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arXiv 2202.08875astro-ph.HEastro-ph.COhep-ph
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磁场模型如何影响轻类轴子粒子的天体物理极限？使用NGC 1275的X射线案例研究

How do Magnetic Field Models Affect Astrophysical Limits on Light Axion-like Particles? An X-ray Case Study with NGC 1275

James H. Matthews, Christopher S. Reynolds, M. C. David Marsh, Júlia Sisk-Reynés, Payton E. Rodman

备注：
17 pages, 9 figures, 2 tables. Accepted for publication in The Astrophysical Journal. ALPro code available at https://github.com/jhmatthews/alpro with accompanying documentation, as well as notebooks and data for reproducing the main results
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摘要：

类轴子粒子（Axion-like particles，ALP）是粒子物理学标准模型的一个很好的扩展，目前对活动星系核（AGN）的X射线观测对ALP与电磁场的耦合（$g_{a γ}$）提出了最严格的限制，特别是对于非常轻的ALP（$m_a\lesssim10^{-11}$ eV）。我们重新审视了Reynolds等人（2020）使用NGC 1275（英仙座星系团的中心AGN）的Chandra X射线光栅光谱学获得的限制，检查X射线光谱模型和磁场模型的影响。我们还提出了一个新的公开可用的代码，ALPro，我们用它来解决ALP传播问题。我们讨论了英仙座湍流磁场的证据，并表明，它可以是重要的解决尺度低于相干长度的磁场结构。我们重新分析了NGC 1275 X射线光谱使用改进的数据处理和基线光谱模型。我们发现的限制是不敏感的部分覆盖的吸收体是否被用于配合。在低$m_a$（$m_a\lesssim10^{-13}$ eV）下，与Reynolds等人（2020）的模型B相比，我们发现不同磁场模型对$g_{a γ}$（通过$0.1-0.3$ dex）的限制略弱。设计用于模拟$\sim50$ kpc尺度相干结构的高斯随机场（GRF）模型也仅导致稍微弱的限制。我们的结论是，现有的模型B的限制是强大的假设$β_{\rm pl}\approx100$，是不敏感的细胞为基础的方法或GRF使用。然而，天体物理学的不确定性的强度和结构的集群磁场持续存在，激发高灵敏度RM观测和更严格的约束径向轮廓的$β_{\rm pl}$。

英文摘要：

Axion-like particles (ALPs) are a well-motivated extension to the standard model of particle physics, and X-ray observations of cluster-hosted AGN currently place the most stringent constraints on the ALP coupling to electromagnetism, $g_{a γ}$, for very light ALPs ($m_a\lesssim10^{-11}$ eV). We revisit limits obtained by Reynolds et al. (2020) using Chandra X-ray grating spectroscopy of NGC 1275, the central AGN in the Perseus cluster, examining the impact of the X-ray spectral model and magnetic field model. We also present a new publicly available code, ALPro, which we use to solve the ALP propagation problem. We discuss evidence for turbulent magnetic fields in Perseus and show that it can be important to resolve the magnetic field structure on scales below the coherence length. We re-analyse the NGC 1275 X-ray spectra using an improved data reduction and baseline spectral model. We find the limits are insensitive to whether a partially covering absorber is used in the fits. At low $m_a$ ($m_a\lesssim10^{-13}$ eV), we find marginally weaker limits on $g_{a γ}$ (by $0.1-0.3$ dex) with different magnetic field models, compared to Model B from Reynolds et al. (2020). A Gaussian random field (GRF) model designed to mimic $\sim50$ kpc scale coherent structures also results in only slightly weaker limits. We conclude that the existing Model B limits are robust assuming that $β_{\rm pl}\approx100$, and are insensitive to whether cell-based or GRF methods are used. However, astrophysical uncertainties regarding the strength and structure of cluster magnetic fields persist, motivating high sensitivity RM observations and tighter constraints on the radial profile of $β_{\rm pl}$.

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