Deep optical CCD images of the supernova remnant G 32.8-0.1 were obtained where filamentary and diffuse emission was discovered. The images were acquired in the emission lines of Halpha+[N II] and [S II]. Filamentary and diffuse structures are detected in most areas of the remnant, while no significant [O III] emission is present. The flux-calibrated images suggest that the optical emission originates from shock-heated gas since the [S II]/Halpha ratio is greater than 1.2. The Spitzer images at 8 micron and 24 micron show a few filamentary structures to be correlated with the optical filaments, while the radio emission at 1.4 GHz in the same area is found to be very well correlated with the brightest optical filaments. Furthermore, the results from deep long-slit spectra also support the origin of the emission to be from shock-heated gas ([S II]/Halpha > 1.5). The absence of [O III] emission indicates slow shocks velocities into the interstellar "clouds" (< 100 km/s), while the [S II] 6716/6731 ratio indicates electron densities up to ~200 cm^{-3}. Finally, the Halpha emission is measured to lie between 1.8 to 4.6 x 10^{-17} erg/s/cm^2/arcsec^2, while from VGPS HI images a distance to the SNR is estimated to be between 6 to 8.5 kpc.
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。
