Far-Infrared Luminous Supernova Remnant Kes 17
Far-Infrared Luminous Supernova Remnant Kes 17
复制标题
远红外发光超新星遗迹 Kes 17
DOI：
10.1088/0004-637x/740/1/31
复制
发表时间：
2011
影响因子：
4.9
通讯作者：
7番
中科院分区：
文献类型：
--
作者：
Lee;Ho-Gyu;他6名;7番
本文介绍了利用AKARI和Spitzer卫星对超新星遗迹Kes 17的红外（IR; 2.5-160 μm）观测结果。我们首先检测到明亮的连续发射的西壳在中红外和远红外波段连同其近红外分子线发射。我们还检测到隐藏的中红外发射后，在该地区的背景发射减去其南部壳。西壳的远红外光度为108100 L，这使得Kes 17成为少数几个有显著远红外辐射的SNR之一。光谱能量分布的拟合表明存在两个尘埃成分：热的79 K和冷的27 K，分别对应于6.2× 10− 4 M和6.7 M的尘埃质量。我们认为，热分量代表的灰尘排放的SNR扫到其西部和南部边界的材料，兼容的无线电连续辐射的分布重叠的中红外发射在西部和南部壳。另一方面，西壳层的近红外分子线发射揭示了热的（约2000 K）冲击致密分子气体的存在，这表明冷尘埃成分代表了与SNR和附近分子气体之间相互作用有关的尘埃发射。分子气体的激发条件似乎与不同温度的激波、凝块混合气体的激发条件一致。本文讨论了西壳层冷尘埃明亮远红外辐射的三种可能来源：激波分子云团间介质中的尘埃辐射、被热气体吞没的分子云蒸发流中的尘埃辐射以及辐射激波照射的附近分子云的尘埃辐射。
We present the results of infrared (IR; 2.5–160 μm) observations of the supernova remnant (SNR) Kes 17 based on the data obtained with the AKARI and Spitzer satellites. We first detect bright continuum emission of its western shell in the mid-and far-IR wavebands together with its near-IR molecular line emission. We also detect hidden mid-IR emission of its southern shell after subtraction of the background emission in this region. The far-IR luminosity of the western shell is∼ 8100 L☉, which makes Kes 17 one of the few SNRs of significant far-IR emission. The fittings of the spectral energy distribution indicate the existence of two dust components:∼ 79 K (hot) and∼ 27 K (cold) corresponding to the dust masses of∼ 6.2× 10− 4 M☉ and∼ 6.7 M☉, respectively. We suggest that the hot component represents the dust emission of the material swept up by the SNR to its western and southern boundaries, compatible with the distribution of radio continuum emission overlapping the mid-IR emission in the western and southern shells. The existence of hot (∼ 2000 K), shocked dense molecular gas revealed by the near-IR molecular line emission in the western shell, on the other hand, suggests that the cold dust component represents the dust emission related to the interaction between the SNR and nearby molecular gas. The excitation conditions of the molecular gas appear to be consistent with those from shocked, clumpy admixture gas of different temperatures. We discuss three possibilities for the origin of the bright far-IR emission of the cold dust in the western shell: the emission of dust in the inter-clump medium of shocked molecular clouds, the emission of dust in evaporating flows of molecular clouds engulfed by hot gas, and the emission of dust of nearby molecular clouds illuminated by radiative shocks.