（136199）Eris在350和2350 nm之间的光谱：使用X-Shooter的结果
The spectrum of (136199) Eris between 350 and 2350 nm: Results with X-Shooter
摘要：
X-Shooter是ESO-VLT的第一个第二代仪器。它是一台光谱仪，具有高分辨率，可同时覆盖300 - 2480 nm的光谱范围.这些性质诱使我们在仪器的科学验证期间观察（136199）厄里斯。目标在光学和近红外区域具有许多吸收特征，不同的作者观察到了这些特征，显示出它们的位置和强度的差异。我们试图限制超挥发物的存在，例如，CH 4，CO和N2，特别是试图了解厄里斯表面冰的物理化学状态。我们观察到厄里斯在300-2480 nm范围内，并比较新获得的光谱与文献中提供的。我们确定了几个吸收功能，测量它们的位置和深度，并将它们与纯甲烷冰的反射率进行比较，这些反射率是从30 K时冰的光学常数中获得的，以研究它们的位置变化，并找到它们的起源的可能解释。我们确定了光谱中的几个吸收带，都与甲烷冰的存在相一致。我们没有发现与N2或CO有关的谱带，我们测量了这些谱带的中心波长，并发现相对于30 K下纯CH 4的光谱的可变位移。结论.基于这些波长的变化，我们证实了稀释的CH 4在其他冰的厄里斯的表面上的存在和纯CH 4的存在空间隔离。这些带的中心和形状与以前的作品的比较表明，表面是异质的。如果地面温度低于35.6 K，即该冰的α和β相之间的转变温度，则可以解释N2的2160 nm带的缺失。我们的研究结果，包括重新分析其他地方发表的数据，指向厄里斯的异质表面。
英文摘要：
X-Shooter is the first second-generation instrument for the ESO-VLT. It as a spectrograph covering the 300 - 2480 nm spectral range at once with a high resolving power. These properties enticed us to observe (136199) Eris during the science verification of the instrument. The target has numerous absorption features in the optical and near-infrared domain which has been observed by different authors, showing differences in their positions and strengths. We attempt at constraining the existence of super-volatiles, e.g., CH4, CO and N2, and in particular try to understand the physical-chemical state of the ices on Eris' surface. We observed Eris in the 300-2480 nm range and compared the newly obtained spectra with those available in the literature. We identified several absorption features, measuring their positions and depth and compare them with those of reflectance of pure methane ice obtained from the optical constants of this ice at 30 K to study shifts in their positions and find a possible explanation for their origin. We identify several absorption bands in the spectrum all consistent with the presence of CH4 ice. We do not identify bands related with N2 or CO. We measured the central wavelengths of the bands and find variable shifts, with respect to the spectrum of pure CH4 at 30 K. Conclusions. Based on these wavelength shifts we confirm the presence of a dilution of CH4 in other ice on the surface of Eris and the presence of pure CH4 spatially segregated. The comparison of the centers and shapes of these bands with previous works suggest that the surface is heterogeneous. The absence of the 2160 nm band of N2 can be explained if the surface temperature is below 35.6 K, the transition temperature between the alpha and beta phases of this ice. Our results, including the reanalysis of data published elsewhere, point to an heterogeneous surface on Eris.
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