现震动的分子和原子气体。我们还发现朝向Pulsar Wind Gebula候选CXO .1192318.5 + 140305的功能。这种脉冲星风云星云候选人的可能贡献，假设点状源增加了最多20％的整体排放。整个伽马射线源的宽带光谱能量分布可以用简单的辐射模型来解释，其意味着质子加速度至少高达100秒。建模的结果与来源的形态，表明我们确实观察了超新星残余和云之间的相互作用区中的离子的持续加速。

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