发表机构
INAF, Osservatorio Astrofisico di Catania; Department of Astronomy, Faculty of Mathematics, University of Belgrade; Department of Physics and Astronomy, University of Calgary; Instituto de Astrofísica de Andalucía (IAA-CSIC); Astrophysics and Space Technologies Research Centre, Macquarie University; INAF, Osservatorio Astronomico di Cagliari; Western Sydney University; Australia Telescope National Facility, CSIRO; Astronomical Observatory, Volgina 7; SBASSE at Lahore University of Management Sciences, LUMS（意大利国家天体物理研究所，卡塔尼亚天文台; 贝尔格莱德大学数学学院天文学系; 卡尔加里大学物理与天文学系; 安达卢西亚天体物理学研究所（西班牙高等科学研究委员会）; 麦夸里大学天体物理学与空间技术研发中心; 意大利国家天体物理研究所，卡利亚里天文台; 西悉尼大学; 澳大利亚望远镜国家设施，CSIRO; 伏尔吉纳街7号天文台; 拉合尔管理科学大学SBASSE）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
利用ASKAP和MWA-GLEAM数据对超新星遗迹G343.1-00.7进行空间分辨射电谱分析，确定其谱指数并揭示丝状结构及演化阶段。
AI 中文摘要
超新星遗迹（SNRs）是延展射电源，其形态和演化受强激波与周围介质相互作用的塑造。我们结合了来自宇宙演化图谱（EMU）巡天的0.944 GHz澳大利亚平方公里阵列探路者（ASKAP）图像与0.088-0.200 GHz的MWA-GLEAM数据，以表征G343.1$-$00.7的综合射电谱，并进行了其首次灵敏的空间分辨谱分析。我们推导出综合谱指数为$\alpha=-0.50\pm0.01$，以更高的精度确认了先前报道的值。我们重新定义了该遗迹的射电形态，提供了首个形态学和谱学证据，表明与邻近的\hii\\ G343.147$-$00.44重叠的丝状结构与SNR相关。局部亮度-亮度分析揭示了东南壳层上谱指数较平的丝状结构，这与辐射性或部分辐射性激波可能产生的热轫致辐射贡献一致。与\hi\\和CO数据的比较识别出与SNR距离在运动学上一致的气体成分，尽管未发现相互作用的明确形态学证据。\hii\\周围的气体分布表明存在一个膨胀的\hi\\壳层，部分嵌入其母分子云中。理论模型将G343.1$-$00.7置于晚期Sedov阶段和早期压力驱动阶段之间，表明该遗迹的不同部分处于不同的演化阶段。这些结果凸显了高分辨率ASKAP观测在复杂银河环境中对表征不足的SNR进行空间分辨研究的潜力。
英文摘要
Supernova remnants (SNRs) are extended radio sources whose morphology and evolution are shaped by the interaction of strong shocks with the surrounding medium. We combined the 0.944 GHz Australian Square Kilometre Array Pathfinder (ASKAP) image from the Evolutionary Map of the Universe (EMU) survey with 0.088-0.200 GHz MWA-GLEAM data to characterize the integrated radio spectrum of G343.1$-$00.7 and perform its first sensitive spatially resolved spectral analysis. We derived an integrated spectral index of $α=-0.50\pm0.01$, confirming the previously reported value with improved accuracy. We redefined the radio morphology of the remnant, providing the first morphological and spectral evidence that filamentary structures overlapping the nearby \hii\ G343.147$-$00.44 are associated with the SNR. Local brightness-brightness analysis revealed flatter-spectrum filaments along the south-eastern shell, consistent with a possible thermal bremsstrahlung contribution from radiative or partially radiative shocks. Comparison with \hi\ and CO data identified gas components kinematically consistent with the SNR distance, although no clear morphological evidence of interaction was found. The gas distribution around the \hii\ suggests an expanding \hi\ shell partially embedded within its parent molecular cloud. Theoretical models place G343.1$-$00.7 between the late Sedov and early pressure-driven phases, suggesting different evolutionary stages across the remnant. These results highlight the potential of high-resolution ASKAP observations for spatially resolved studies of poorly characterized SNRs in complex Galactic environments.
Comments16 pages, 12 figures. Accepted for publication in Astronomy & Astrophysics (A&A)
