Abstract

This paper presents a method for solving the inverse problem of thermal sounding using calibrated data from the ACS TIRVIM experiment on board the ExoMars Trace Gas Orbiter. The 1.7–17 µm range TIRVIM Fourier spectrometer as part of the ACS instrument complex aboard the ExoMars TGO operates in the nadir and solar occultation modes in orbit around Mars. The main scientific goal of TIRVIM in the nadir observation mode is the long-term constant monitoring of the thermal structure of the Martian atmosphere and the general content of aerosols and water vapor from measurements in the range of 5–16.7 µm (600–2000 cm^–1). To process the TIRVIM nadir measurements, an algorithm was developed, allowing the retrieval of the vertical temperature profile from the surface to 60 km, the surface temperature, and the general content of dust and water ice in the atmosphere from the TIRVIM spectrum in the range of 600–1250 cm^–1, as well as the water vapor column abundance according to measurements in the range of 1250–1830 cm^–1. The processing method widely uses the achievements of previous similar experiments, taking into account the features of the TIRVIM spectra. Using the developed method 2.28 × 10⁶ spectra obtained by TIRVIM in nadir by regular measurements, were processed with retrieval of the thermal structure up to 60 km altitude and the aerosol content in the atmosphere as well as additional 2.3 × 10⁵ specially averaged TIRVIM spectra, were processed with retrieval of the water vapor column abundancein the Martian atmosphere.

中文翻译：

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使用 ExoMars TGO 上的 ACS TIRVIM FT-IR 光谱仪对火星大气进行热探测：解决反演问题的方法

摘要

本文提出了一种利用ExoMars 痕量气体轨道飞行器上的 ACS TIRVIM 实验的校准数据解决热探测反演问题的方法。1.7–17 µm 范围的 TIRVIM 傅立叶光谱仪是ExoMars TGO上 ACS 仪器综合体的一部分，在绕火星轨道上以最低点和掩星模式运行。TIRVIM 在天底观测模式下的主要科学目标是长期持续监测火星大气的热结构以及 5–16.7 µm（600–2000 cm）范围内气溶胶和水蒸气的一般含量。^–1）。为了处理 TIRVIM 天底测量，开发了一种算法，允许从该范围内的 TIRVIM 光谱中检索从地表到 60 公里的垂直温度剖面、地表温度以及大气中灰尘和水冰的一般含量。 600~1250 cm ^{–1 范围}内的水汽柱丰度，以及1250~1830 cm ^–1范围内测量的水汽柱丰度。该处理方法广泛借鉴了以往类似实验的成果，同时考虑了TIRVIM谱的特点。使用开发的方法，通过定期测量由 TIRVIM 在最低点获得的 2.28 × 10 ⁶光谱，通过检索高达 60 km 高度的热结构和大气中的气溶胶含量以及附加的 2.3 × 10 ⁵特别平均 TIRVIM 光谱进行处理，通过检索火星大气中的水蒸气柱丰度进行处理。