来自interstellar dust的X射线消光：观测碳、硫和其它微量元素的前景
X-ray extinction from interstellar dust: Prospects of observing carbon, sulfur and other trace elements
摘要：
我们提出了一个研究的前景，观察碳，硫，和其他低丰度元素（即铝，钙，钛和镍）存在于星际介质中使用未来的X射线仪器。我们特别关注沿视线的星际尘埃的探测和表征。我们比较了模拟数据与不同的尘埃聚集体，无论是从过去的文献中获得的或由我们使用SOLEIL-LUCIA同步加速器光束线测量。由星际颗粒引起的消光引起给定光电边缘的调制，这在原则上可以追溯到吸收颗粒的化学性质。我们模拟了具有当前Athena，XRISM和Arcus概念的分辨率和灵敏度特性的仪器的数据。在不久的将来，将有把握地确定所研究元素的贫化和丰度。在碳和硫的情况下，还将确定吸收粉尘的化学特性，这取决于主要化合物。对于铝和钙，尽管在星际介质中有很大的损耗和显著的尘埃吸收，但在许多情况下，边缘特征可能不会随着含Al $^-$或Ca $^-$化合物的化学性质的变化而显著改变。可以检测和模拟大颗粒的排除特征，从而允许对这些元素的不同颗粒尺寸分布进行测试。Ti和Ni的低宇宙丰度将不允许我们详细研究边缘特征。
英文摘要：
We present a study on the prospects of observing carbon, sulfur, and other lower abundance elements (namely Al, Ca, Ti and Ni) present in the interstellar medium using future X-ray instruments. We focus in particular on the detection and characterization of interstellar dust along the lines of sight. We compare the simulated data with different sets of dust aggregates, either obtained from past literature or measured by us using the SOLEIL-LUCIA synchrotron beamline. Extinction by interstellar grains induces modulations of a given photolelectric edge, which can be in principle traced back to the chemistry of the absorbing grains. We simulated data of instruments with characteristics of resolution and sensitivity of the current Athena, XRISM and Arcus concepts. In the relatively near future, the depletion and abundances of the elements under study will be determined with confidence. In the case of carbon and sulfur, the characterization of the chemistry of the absorbing dust will be also determined, depending on the dominant compound. For aluminum and calcium, despite the large depletion in the interstellar medium and the prominent dust absorption, in many cases the edge feature may not be changing significantly with the change of chemistry in the Al$^-$ or Ca$^-$ bearing compounds. The exinction signature of large grains may be detected and modeled, allowing a test on different grain size distributions for these elements. The low cosmic abundance of Ti and Ni will not allow us a detailed study of the edge features.
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