银河系中心的冰：中央秒差距内的固态冰和气态CO
Ices in the Galactic Centre : solid ice and gaseous CO in the central parsec
摘要：
在过去的几年里，我们在2.8到5.1微米的中红外波段观测到了银河系中央半秒差距。我们的目标是提高我们对银河系中心超大质量黑洞SgrA* 的直接环境的理解。本论文和Moultaka et al. 2015（已提交）描述了这项工作。在这里，我们重点研究的空间分布的12 CO冰和气相沉积。我们用位于智利UT 3/VLT ESO望远镜的ISAAC摄谱仪观测了中心半秒差距。沿着彼此平行布置的22个位置放置狭缝以映射该区域。我们在这个波长范围内建立了第一个数据立方体，覆盖了中央半秒差距。所使用的M波段滤波器的波长间隔范围为4.6至5.1微米。它拥有气态12 CO和13 CO的振转跃迁的P-和R-分支，以及归因于4.675微米处的12 CO冰的吸收带。使用两个校准器，我们可以将局部从视线衰减中分离出来，并提供前景消光的一阶估计。我们发现残留的冰和气相CO，可以归因于当地的approptions由于材料从星际和/或中央秒差距的拱星介质。我们的发现意味着温度在10到60 K的数量级，这与Moultaka等人（2004，2005）强调的该地区存在水冰的情况一致。
英文摘要：
For the past few years, we have observed the central half parsec of our Galaxy in the mid-infrared from 2.8 to 5.1 micron. Our aim is to improve our understanding of the direct environment of SgrA*, the supermassive blackhole at the centre of the Milky Way. This work is described in the present paper and by Moultaka et al. 2015 (submitted). Here, we focus on the study of the spatial distribution of the 12CO ice and gas-phase absorptions. We observed the central half parsec with ISAAC spectrograph located at the UT3/VLT ESO telescope in Chile. The slit was placed along 22 positions arranged parallel to each other to map the region. We built the first data cube in this wavelength range covering the central half parsec. The wavelength interval of the used M-band filter ranges from 4.6 to 5.1 micron. It hosts the P- and R- branches of the ro-vibrational transitions of the gaseous 12CO and 13CO, as well as the absorption band attributed to the 12CO ice at 4.675 micron. Using two calibrators, we could disentangle the local from the line-of-sight absorptions and provide a first-order estimate of the foreground extinction. We find residual ices and gase-phase CO that can be attributed to local absorptions due to material from the interstellar and/or the circumstellar medium of the central parsec. Our finding implies temperatures of the order of 10 to 60K which is in agreement with the presence of water ices in the region highlighted by Moultaka et al. (2004, 2005).
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