船帆座SNR中的X射线发射结构：喷出物各向异性和祖先恒星风残余
X-ray emitting structures in the Vela SNR: ejecta anisotropies and progenitor stellar wind residuals
摘要：
船帆座超新星遗迹（SNR）显示了几个突出于前激波（弹片）之外的喷出物碎片。最近的研究表明，高硅丰度的两个弹片（A和G），位于相对于SNR中心的相反方向。这表明可能存在富硅喷流-反喷流结构。我们分析了XMM-牛顿观测到的一个明亮的团块，位于弹片G后面，沿着A和G的连接方向。目的是研究这个团块的物理和化学性质，以确定它是否是这个假定的喷流状结构的一部分。我们制作了背景校正和自适应平滑的计数率图像和中值光子能量图，并进行了空间分辨光谱分析。我们发现了两种具有不同物理性质的结构。第一个沿连接A和G的方向显著伸长。它的X射线光谱比另外两个弹片的光谱要柔和得多，以至于妨碍了对硅丰度的测定，但它的物理和化学性质与弹片A和G的一致。第二个结构，沿东南-西北方向，具有较高的温度，看起来像一个细丝。通过分析ROSAT数据，我们发现，这条细丝是我们在外壳西部边缘发现的一个非常大的连贯结构的一部分。我们得到了G型榴散弹尾部的详细描述。此外，我们发现了一个连贯的和非常广泛的功能，我们解释为早期的残留物与其祖先恒星的恒星风相互作用的签名。我们在风残差中发现的奇特的Ne/O比值可能暗示船帆座SNR的沃尔夫-拉叶祖先，尽管需要进一步的分析来解决这一点。
英文摘要：
The Vela supernova remnant (SNR) shows several ejecta fragments protruding beyond the forward shock (shrapnel). Recent studies have revealed high Si abundance in two shrapnel (A and G), located in opposite directions with respect to the SNR center. This suggests the possible existence of a Si-rich jet-counterjet structure. We analyzed an XMM-Newton observation of a bright clump, behind shrapnel G, which lies along the direction connecting A and G. The aim is to study the physical and chemical properties of this clump to ascertain whether it is part of this putative jet-like structure. We produced background-corrected and adaptively-smoothed count-rate images and median photon energy maps, and performed a spatially resolved spectral analysis. We identified two structures with different physical properties. The first one is remarkably elongated along the direction connecting A and G. Its X-ray spectrum is much softer than that of the other two shrapnel, to the point of hindering the determination of the Si abundance, however its physical and chemical properties are consistent with those of shrapnel A and G. The second structure, running along the southeast-northwest direction, has a higher temperature and appears like a thin filament. By analyzing the ROSAT data, we have found that this filament is part of a very large and coherent structure that we identified in the western rim of the shell. We obtained a thorough description of the tail of Shrapnel G. In addition we discovered a coherent and very extended feature that we interpret as a signature of an earlier interaction of the remnant with the stellar wind of its progenitor star. The peculiar Ne/O ratio we found in the wind residual may be suggestive of a Wolf-Rayet progenitor for Vela SNR, though further analysis is required to address this point.
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