发表机构
Laboratoire Univers et Particules de Montpellier, Université de Montpellier, CNRS/IN2P3（蒙彼利埃宇宙与粒子实验室，蒙彼利埃大学，法国国家科学研究中心/法国国家核子与亚核子物理研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究评估H.E.S.S.和CTAO对脉冲星晕的探测能力，通过模拟数据和模板模型，证明CTAO能显著提升晕与二维高斯源的区分度，并量化弥散辐射对参数估计的影响。
AI 中文摘要
脉冲星晕是一类扩展的伽马射线源，由逃离脉冲星风云束缚的电子和正电子与周围光子发生逆康普顿散射而产生。HAWC首先在PSR J0633+1746和PSR B0656+14方向识别出此类源，越来越多的由脉冲星驱动的伽马射线源被提议作为候选晕。利用各向同性扩散模型，我们评估了当前及未来一代成像大气切伦科夫望远镜表征内银河系此类源物理性质的能力。我们在Gammapy库中构建了基于模板的脉冲星晕模型，并将其拟合到具有不同物理参数的模拟H.E.S.S.和CTAO数据中。这些源通过二维高斯分量进行了光谱形态学表征。我们通过模拟数据评估了晕模型与二维高斯假设之间的统计偏好，并量化了银河系弥散辐射的影响。多个晕参数可以同时被约束，包括脉冲星的真实年龄、其自行、扩散系数、注入粒子谱的谱指数以及注入效率。在某些情况下，H.E.S.S.阵列可以在统计上区分晕模型与包含二维高斯分量的模型，而CTAO则显示出显著改进。源的探测显著性随着银河系弥散辐射强度的增加而急剧降低。如果后者未使用数据生成模型进行建模，晕参数估计将产生偏差。物理动机驱动的脉冲星晕模型可以促进在高层次数据分析中对此类源的识别和表征。模拟的晕所展现的性质可能已经能在当前一代望远镜的巡天中仅用适度的观测时间被发现。
英文摘要
Pulsar halos are a class of extended gamma-ray sources, resulting from inverse Compton scattering of ambient photons by electrons and positrons believed to have escaped confinement in a pulsar wind nebula. First identified by HAWC towards PSR J0633+1746 and PSR B0656+14, a growing number of pulsar-powered gamma-ray sources is proposed as candidate halos. Using a model of isotropic diffusion, we assessed the ability of current-and-future generation imaging atmospheric Cherenkov telescopes to characterize the physical properties of such sources in the inner Galaxy. We constructed template-based pulsar halo models in the Gammapy library and fitted them to simulated H.E.S.S. and CTAO data of halos with different physical parameters. The sources were characterized spectro-morphologically using 2D Gaussian components. We assessed the statistical preference between the halo and 2D Gaussian hypotheses by the simulated data and quantified the impact of the diffuse Galactic emission. A multitude of the halos' parameters can be constrained simultaneously, including the pulsar's true age, its proper motion, the diffusion coefficient, the index of the injected particle spectrum and the injection efficiency. In some cases, the H.E.S.S. array can statistically distinguish between the halo model and a model containing 2D Gaussian components, while a significant improvement is seen with CTAO. The source's detection significance is drastically reduced with increasing intensity of the Galactic diffuse emission. If the latter is not modeled using the data-generating model, the halo parameter estimation is biased. A physically-motivated model of pulsar halos can facilitate the identification and characterization of this class of sources in high-level data analyses. The simulated halos exhibit properties that may already be found in surveys of current-generation telescopes with only a modest observation time.
CommentsTo be submitted for review soon
