发表机构
State Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences; Department of Physics and Astronomy, University of Notre Dame（中国科学院高能物理研究所粒子天体物理国家重点实验室; 圣母大学物理与天文系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文提出HESS J1507-622是一个年轻的银河系千新星遗迹，通过轻子逆康普顿散射模型解释其GeV-TeV辐射，并推断其距离和年龄，为验证该假说提供了多波长观测前景。
AI 中文摘要
HESS J1507$-$622是H.E.S.S.银河系平面巡天中发现的一个不寻常的TeV伽马射线源，其显著特征在于偏离银道面的位置（$b \simeq -3.5^{\circ}$）和紧凑的角尺度（$\sim 0.3^{\circ}$）。它的位置和形态挑战了传统的脉冲星风云和超新星遗迹的解释，且未探测到壳层或关联脉冲星，使其起源问题悬而未决。在此，我们提出HESS J1507$-$622是一个年轻的银河系千新星遗迹，其伽马射线辐射起源于轻子过程。在该场景中，该源偏离银道面的位置可自然地由前身双中子星系统受到的诞生冲撞（natal kick）所解释。我们证明，一个轻子千新星遗迹模型能够通过冲击加速电子的逆康普顿散射成功再现观测到的GeV-TeV通量，而相应的同步辐射仍低于当前的X射线和射电上限。基于该源的能量学和角大小，我们推断其距离为3.8-14.3千秒差距（kpc），年龄为0.2-3.0千年（kyr）。重要的是，我们的分析倾向于一个年龄小于1千年的千新星遗迹。缺乏历史肉眼记录可归因于该瞬变源的快速衰减、极南赤纬以及潜在的视线消光。我们进一步评估了可能证实这一假说的独特多波长信号的探测可行性。我们发现，利用未来观测设备探测来自$r$-过程放射性同位素衰变的独特MeV伽马射线具有良好前景，同时还有来自热尘埃辐射和可能的光学光回波的互补低能信号。这些独特的信号为千新星遗迹解释提供了决定性检验，并推动当前及未来设施进行有针对性的观测。
英文摘要
HESS J1507$-$622 is an unusual TeV gamma-ray source in the H.E.S.S. Galactic Plane Survey, distinguished by its off-plane location ($b \simeq -3.5^{\circ}$) and compact angular extent ($\sim 0.3^{\circ}$). Its location and morphology challenge conventional pulsar wind nebula and supernova remnant interpretations, and the absence of a detected shell or associated pulsar leaves its origin unresolved. Here, we propose that HESS J1507$-$622 is a young Galactic kilonova remnant with gamma-ray emission of leptonic origin. In this scenario, the source's off-plane location is naturally explained by the natal kick imparted to the progenitor binary neutron star system. We demonstrate that a leptonic kilonova remnant model can successfully reproduce the observed GeV-TeV flux via inverse-Compton scattering from shock-accelerated electrons, while the corresponding synchrotron emission remains below current X-ray and radio upper limits. Based on the source's energetics and angular size, we infer a distance of 3.8-14.3 kpc and an age of 0.2-3.0 kyr. Importantly, our analysis favors a kilonova remnant younger than 1 kyr. The lack of a historical naked-eye record can be explained by the transient's rapid fading, far-southern declination, and potential line-of-sight extinction. We further assess the detectability of unique multi-wavelength signatures that could confirm this hypothesis. We find promising prospects for detecting the unique MeV gamma rays from the decay of $r$-process radioisotopes using future observatories, alongside complementary low-energy signatures from thermal dust emission and a possible optical light echo. These distinct signals offer definitive tests of the kilonova remnant interpretation and motivate targeted observations with current and future facilities.
Comments11 pages, 3 captioned figures. Prepared for submission to ApjL. Queries and comments are most Welcome
