超高能宇宙射线被Milky Way磁场偏转：它们能被校正得多好？
Deflections of ultra-high energy cosmic rays by the Milky Way magnetic field: how well can they be corrected?
摘要：
超高能宇宙射线（UHECR）源的定位仍然是现代天体物理学的一个难题。在寻找源的一个主要障碍是事实上，UHECR是由银河磁场（GMF）偏转。目前对GMF的了解是有限的，因为大多数实验测量跟踪视线-用于获得包括大随机分量的全球模型的最佳拟合参数的积分量。然而，盖亚时代的到来，伴随着对$\sim 10^9$恒星散射的测量，以及即将到来的大型偏振测量，使得GMF的3D测量第一次在原则上成为可能。这样的测量可以用来尝试重建个别UHECR通过银河系的轨迹，以纠正它们的偏转。出于这些发展，在目前的工作中，我们研究这样的校正的限制，通过检查其有效性如何取决于任何这样的未来磁场测量的不确定性。为此，我们模拟尝试重建的宇宙射线的轨迹，通过使用假设的测量的GMF，从两个最近更新的GMF模型收到的值的基础上。为了模拟三维测量的不确定性，分别为天空平面（POS）幅度，视线（LOS）幅度和POS方向引入这些值的随机误差。我们的研究结果突出了一个有效的校正是可以实现的条件。我们发现，有效性取决于粒子的刚度和到达方向，并可以根据所使用的GMF模型显着变化。
英文摘要：
Locating the sources of ultra-high energy cosmic rays (UHECRs) still remains a difficult puzzle for modern astrophysics. A major hurdle in the search for the sources is the fact that UHECRs are deflected by the Galactic magnetic field (GMF). Current knowledge of the GMF is limited, as most experimental measurements track line-of-sight--integrated quantities that are used to obtain best-fit parameters for global models including a large random component. The advent, however, of the Gaia era, with measurements of $\sim 10^9$ stellar parallaxes, in combination with upcoming large polarimetric surveys, make, for the first time, a 3D measurement of the GMF possible in principle. Such measurements can then be used to attempt a reconstruction of the trajectories of individual UHECRs through the Galaxy, in order to correct for their deflection. Motivated by these developments, in the present work, we study the limits of such a correction, by examining how its effectiveness depends on the uncertainty of any such future magnetic field measurements. To that end, we simulate attempts to reconstruct the trajectory of the cosmic ray by using hypothetical measurements of the GMF, based on values received from two recently updated GMF models. To simulate the uncertainty of a 3D measurement, random errors to these values are introduced separately for the plane-of-the-sky (POS) magnitude, the line-of-sight (LOS) magnitude and the POS direction. Our results highlight the conditions under which an effective correction is achievable. We find that the effectiveness is dependent on the particle rigidity and arrival direction, and can vary significantly depending on the GMF model used.
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