关于 JWST/MIRI 观测到的气相 H2O 中红外吸收线的解释

Jialu Li, Adwin Boogert, Alexander G. G. M. Tielens
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摘要

在 5-8 μm 波长范围内的 H2O 振荡吸收线可以在年轻恒星天体和活动星系核内部区域的中红外连续发射背景下选择性地探测气体,并提供有关这些温暖、尘埃遮蔽环境的重要信息。JWST/Mid-Infrared Instrument (MIRI)以 R ∼ 3500 的中等光谱分辨能力(85 km s-1 的半最大全宽)在许多视线中探测到这些谱线。根据我们对高分辨率 SOFIA/EXES 观测数据的分析,我们发现 JWST/MIRI 吸收光谱的解释可能会因为单个跃迁的混合、内在线宽信息的丢失或背景连续光源的部分覆盖而受到严重影响。在本文中,我们指出了从解析度不够的光谱推导物理性质时出现的退化等问题。这可能导致柱密度相差 2 个数量级。我们强调了在光谱分析中对光学细线和弱线进行加权的重要性,并提供了分解耦合参数的方法。我们还提供了一个生成 H2O 吸收线光谱的在线工具,可以将其与观测数据进行比较。
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On the Interpretation of Mid-infrared Absorption Lines of Gas-phase H2O as Observed by JWST/MIRI
Rovibrational absorption lines of H2O in the 5–8 μm wavelength range selectively probe gas against the mid-infrared continuum-emitting background of the inner regions of young stellar objects and active galactic nuclei and deliver important information about these warm, dust-obscured environments. JWST/Mid-Infrared Instrument (MIRI) detects these lines in many lines of sight at a moderate spectral resolving power of R ∼ 3500 (full width at half-maximum of 85 km s−1). Based on our analysis of high-resolution SOFIA/EXES observations, we find that the interpretation of JWST/MIRI absorption spectra can be severely hampered by the blending of individual transitions and the lost information on the intrinsic line width or the partial coverage of the background continuum source. In this paper, we point out problems such as degeneracy that arise in deriving physical properties from an insufficiently resolved spectrum. This can lead to differences in the column density by 2 orders of magnitude. We emphasize the importance of weighting optically thin and weak lines in spectral analyses and provide recipes for breaking down the coupled parameters. We also provide an online tool to generate the H2O absorption line spectra that can be compared to observations.
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