Condensed Matter天体物理学：用X射线确定Interstellar Dust的物种特异性成分和数量的处方
Condensed Matter Astrophysics: A Prescription for Determining the Species-Specific Composition and Quantity of Interstellar Dust using X-rays
摘要：
我们提出了一种使用<6 keV X射线确定天体物理环境中尘埃的数量和成分的新技术。我们认为，高分辨率的X射线光谱，使钱德拉和XMM-牛顿光栅应被视为一个强大的和可行的新资源，深入到一个相对未开发的制度，直接确定尘埃的性质：成分，数量和分布。我们目前的初始横截面测量的天体物理学可能的铁基尘埃候选人在劳伦斯伯克利国家实验室先进光源同步加速器光束线，作为一个说明性的工具，制定我们的方法。集中在700 eV的Fe LIII和LII光电边缘，我们讨论了一种技术，用于模拟尘埃的软X射线使用L-边缘数据的属性，以补充K-边缘X射线吸收精细结构分析技术在李和拉威尔2005年讨论。这是一份对凝聚态实验学家和天体物理学家都感兴趣和有用的技术论文。对于实验者，我们提供了一个新的处方归一化相对较低的S/N L-边缘截面测量。对于天体物理学的利益，我们讨论了使用X射线吸收光谱确定尘埃成分在寒冷和电离的天体物理环境中，和一种新的方法来确定 * 特定种类的气体-尘埃比 *。可能感兴趣的天体物理学应用，提供。在光栅和量热计的光谱分辨率目标方面，针对Astro-H和国际X射线天文台等拟议和计划的飞行任务，提出了今后X射线飞行任务具有更高吞吐量和光谱分辨率的改进这一工作的前景。
英文摘要：
We present a new technique for determining the *quantity and composition* of dust in astrophysical environments using <6keV X-rays. We argue that high resolution X-ray spectra as enabled by the Chandra and XMM-Newton gratings should be considered a powerful and viable new resource for delving into a relatively unexplored regime for directly determining dust properties: composition, quantity, and distribution. We present initial cross-section measurements of astrophysically likely iron-based dust candidates taken at the Lawrence Berkeley National Laboratory Advanced Light Source synchrotron beamline, as an illustrative tool for the formulation of our methodology. Focused at the 700eV Fe LIII and LII photoelectric edges, we discuss a technique for modeling dust properties in the soft X-rays using L-edge data, to complement K-edge X-ray absorption fine structure analysis techniques discussed in Lee & Ravel 2005. This is intended to be *a techniques paper* of interest and usefulness to both condensed matter experimentalists and astrophysicists. For the experimentalists, we offer a new prescription for normalizing relatively low S/N L-edge cross section measurements. For astrophysics interests, we discuss the use of X-ray absorption spectra for determining dust composition in cold and ionized astrophysical environments, and a new method for determining *species-specific gas-to-dust ratios*. Possible astrophysical applications of interest, are offered. Prospects for improving on this work with future X-ray missions with higher throughput and spectral resolution are presented in the context of spectral resolution goals for gratings and calorimeters, for proposed and planned missions such as Astro-H and the International X-ray Observatory.
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