超新星遗迹IC443与IRSF/SIRIUS的近红外[ FeII ]和H2线映射
Near-infrared [FeII] and H2 line mapping of the supernova remnant IC443 with the IRSF/SIRIUS
摘要：
利用IRSF/SIRIUS的近红外[FeII]和H2线映射结果，研究了银河系超新星遗迹IC 443周围激波与星际介质相互作用的性质.在目前的研究中，我们新进行了H2 1-0 S（1）和2-1 S（1）线映射与窄带滤波器调整这些线，覆盖整个残余（30'x35'）。结合[Fe II]线图，我们的结果表明，H2线发射在南部区域明显，而[Fe II]线发射则遍布整个遗迹，这表明慢震和快震分别通过南部区域和整个遗迹传播。特别是，H2线的发射是相对较强的[Fe II]线的发射在西南地区，其中TeV的伽马射线发射检测。由于强烈的H2线发射表明致密的ISM占据主导地位，因此这一结果支持了伽马射线发射可能是通过宇宙射线质子与西南壳致密的ISM之间的强烈相互作用产生的假设。我们还发现，H2和[Fe Ⅱ]线的排放量在同一地区显示出反相关的空间分布，这表明存在cluphilism。IC 443周围ISM的这种团簇形态可能有助于宇宙射线质子与大量ISM质子有效地相互作用。
英文摘要：
We investigate properties of the interstellar medium (ISM) interacting with shocks around the Galactic supernova remnant IC443, using the results of near-infrared [FeII] and H2 line mapping with the IRSF/SIRIUS. In the present study, we newly performed H2 1-0 S(1) and 2-1 S(1) line mapping with the narrow-band filters tuned for these lines, covering the entire remnant (30'x35'). Combined with an [FeII] line map, our result shows that the H2 line emission is significantly detected in the southern region, while the [FeII] line emission is detected all over the remnant, suggesting that slow and fast shocks propagate through the southern region and the entire remnant, respectively. In particular, the H2 line emission is relatively strong compared to the [FeII] line emission in the southwestern region, where TeV gamma-ray emission is detected. As the strong H2 line emission indicates the dominance of the dense ISM, this result supports the scenario that the gamma-ray emission is likely to be produced through a heavy interaction between cosmic-ray protons and the dense ISM in the southwestern shell. We also find that the H2 and [FeII] line emissions show an anti-correlated spatial distribution in the same region, suggesting the presence of the clumpy ISM. Such a clumpy morphology of the ISM around IC443 may assist cosmic-ray protons to efficiently interact with large amounts of the ISM protons.
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