由噪声和不完全近红外光谱反演S-型小行星组成的新方法
A new method for deriving composition of S-type asteroids from noisy and incomplete near-infrared spectra
摘要：
利用从S型小行星的近红外光谱（0.7-2.50 $μ$ m）中提取的谱带参数以及从实验室样品中得出的光谱校准值，可以确定S型小行星的表面组成。在过去，这些经验公式是通过将陨石样品的近红外光谱与其成分和矿物丰度的信息相结合而获得的。为了使这些方程得到准确的结果，它们所来源的实验室光谱的特征应该与小行星光谱数据的特征相似（即，相似信噪比（S/N）和波长范围）。在这里，我们提出了新的光谱校准，可用于确定普通的陨石般的S-型小行星的矿物成分。与以前的工作相反，在这项研究中使用的普通球粒陨石光谱的S/N已被降低，以重现小行星光谱中通常观察到的S/N，使我们能够获得更真实的结果。此外，还推导出了涵盖0.7至2.50 $μ$ m的五个波长范围的新方程，从而有可能确定数据不完整的小行星的组成。使用从小行星（25143）丝川号的近红外光谱测量的波段参数对新的光谱校准进行了测试，并将结果与返回样品的实验室测量结果进行了比较。我们发现，由铁橄榄石（Fa）和硅铁石（Fs）的摩尔含量给出的光谱衍生橄榄石和辉石化学性质与从样品（Fa $_{28.6\pm1.1}$和Fs $_{23.1\pm2.2}$）测量的平均值非常一致，Fa的最大差异为0.6 mol %，Fs的最大差异为1.4 mol %。
英文摘要：
The surface composition of S-type asteroids can be determined using band parameters extracted from their near-infrared (NIR) spectra (0.7-2.50 $μ$m) along with spectral calibrations derived from laboratory samples. In the past, these empirical equations have been obtained by combining NIR spectra of meteorite samples with information about their composition and mineral abundance. For these equations to give accurate results, the characteristics of the laboratory spectra they are derived from should be similar to those of asteroid spectral data (i.e., similar signal-to-noise ratio (S/N) and wavelength range). Here we present new spectral calibrations that can be used to determine the mineral composition of ordinary chondrite-like S-type asteroids. Contrary to previous work, the S/N of the ordinary chondrite spectra used in this study has been decreased to recreate the S/N typically observed among asteroid spectra, allowing us to obtain more realistic results. In addition, the new equations have been derived for five wavelength ranges encompassed between 0.7 and 2.50 $μ$m, making it possible to determine the composition of asteroids with incomplete data. The new spectral calibrations were tested using band parameters measured from the NIR spectrum of asteroid (25143) Itokawa, and comparing the results with laboratory measurements of the returned samples. We found that the spectrally derived olivine and pyroxene chemistry, which are given by the molar contents of fayalite (Fa) and ferrosilite (Fs), are in excellent agreement with the mean values measured from the samples (Fa$_{28.6\pm1.1}$ and Fs$_{23.1\pm2.2}$), with a maximum difference of 0.6 mol\% for Fa and 1.4 mol\% for Fs.
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