We present the results of infrared (IR; 2.5--160 um) 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_sun, 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 mass of ~ 6.2x10^{-4} M_sun and ~ 6.7 M_sun, 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 (~ 2,000 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.
Probing the Innermost Ejecta Layers in SNR Kes 75: Implications for the Supernova Progenitor
包含脉冲星风星云（PWNe）的超新星遗迹（SNR）具有不同的演化阶段。在非常年轻的系统中，PWN驱动冲击进入最里面的超新星（SN）材料，产生低激发线和来自加热尘埃颗粒的红外（IR）连续谱。这些观测特征使得有可能干净地测量最深的SN喷出物层的属性，这反过来又可以对SN祖源提供约束。我们提出了赫歇尔空间天文台远红外观测的PWN在银河SNR Kes 75，包含最年轻的已知脉冲星，表现出类似磁星的活动。我们检测到高度增宽的氧和碳线发射所产生的SN喷出物所遇到的PWN。我们还检测到少量（太阳质量的千分之几）的冲击加热的尘埃，空间上与喷出物材料相吻合，很可能是在SN爆炸形成的。我们使用流体动力学模型来模拟Kes 75的演化，发现PWN到目前为止已经扫除了0.05-0.1太阳质量的SN喷出物。使用爆炸和nucleosynthesis模型为不同的祖人群众与冲击模型相结合，我们比较预测的远红外辐射与观测到的线强度，发现较低的质量和爆炸能量SN祖人轻度混合喷出物的配置文件和可比丰度分数的碳和氧的青睐于较高的质量。我们的结论是，Kes 75可能是由一个8-12太阳质量的祖星产生的，这进一步证明了这种祖星的低能量爆炸可以产生磁星。
A Spectroscopic Study of Supernova Remnants with the Infrared Space Observatory
利用红外空间天文台（$ISO$）的长波光谱仪（LWS）观测数据，对超新星遗迹的远红外光谱进行了研究。我们的样本包括以前未发表的配置文件的线和连续光谱的20个信噪比在银河系和麦哲伦云。在包括G21.5-0.9、G29.7-0.3、蟹状星云和G320.4-1.2在内的几个SNR中，我们发现了[O I]、[O III]、[N II]和[C II]宽谱线的证据，这些谱线的速度色散高达几个10 $^3$ km s $^{-1}$，表明它们与高速SN喷出物有关。我们探测到的多普勒展宽的原子发射线和明亮的远红外连续暗示了SN喷出物中存在新形成的尘埃。对于G320.4-1.2，我们提出了第一次估计的喷出物尘埃质量为0.1 - 0.2 M $_\odot$，这在空间上与宽线发射相吻合，通过应用黑体模型拟合的SNR和背景发射的组件。我们的示例包括指向SNR Kes 79、CTB 109和IC 443的63，145 $μ$ m [O I]和158 $μ$ m [C II]线的光栅图。基于这些线强度，我们建议在这些SNR相互作用的冲击类型。最后，我们比较了我们的样本信噪比的LWS光谱与几个HII区的光谱，并讨论了它们的FIR线强度比和连续特性。鼓励使用具有更高空间和光谱分辨率的现代仪器（如$JWST$和$SOFIA$）进行后续观测，以便对SN喷出物和SN尘埃进行广泛研究。
Life After the Quasar: Overmassive Black Holes and Remnant Ionised Bubbles in and Around Two z~6.6 Galaxies
University of Geneva（日内瓦大学）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；University College London（伦敦大学学院）；Heidelberg University（海德堡大学）；Max Planck Institut für Astronomie（马克斯·普朗克天文学研究所）；University of Hertfordshire（赫特福德大学）；Aix Marseille Université（艾克斯-马赛大学）；Institute of Science and Technology Austria (ISTA)（奥地利科学和技术研究所）
