在57 $\times$ 10^{18} eV以上观测到的最亮cosmic-ray源的特征角尺寸的一种约束方法
A method to constrain the characteristic angular size of the brightest cosmic-ray sources observed above 57 $\times$ 10^{18} eV
摘要：
我们介绍了一种方法来限制观察到的最亮的宇宙射线源以上57 \times 1018 eV的特征角大小。源的角大小，我们指的是来自该源的宇宙射线到达地球的有效角范围。该方法基于宇宙射线到达方向的小尺度（< 10 \circ）自聚类。该方法适用于稀疏数据集，其中强本地化的CR* 方向尚未观察到。我们表明，有用的约束源的大小可以在不久的将来，这些约束并不强烈依赖于假设的空间分布和宇宙射线源的光度函数。我们认为，源大小的指示是很有说服力的。例如，源大小的指示可用于推断粒子电荷和介入磁场的限制（不是独立的），这两者到目前为止都没有很好地约束。这是可能的，因为源的大小在尺度上与磁偏转相似。
英文摘要：
We introduce a method to constrain the characteristic angular size of the brightest cosmic-ray sources observed above 57 \times 1018 eV. By angular size of a source, we mean the effective angular extent over which cosmic-rays from that source arrive at earth. The method is based on the small-scale (< 10\circ) self-clustering of cosmic-ray arrival directions. The method is applicable to sparse data sets in which strong localizations of CR* directions are not yet observed. We show that useful constraints on the source size can be made in the near future and that these constraints are not strongly dependent on the assumed spatial distribution and luminosity function of the cosmic-ray sources. We suggest that an indication of the source size is quite telling. For example, an indication of the source size can be used to infer limits on the particle charge and intervening magnetic fields (not independently), both of which are not well constrained so far. This is possible because the source size is similar in scale to the magnetic deflection.
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