Gas Orbiter(氣體軌道飛行器)到底是什麼？
Gas Orbiter 氣體軌道飛行器 - Solar occultations performed by the Nadir and Occultation for MArs Discovery (NOMAD) ultraviolet and visible spectrometer (UVIS) onboard the ExoMars Trace Gas Orbiter (TGO) have provided a comprehe. [1] The ExoMars Trace Gas Orbiter (TGO)’s Colour and Stereo Surface Imaging System (CaSSIS) provides multi-spectral optical imagery at 4-5m/pixel spatial resolution. [2] FREND is a neutron telescope installed onboard Russian-European ExoMars mission Trace Gas Orbiter. [3] Moreover, we note that numerous scenarios of methane fluxes from terrestrial analogs may explain non-detections by the ExoMars Trace Gas Orbiter (TGO), as they can produce atmospheric concentrations below the TGO limit of detection. [4] The Trace Gas Orbiter, the first element of the ExoMars programme, began its science phase in 2018 focusing on investigations of the atmospheric composition with unprecedented sensitivity as well as surface and subsurface studies. [5] Our results are based on solar occultation measurements by Atmospheric Chemistry Suite (ACS) onboard the ExoMars Trace Gas Orbiter (TGO). [6] Measurements by the Atmospheric Chemistry Suite mid-infrared channel (ACS MIR) on the ExoMars Trace Gas Orbiter allow us to measure the ratio of hydrogen chloride two stable isotopologues, H35Cl and H37Cl. [7] Here, we analyze data from the High Resolution Imaging Science Experiment (HiRISE) and from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instruments onboard NASA's Mars Reconnaissance Orbiter and the Colour and Stereo Surface Imaging System (CaSSIS) onboard ESA's Trace Gas Orbiter to characterize, at a high spatial resolution, the morphological and spectral variability of Oxia Planum's surface deposits. [8] Hydrogen chloride (HCl) was recently discovered in the atmosphere of Mars by two spectrometers onboard the ExoMars Trace Gas Orbiter. [9] We present simulations of the HDO cycle with the LMD Mars GCM and compare the retrieved cycle with observations provided by the Atmospheric Chemistry Suite (ACS) on board the ESA/Roscosmos Trace Gas Orbiter (TGO). [10] We demonstrate the wide applicability of this technique with the ExoMars Trace Gas Orbiter Colour and Stereo Surface Imaging System (CaSSIS) 4. [11] "The Colour and Stereo Surface Imaging System (CaSSIS) for the ExoMars Trace Gas Orbiter. [12] The paper summarises the results achieved, identifies lessons learned and gives an overview of what is coming next as ERCO prepares for its operational roll-out to support relay services provided by ESA's Trace Gas Orbiter to NASA's Curiosity and Perseverance Rovers. [13] Our intent is to complement and improve on the previously reported detection attempts by the Atmospheric Chemistry Suite(ACS) on board the ExoMars Trace Gas Orbiter (TGO). [14] 8 μm with the Atmospheric Chemistry Suite and confirmed with Nadir and Occultation for Mars Discovery instruments onboard the ExoMars Trace Gas Orbiter, reveal widely distributed HCl in the 1- to 4-ppbv range, 20 times greater than previously reported upper limits. [15] HCl was discovered in the atmosphere of Mars for the first time during the global dust storm in Mars year (MY) 34 (July 2018) using the Atmospheric Chemistry Suite mid-infrared channel (ACS MIR) on the ExoMars Trace Gas Orbiter. [16] CaSSIS is the multispectral stereo push frame camera on board ExoMars TGO (Trace Gas Orbiter) which will image 1. [17] More than a full Martian year of observations have now been made by the Nadir Occultation for MArs Discovery (NOMAD) instrument suite on-board the ExoMars Trace Gas Orbiter. [18] Here we report HDO and H2O profiles observed by the Atmospheric Chemistry Suite (ExoMars Trace Gas Orbiter) in orbit around Mars that, once combined with expected photolysis rates, reveal the prevalence of the perihelion season for the formation of atomic H and D at altitudes relevant for escape. [19] The Open University modelling group global circulation model is combined with retrievals from the ExoMars Trace Gas Orbiter (temperature and water vapour profiles from the Atmospheric Chemistry Suite and water vapour profiles from the Nadir and Occultation for Mars Discovery instrument) and the Mars Climate Sounder (temperature profiles and dust column) on the Mars Reconnaissance Orbiter. [20] This work takes advantage of the NOMAD spectrometer observations, on board the 2016 ExoMars Trace Gas Orbiter. [21] 3 µm in the atmosphere of Mars by ExoMars Trace Gas Orbiter ACS instrument. [22] The Atmospheric Chemistry Suite (ACS) is a set of three spectrometers (-NIR, -MIR, and -TIRVIM) intended to observe Mars atmosphere onboard the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission (Korablev et al. [23] 6 µm) spectra measured by TIRVIM and NIR instruments onboard the ExoMars Trace Gas Orbiter (TGO) in solar occultation geometry. [24] The Trace Gas Orbiter, TGO, is now well into its second Martian year of operations. [25] Here we report vertical profiles of CO from 10 to 120 km, and from a broad range of latitudes, inferred from the Atmospheric Chemistry Suite on board the ExoMars Trace Gas Orbiter. [26] This large day-night difference suggests that methane accumulates while contained near the surface at night, but drops below TLS-SAM detection limits during the day, consistent with the daytime nondetection by instruments on board the ExoMars Trace Gas Orbiter. [27] The Atmospheric Chemistry Suite on the ExoMars Trace Gas Orbiter has a spectral range that includes several absorption lines of PH3 with line strengths comparable to previously observed CH4 lines. [28] The ExoMars Trace Gas Orbiter (TGO) spacecraft has detected no methane on Mars despite having better sensitivity than Curiosity, but had not yet examined the Gale location. [29] Technical details of the method are described, and results are demonstrated using a 4 m/pixel Trace Gas Orbiter Colour and Stereo Surface Imaging System (CaSSIS) panchromatic image and an overlapping 6 m/pixel Mars Reconnaissance Orbiter Context Camera (CTX) stereo pair to produce a 1 m/pixel CaSSIS Super-Resolution Restoration (SRR) DTM for different areas over Oxia Planum on Mars—the future ESA ExoMars 2022 Rosalind Franklin rover’s landing site. [30] Purpose This paper aims to describe the development of a knowledge management system (KMS) for the Nadir and Occultation for Mars Discovery (NOMAD) instrument on board the ESA/Roscosmos 2016 ExoMars Trace Gas Orbiter (TGO) spacecraft. [31] The ExoMars Trace Gas Orbiter (TGO) began its nominal science phase at Mars in April 2018, following releases of editions to two major spectroscopic line lists: GEISA 2015 (Gestion et Etude des Informations Spectroscopiques Atmospheriques: Management and Study of Atmospheric Spectroscopic Information), and HITRAN 2016 (High Resolution Transmission). [32] We present a new data set of density perturbation amplitudes derived from accelerometer measurements during aerobraking of the European Space Agency’s Trace Gas Orbiter. [33] In this study we use images from the Colour and Stereo Surface Imaging System (CaSSIS) aboard ESA’s Trace Gas Orbiter (TGO) to study the relationship between surface frosts and gullies. [34] The Atmospheric Chemistry Suite (ACS) instrument onboard the ExoMars Trace Gas Orbiter (TGO) ESA-Roscosmos mission began science operations in March 2018. [35] This paper aims at giving a flight dynamics perspective on ExoMars Trace Gas Orbiter aerobraking operations, discussing the main challenges for both navigation and spacecraft commanding, describing the work-flow of activities within an operation cycle and presenting some results from the successful campaign, together with the most important lessons learnt. [36] Using synergy, the scientific return of nadir observations of current and future missions at Mars (such as the ExoMars Trace Gas Orbiter) can be fully optimized. [37] Here we report highly sensitive measurements of the atmosphere of Mars in an attempt to detect methane, using the ACS and NOMAD instruments onboard the ESA-Roscosmos ExoMars Trace Gas Orbiter from April to August 2018. [38] The ExoMars Trace Gas Orbiter (TGO), Emirates Mars Mission (EMM), and possible future Mars stationary satellite(s) will provide innovative data products on the optical depth of dust and water ice clouds in the Martian atmosphere with a temporal resolution of hours. [39] Although the presence of CH4 is still under debate because of large measurement uncertainties, the forthcoming ESA-Roscosmos mission, which employs the Trace Gas Orbiter (TGO), will settle questions on the existence of this gas and its origin. [40] Here we present concurrent, high-resolution measurements of dust, water and semiheavy water (HDO) at the onset of a global dust storm, obtained by the NOMAD and ACS instruments onboard the ExoMars Trace Gas Orbiter. [41] Trace Gas Orbiter spacecraft did not find the gas in red planet’s atmosphere during its first months of operation. [42] We report infrared measurements of the Martian atmosphere obtained with the mid-infrared channel (MIR) of the Atmospheric Chemistry Suite (ACS), onboard the ExoMars Trace Gas Orbiter. [43] The Nadir and Occultation for MArs Discovery instrument (NOMAD), onboard the ExoMars Trace Gas Orbiter (TGO) spacecraft was conceived to observe Mars in solar occultation, nadir, and limb geometries, and will be able to produce an outstanding amount of diverse data, mostly focused on properties of the atmosphere. [44] Here we present water vapor vertical profiles in the periods of the two dust storms (Ls = 162–260° and Ls = 298–345°) from the solar occultation measurements by Nadir and Occultation for Mars Discovery (NOMAD) onboard ExoMars Trace Gas Orbiter (TGO). [45]ExoMars Trace Gas Orbiter (TGO) 上的 Nadir 和 Occultation for MArs Discovery (NOMAD) 紫外和可見光譜儀 (UVIS) 進行的太陽掩星提供了一個全面的信息。 [1] ExoMars 微量氣體軌道器 (TGO) 的彩色和立體表面成像系統 (CaSSIS) 以 4-5m/像素的空間分辨率提供多光譜光學圖像。 [2] <p>FREND 是安裝在俄羅斯-歐洲 ExoMars 任務 Trace Gas Orbiter 上的中子望遠鏡。 [3] 此外，我們注意到來自陸地類似物的大量甲烷通量情景可能解釋了 ExoMars 微量氣體軌道器 (TGO) 未檢測到的原因，因為它們可以產生低於 TGO 檢測限的大氣濃度。 [4] 微量氣體軌道器是 ExoMars 計劃的第一個元素，於 2018 年開始其科學階段，重點以前所未有的靈敏度調查大氣成分以及地表和地下研究。 [5] 我們的結果基於 ExoMars 微量氣體軌道器 (TGO) 上的大氣化學套件 (ACS) 對太陽掩星的測量。 [6] 通過 ExoMars 微量氣體軌道器上的大氣化學套件中紅外通道 (ACS MIR) 進行的測量使我們能夠測量氯化氫兩種穩定同位素體 H35Cl 和 H37Cl 的比率。 [7] 在這裡，我們分析來自美國宇航局火星偵察軌道器上的高分辨率成像科學實驗 (HiRISE) 和緊湊型火星偵察成像光譜儀 (CRISM) 儀器以及歐空局微量氣體軌道器上的彩色和立體表面成像系統 (CaSSIS) 的數據，以以高空間分辨率表徵 Oxia Planum 表面沉積物的形態和光譜變化。 [8] ExoMars 微量氣體軌道器上的兩個光譜儀最近在火星大氣中發現了氯化氫 (HCl)。 [9]  </p> <p>我們使用 LMD Mars GCM 模擬 HDO 循環，並將檢索到的循環與 ESA/Roscosmos 痕量氣體軌道器 (TGO) 上的大氣化學套件 (ACS) 提供的觀測結果進行比較。 [10] 我們通過 ExoMars 示踪氣體軌道器顏色和立體表面成像系統 (CaSSIS) 4 展示了該技術的廣泛適用性。 [11] “用於 ExoMars 微量氣體軌道器的彩色和立體表面成像系統 (CaSSIS)。 [12] 該文件總結了取得的成果，確定了經驗教訓，並概述了 ERCO 準備其業務推出以支持 ESA 的微量氣體軌道器向 NASA 的好奇號和毅力號漫遊車提供的中繼服務。 [13] 我們的目的是補充和改進先前報告的 ExoMars 微量氣體軌道器 (TGO) 上的大氣化學套件 (ACS) 的檢測嘗試。 [14] 8 μm 使用 Atmospheric Chemistry Suite 並通過 ExoMars Trace Gas Orbiter 上的火星發現儀器的 Nadir 和 Occultation 確認，揭示了 1 至 4 ppbv 範圍內廣泛分佈的 HCl，比之前報導的上限高 20 倍。 [15] 在火星年 (MY) 34（2018 年 7 月）的全球沙塵暴期間，使用 ExoMars 微量氣體軌道器上的大氣化學套件中紅外通道 (ACS MIR) 首次在火星大氣中發現了 HCl。 [16] CaSSIS 是 ExoMars TGO（微量氣體軌道飛行器）上的多光譜立體推幀相機，它將對 1 進行成像。 [17] ExoMars 微量氣體軌道器上的火星探測天底掩星 (NOMAD) 儀器套件現已對火星進行了整整一年多的觀測。 [18] 在這裡，我們報告了大氣化學套件（ExoMars Trace Gas Orbiter）在火星軌道上觀察到的 HDO 和 H2O 剖面，一旦與預期的光解速率相結合，揭示了在相關高度形成原子 H 和 D 的近日點季節的普遍性為了逃跑。 [19] 開放大學建模小組全球環流模型與來自 ExoMars 微量氣體軌道器（大氣化學套件的溫度和水蒸氣剖面以及火星發現儀器的天底和掩星）和火星氣候探測儀（溫度輪廓和塵埃柱）在火星偵察軌道器上。 [20] <p>這項工作利用了 2016 年 ExoMars 微量氣體軌道器上的 NOMAD 光譜儀觀測結果。 [21] ExoMars Trace Gas Orbiter ACS 儀器在火星大氣中測量 3 µm。 [22] </p><p>大氣化學套件 (ACS) 是一組三個光譜儀（-NIR、-MIR 和 -TIRVIM），用於在 ESA-Roscosmos ExoMars 2016 微量氣體軌道飛行器 (TGO) 任務上觀察火星大氣（Korablev 等人。 [23] 6 µm) 光譜，由 ExoMars 微量氣體軌道器 (TGO) 上的 TIRVIM 和 NIR 儀器在太陽掩星幾何中測量。 [24] <p>TGO 微量氣體軌道器現已進入火星運行的第二個年頭。 [25] 在這裡，我們報告了從 ExoMars 微量氣體軌道器上的大氣化學套件推斷出的 10 到 120 km 以及來自廣泛緯度的 CO 垂直剖面。 [26] 這種巨大的晝夜差異表明，甲烷在夜間聚集在地表附近，但在白天低於 TLS-SAM 檢測限，這與 ExoMars 微量氣體軌道器上的儀器在白天未檢測到一致。 [27] ExoMars 微量氣體軌道器上的大氣化學套件的光譜範圍包括多個 PH3 吸收線，其線強度與之前觀察到的 CH4 線相當。 [28] ExoMars Trace Gas Orbiter (TGO) 宇宙飛船在火星上沒有檢測到甲烷，儘管它的靈敏度比好奇號更高，但尚未檢查大風的位置。 [29] 描述了該方法的技術細節，並使用 4 m/像素的示踪氣體軌道器彩色和立體表面成像系統 (CaSSIS) 全色圖像和重疊的 6 m/像素火星偵察軌道器上下文相機 (CTX) 立體對來演示結果為火星上 Oxia Planum 上的不同區域（未來的 ESA ExoMars 2022 Rosalind Franklin 漫遊者的著陸點）生成 1 m/像素的 CaSSIS 超分辨率恢復 (SRR) DTM。 [30] 目的 本文旨在描述 ESA/Roscosmos 2016 ExoMars 微量氣體軌道器 (TGO) 航天器上的火星探測天底和掩星 (NOMAD) 儀器知識管理系統 (KMS) 的開發。 [31] ExoMars 微量氣體軌道器 (TGO) 於 2018 年 4 月在火星開始其名義科學階段，隨後發布了兩個主要光譜線列表的版本：GEISA 2015（Gestion et Etude des Informations Spectroscopiques Atmospheriques：大氣光譜信息的管理和研究），和 HITRAN 2016（高分辨率傳輸）。 [32] 我們提出了一組新的密度擾動幅度數據集，該數據集源自歐洲航天局的微量氣體軌道器航空制動期間的加速度計測量值。 [33] 在這項研究中，我們使用來自 ESA 微量氣體軌道飛行器 (TGO) 上的彩色和立體表面成像系統 (CaSSIS) 的圖像來研究地表霜凍和溝壑之間的關係。 [34] ExoMars 微量氣體軌道器 (TGO) ESA-Roscosmos 任務上的大氣化學套件 (ACS) 儀器於 2018 年 3 月開始科學運行。 [35] 本文旨在從飛行動力學角度對 ExoMars Trace Gas Orbiter 航空制動操作進行討論，討論導航和航天器指揮的主要挑戰，描述操作週期內活動的工作流程，並介紹成功運動的一些結果，以及最重要的經驗教訓。 [36] 使用協同作用，可以充分優化當前和未來火星任務（例如 ExoMars Trace Gas Orbiter）的最低點觀測的科學返回。 [37] 在這裡，我們在 2018 年 4 月至 2018 年 8 月期間使用 ESA-Roscosmos ExoMars Trace Gas Orbiter 上的 ACS 和 NOMAD 儀器報告了對火星大氣的高度敏感測量，以檢測甲烷。 [38] ExoMars Trace Gas Orbiter (TGO)、Emirates Mars Mission (EMM) 和未來可能的火星靜止衛星將提供有關火星大氣中塵埃和水冰雲光學深度的創新數據產品，時間分辨率為數小時. [39] 儘管由於測量不確定性很大，CH4 的存在仍在爭論中，但即將使用微量氣體軌道器 (TGO) 的 ESA-Roscosmos 任務將解決有關這種氣體的存在及其來源的問題。 [40] 在這裡，我們展示了在全球沙塵暴開始時對塵埃、水和半重水 (HDO) 的同時高分辨率測量，這些測量是由 ExoMars 微量氣體軌道器上的 NOMAD 和 ACS 儀器獲得的。 [41] Trace Gas Orbiter 宇宙飛船在運行的頭幾個月沒有在紅色星球的大氣層中發現這種氣體。 [42] 我們報告了使用 ExoMars 微量氣體軌道器上的大氣化學套件 (ACS) 的中紅外通道 (MIR) 獲得的火星大氣紅外測量結果。 [43] 火星探測儀 (NOMAD) 搭載在 ExoMars 微量氣體軌道飛行器 (TGO) 航天器上的最低點和掩星探測儀旨在觀察火星的太陽掩星、最低點和邊緣幾何形狀，並將能夠產生大量不同的數據，主要集中在大氣的特性上。 [44] 在這裡，我們展示了兩次沙塵暴期間的水蒸氣垂直剖面（Ls = 162-260° 和 Ls = 298-345°），來自天底和火星發現掩星 (NOMAD) 在 ExoMars Trace Gas Orbiter 上進行的太陽掩星測量（TGO）。 [45]
mid infrared channel 中紅外通道
Measurements by the Atmospheric Chemistry Suite mid-infrared channel (ACS MIR) on the ExoMars Trace Gas Orbiter allow us to measure the ratio of hydrogen chloride two stable isotopologues, H35Cl and H37Cl. [1] HCl was discovered in the atmosphere of Mars for the first time during the global dust storm in Mars year (MY) 34 (July 2018) using the Atmospheric Chemistry Suite mid-infrared channel (ACS MIR) on the ExoMars Trace Gas Orbiter. [2]通過 ExoMars 微量氣體軌道器上的大氣化學套件中紅外通道 (ACS MIR) 進行的測量使我們能夠測量氯化氫兩種穩定同位素體 H35Cl 和 H37Cl 的比率。 [1] 在火星年 (MY) 34（2018 年 7 月）的全球沙塵暴期間，使用 ExoMars 微量氣體軌道器上的大氣化學套件中紅外通道 (ACS MIR) 首次在火星大氣中發現了 HCl。 [2]
Trace Gas Orbiter 微量氣體軌道器
Solar occultations performed by the Nadir and Occultation for MArs Discovery (NOMAD) ultraviolet and visible spectrometer (UVIS) onboard the ExoMars Trace Gas Orbiter (TGO) have provided a comprehe. [1] The ExoMars Trace Gas Orbiter (TGO)’s Colour and Stereo Surface Imaging System (CaSSIS) provides multi-spectral optical imagery at 4-5m/pixel spatial resolution. [2] FREND is a neutron telescope installed onboard Russian-European ExoMars mission Trace Gas Orbiter. [3] Moreover, we note that numerous scenarios of methane fluxes from terrestrial analogs may explain non-detections by the ExoMars Trace Gas Orbiter (TGO), as they can produce atmospheric concentrations below the TGO limit of detection. [4] The Trace Gas Orbiter, the first element of the ExoMars programme, began its science phase in 2018 focusing on investigations of the atmospheric composition with unprecedented sensitivity as well as surface and subsurface studies. [5] Our results are based on solar occultation measurements by Atmospheric Chemistry Suite (ACS) onboard the ExoMars Trace Gas Orbiter (TGO). [6] Measurements by the Atmospheric Chemistry Suite mid-infrared channel (ACS MIR) on the ExoMars Trace Gas Orbiter allow us to measure the ratio of hydrogen chloride two stable isotopologues, H35Cl and H37Cl. [7] Here, we analyze data from the High Resolution Imaging Science Experiment (HiRISE) and from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instruments onboard NASA's Mars Reconnaissance Orbiter and the Colour and Stereo Surface Imaging System (CaSSIS) onboard ESA's Trace Gas Orbiter to characterize, at a high spatial resolution, the morphological and spectral variability of Oxia Planum's surface deposits. [8] Hydrogen chloride (HCl) was recently discovered in the atmosphere of Mars by two spectrometers onboard the ExoMars Trace Gas Orbiter. [9] We present simulations of the HDO cycle with the LMD Mars GCM and compare the retrieved cycle with observations provided by the Atmospheric Chemistry Suite (ACS) on board the ESA/Roscosmos Trace Gas Orbiter (TGO). [10] We demonstrate the wide applicability of this technique with the ExoMars Trace Gas Orbiter Colour and Stereo Surface Imaging System (CaSSIS) 4. [11] "The Colour and Stereo Surface Imaging System (CaSSIS) for the ExoMars Trace Gas Orbiter. [12] The paper summarises the results achieved, identifies lessons learned and gives an overview of what is coming next as ERCO prepares for its operational roll-out to support relay services provided by ESA's Trace Gas Orbiter to NASA's Curiosity and Perseverance Rovers. [13] Our intent is to complement and improve on the previously reported detection attempts by the Atmospheric Chemistry Suite(ACS) on board the ExoMars Trace Gas Orbiter (TGO). [14] 8 μm with the Atmospheric Chemistry Suite and confirmed with Nadir and Occultation for Mars Discovery instruments onboard the ExoMars Trace Gas Orbiter, reveal widely distributed HCl in the 1- to 4-ppbv range, 20 times greater than previously reported upper limits. [15] HCl was discovered in the atmosphere of Mars for the first time during the global dust storm in Mars year (MY) 34 (July 2018) using the Atmospheric Chemistry Suite mid-infrared channel (ACS MIR) on the ExoMars Trace Gas Orbiter. [16] CaSSIS is the multispectral stereo push frame camera on board ExoMars TGO (Trace Gas Orbiter) which will image 1. [17] More than a full Martian year of observations have now been made by the Nadir Occultation for MArs Discovery (NOMAD) instrument suite on-board the ExoMars Trace Gas Orbiter. [18] Here we report HDO and H2O profiles observed by the Atmospheric Chemistry Suite (ExoMars Trace Gas Orbiter) in orbit around Mars that, once combined with expected photolysis rates, reveal the prevalence of the perihelion season for the formation of atomic H and D at altitudes relevant for escape. [19] The Open University modelling group global circulation model is combined with retrievals from the ExoMars Trace Gas Orbiter (temperature and water vapour profiles from the Atmospheric Chemistry Suite and water vapour profiles from the Nadir and Occultation for Mars Discovery instrument) and the Mars Climate Sounder (temperature profiles and dust column) on the Mars Reconnaissance Orbiter. [20] This work takes advantage of the NOMAD spectrometer observations, on board the 2016 ExoMars Trace Gas Orbiter. [21] 3 µm in the atmosphere of Mars by ExoMars Trace Gas Orbiter ACS instrument. [22] The Atmospheric Chemistry Suite (ACS) is a set of three spectrometers (-NIR, -MIR, and -TIRVIM) intended to observe Mars atmosphere onboard the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission (Korablev et al. [23] 6 µm) spectra measured by TIRVIM and NIR instruments onboard the ExoMars Trace Gas Orbiter (TGO) in solar occultation geometry. [24] The Trace Gas Orbiter, TGO, is now well into its second Martian year of operations. [25] Here we report vertical profiles of CO from 10 to 120 km, and from a broad range of latitudes, inferred from the Atmospheric Chemistry Suite on board the ExoMars Trace Gas Orbiter. [26] This large day-night difference suggests that methane accumulates while contained near the surface at night, but drops below TLS-SAM detection limits during the day, consistent with the daytime nondetection by instruments on board the ExoMars Trace Gas Orbiter. [27] The Atmospheric Chemistry Suite on the ExoMars Trace Gas Orbiter has a spectral range that includes several absorption lines of PH3 with line strengths comparable to previously observed CH4 lines. [28] The ExoMars Trace Gas Orbiter (TGO) spacecraft has detected no methane on Mars despite having better sensitivity than Curiosity, but had not yet examined the Gale location. [29] Technical details of the method are described, and results are demonstrated using a 4 m/pixel Trace Gas Orbiter Colour and Stereo Surface Imaging System (CaSSIS) panchromatic image and an overlapping 6 m/pixel Mars Reconnaissance Orbiter Context Camera (CTX) stereo pair to produce a 1 m/pixel CaSSIS Super-Resolution Restoration (SRR) DTM for different areas over Oxia Planum on Mars—the future ESA ExoMars 2022 Rosalind Franklin rover’s landing site. [30] Purpose This paper aims to describe the development of a knowledge management system (KMS) for the Nadir and Occultation for Mars Discovery (NOMAD) instrument on board the ESA/Roscosmos 2016 ExoMars Trace Gas Orbiter (TGO) spacecraft. [31] The ExoMars Trace Gas Orbiter (TGO) began its nominal science phase at Mars in April 2018, following releases of editions to two major spectroscopic line lists: GEISA 2015 (Gestion et Etude des Informations Spectroscopiques Atmospheriques: Management and Study of Atmospheric Spectroscopic Information), and HITRAN 2016 (High Resolution Transmission). [32] We present a new data set of density perturbation amplitudes derived from accelerometer measurements during aerobraking of the European Space Agency’s Trace Gas Orbiter. [33] In this study we use images from the Colour and Stereo Surface Imaging System (CaSSIS) aboard ESA’s Trace Gas Orbiter (TGO) to study the relationship between surface frosts and gullies. [34] The Atmospheric Chemistry Suite (ACS) instrument onboard the ExoMars Trace Gas Orbiter (TGO) ESA-Roscosmos mission began science operations in March 2018. [35] This paper aims at giving a flight dynamics perspective on ExoMars Trace Gas Orbiter aerobraking operations, discussing the main challenges for both navigation and spacecraft commanding, describing the work-flow of activities within an operation cycle and presenting some results from the successful campaign, together with the most important lessons learnt. [36] Using synergy, the scientific return of nadir observations of current and future missions at Mars (such as the ExoMars Trace Gas Orbiter) can be fully optimized. [37] Here we report highly sensitive measurements of the atmosphere of Mars in an attempt to detect methane, using the ACS and NOMAD instruments onboard the ESA-Roscosmos ExoMars Trace Gas Orbiter from April to August 2018. [38] The ExoMars Trace Gas Orbiter (TGO), Emirates Mars Mission (EMM), and possible future Mars stationary satellite(s) will provide innovative data products on the optical depth of dust and water ice clouds in the Martian atmosphere with a temporal resolution of hours. [39] Although the presence of CH4 is still under debate because of large measurement uncertainties, the forthcoming ESA-Roscosmos mission, which employs the Trace Gas Orbiter (TGO), will settle questions on the existence of this gas and its origin. [40] Here we present concurrent, high-resolution measurements of dust, water and semiheavy water (HDO) at the onset of a global dust storm, obtained by the NOMAD and ACS instruments onboard the ExoMars Trace Gas Orbiter. [41] Trace Gas Orbiter spacecraft did not find the gas in red planet’s atmosphere during its first months of operation. [42] We report infrared measurements of the Martian atmosphere obtained with the mid-infrared channel (MIR) of the Atmospheric Chemistry Suite (ACS), onboard the ExoMars Trace Gas Orbiter. [43] The Nadir and Occultation for MArs Discovery instrument (NOMAD), onboard the ExoMars Trace Gas Orbiter (TGO) spacecraft was conceived to observe Mars in solar occultation, nadir, and limb geometries, and will be able to produce an outstanding amount of diverse data, mostly focused on properties of the atmosphere. [44] Here we present water vapor vertical profiles in the periods of the two dust storms (Ls = 162–260° and Ls = 298–345°) from the solar occultation measurements by Nadir and Occultation for Mars Discovery (NOMAD) onboard ExoMars Trace Gas Orbiter (TGO). [45]ExoMars Trace Gas Orbiter (TGO) 上的 Nadir 和 Occultation for MArs Discovery (NOMAD) 紫外和可見光譜儀 (UVIS) 進行的太陽掩星提供了一個全面的信息。 [1] ExoMars 微量氣體軌道器 (TGO) 的彩色和立體表面成像系統 (CaSSIS) 以 4-5m/像素的空間分辨率提供多光譜光學圖像。 [2] <p>FREND 是安裝在俄羅斯-歐洲 ExoMars 任務 Trace Gas Orbiter 上的中子望遠鏡。 [3] 此外，我們注意到來自陸地類似物的大量甲烷通量情景可能解釋了 ExoMars 微量氣體軌道器 (TGO) 未檢測到的原因，因為它們可以產生低於 TGO 檢測限的大氣濃度。 [4] 微量氣體軌道器是 ExoMars 計劃的第一個元素，於 2018 年開始其科學階段，重點以前所未有的靈敏度調查大氣成分以及地表和地下研究。 [5] 我們的結果基於 ExoMars 微量氣體軌道器 (TGO) 上的大氣化學套件 (ACS) 對太陽掩星的測量。 [6] 通過 ExoMars 微量氣體軌道器上的大氣化學套件中紅外通道 (ACS MIR) 進行的測量使我們能夠測量氯化氫兩種穩定同位素體 H35Cl 和 H37Cl 的比率。 [7] 在這裡，我們分析來自美國宇航局火星偵察軌道器上的高分辨率成像科學實驗 (HiRISE) 和緊湊型火星偵察成像光譜儀 (CRISM) 儀器以及歐空局微量氣體軌道器上的彩色和立體表面成像系統 (CaSSIS) 的數據，以以高空間分辨率表徵 Oxia Planum 表面沉積物的形態和光譜變化。 [8] ExoMars 微量氣體軌道器上的兩個光譜儀最近在火星大氣中發現了氯化氫 (HCl)。 [9]  </p> <p>我們使用 LMD Mars GCM 模擬 HDO 循環，並將檢索到的循環與 ESA/Roscosmos 痕量氣體軌道器 (TGO) 上的大氣化學套件 (ACS) 提供的觀測結果進行比較。 [10] 我們通過 ExoMars 示踪氣體軌道器顏色和立體表面成像系統 (CaSSIS) 4 展示了該技術的廣泛適用性。 [11] “用於 ExoMars 微量氣體軌道器的彩色和立體表面成像系統 (CaSSIS)。 [12] 該文件總結了取得的成果，確定了經驗教訓，並概述了 ERCO 準備其業務推出以支持 ESA 的微量氣體軌道器向 NASA 的好奇號和毅力號漫遊車提供的中繼服務。 [13] 我們的目的是補充和改進先前報告的 ExoMars 微量氣體軌道器 (TGO) 上的大氣化學套件 (ACS) 的檢測嘗試。 [14] 8 μm 使用 Atmospheric Chemistry Suite 並通過 ExoMars Trace Gas Orbiter 上的火星發現儀器的 Nadir 和 Occultation 確認，揭示了 1 至 4 ppbv 範圍內廣泛分佈的 HCl，比之前報導的上限高 20 倍。 [15] 在火星年 (MY) 34（2018 年 7 月）的全球沙塵暴期間，使用 ExoMars 微量氣體軌道器上的大氣化學套件中紅外通道 (ACS MIR) 首次在火星大氣中發現了 HCl。 [16] CaSSIS 是 ExoMars TGO（微量氣體軌道飛行器）上的多光譜立體推幀相機，它將對 1 進行成像。 [17] ExoMars 微量氣體軌道器上的火星探測天底掩星 (NOMAD) 儀器套件現已對火星進行了整整一年多的觀測。 [18] 在這裡，我們報告了大氣化學套件（ExoMars Trace Gas Orbiter）在火星軌道上觀察到的 HDO 和 H2O 剖面，一旦與預期的光解速率相結合，揭示了在相關高度形成原子 H 和 D 的近日點季節的普遍性為了逃跑。 [19] 開放大學建模小組全球環流模型與來自 ExoMars 微量氣體軌道器（大氣化學套件的溫度和水蒸氣剖面以及火星發現儀器的天底和掩星）和火星氣候探測儀（溫度輪廓和塵埃柱）在火星偵察軌道器上。 [20] <p>這項工作利用了 2016 年 ExoMars 微量氣體軌道器上的 NOMAD 光譜儀觀測結果。 [21] ExoMars Trace Gas Orbiter ACS 儀器在火星大氣中測量 3 µm。 [22] </p><p>大氣化學套件 (ACS) 是一組三個光譜儀（-NIR、-MIR 和 -TIRVIM），用於在 ESA-Roscosmos ExoMars 2016 微量氣體軌道飛行器 (TGO) 任務上觀察火星大氣（Korablev 等人。 [23] 6 µm) 光譜，由 ExoMars 微量氣體軌道器 (TGO) 上的 TIRVIM 和 NIR 儀器在太陽掩星幾何中測量。 [24] <p>TGO 微量氣體軌道器現已進入火星運行的第二個年頭。 [25] 在這裡，我們報告了從 ExoMars 微量氣體軌道器上的大氣化學套件推斷出的 10 到 120 km 以及來自廣泛緯度的 CO 垂直剖面。 [26] 這種巨大的晝夜差異表明，甲烷在夜間聚集在地表附近，但在白天低於 TLS-SAM 檢測限，這與 ExoMars 微量氣體軌道器上的儀器在白天未檢測到一致。 [27] ExoMars 微量氣體軌道器上的大氣化學套件的光譜範圍包括多個 PH3 吸收線，其線強度與之前觀察到的 CH4 線相當。 [28] ExoMars Trace Gas Orbiter (TGO) 宇宙飛船在火星上沒有檢測到甲烷，儘管它的靈敏度比好奇號更高，但尚未檢查大風的位置。 [29] 描述了該方法的技術細節，並使用 4 m/像素的示踪氣體軌道器彩色和立體表面成像系統 (CaSSIS) 全色圖像和重疊的 6 m/像素火星偵察軌道器上下文相機 (CTX) 立體對來演示結果為火星上 Oxia Planum 上的不同區域（未來的 ESA ExoMars 2022 Rosalind Franklin 漫遊者的著陸點）生成 1 m/像素的 CaSSIS 超分辨率恢復 (SRR) DTM。 [30] 目的 本文旨在描述 ESA/Roscosmos 2016 ExoMars 微量氣體軌道器 (TGO) 航天器上的火星探測天底和掩星 (NOMAD) 儀器知識管理系統 (KMS) 的開發。 [31] ExoMars 微量氣體軌道器 (TGO) 於 2018 年 4 月在火星開始其名義科學階段，隨後發布了兩個主要光譜線列表的版本：GEISA 2015（Gestion et Etude des Informations Spectroscopiques Atmospheriques：大氣光譜信息的管理和研究），和 HITRAN 2016（高分辨率傳輸）。 [32] 我們提出了一組新的密度擾動幅度數據集，該數據集源自歐洲航天局的微量氣體軌道器航空制動期間的加速度計測量值。 [33] 在這項研究中，我們使用來自 ESA 微量氣體軌道飛行器 (TGO) 上的彩色和立體表面成像系統 (CaSSIS) 的圖像來研究地表霜凍和溝壑之間的關係。 [34] ExoMars 微量氣體軌道器 (TGO) ESA-Roscosmos 任務上的大氣化學套件 (ACS) 儀器於 2018 年 3 月開始科學運行。 [35] 本文旨在從飛行動力學角度對 ExoMars Trace Gas Orbiter 航空制動操作進行討論，討論導航和航天器指揮的主要挑戰，描述操作週期內活動的工作流程，並介紹成功運動的一些結果，以及最重要的經驗教訓。 [36] 使用協同作用，可以充分優化當前和未來火星任務（例如 ExoMars Trace Gas Orbiter）的最低點觀測的科學返回。 [37] 在這裡，我們在 2018 年 4 月至 2018 年 8 月期間使用 ESA-Roscosmos ExoMars Trace Gas Orbiter 上的 ACS 和 NOMAD 儀器報告了對火星大氣的高度敏感測量，以檢測甲烷。 [38] ExoMars Trace Gas Orbiter (TGO)、Emirates Mars Mission (EMM) 和未來可能的火星靜止衛星將提供有關火星大氣中塵埃和水冰雲光學深度的創新數據產品，時間分辨率為數小時. [39] 儘管由於測量不確定性很大，CH4 的存在仍在爭論中，但即將使用微量氣體軌道器 (TGO) 的 ESA-Roscosmos 任務將解決有關這種氣體的存在及其來源的問題。 [40] 在這裡，我們展示了在全球沙塵暴開始時對塵埃、水和半重水 (HDO) 的同時高分辨率測量，這些測量是由 ExoMars 微量氣體軌道器上的 NOMAD 和 ACS 儀器獲得的。 [41] Trace Gas Orbiter 宇宙飛船在運行的頭幾個月沒有在紅色星球的大氣層中發現這種氣體。 [42] 我們報告了使用 ExoMars 微量氣體軌道器上的大氣化學套件 (ACS) 的中紅外通道 (MIR) 獲得的火星大氣紅外測量結果。 [43] 火星探測儀 (NOMAD) 搭載在 ExoMars 微量氣體軌道飛行器 (TGO) 航天器上的最低點和掩星探測儀旨在觀察火星的太陽掩星、最低點和邊緣幾何形狀，並將能夠產生大量不同的數據，主要集中在大氣的特性上。 [44] 在這裡，我們展示了兩次沙塵暴期間的水蒸氣垂直剖面（Ls = 162-260° 和 Ls = 298-345°），來自天底和火星發現掩星 (NOMAD) 在 ExoMars Trace Gas Orbiter 上進行的太陽掩星測量（TGO）。 [45]
gas orbiter colmy 氣體軌道器科爾米
We demonstrate the wide applicability of this technique with the ExoMars Trace Gas Orbiter Colour and Stereo Surface Imaging System (CaSSIS) 4. [1] Technical details of the method are described, and results are demonstrated using a 4 m/pixel Trace Gas Orbiter Colour and Stereo Surface Imaging System (CaSSIS) panchromatic image and an overlapping 6 m/pixel Mars Reconnaissance Orbiter Context Camera (CTX) stereo pair to produce a 1 m/pixel CaSSIS Super-Resolution Restoration (SRR) DTM for different areas over Oxia Planum on Mars—the future ESA ExoMars 2022 Rosalind Franklin rover’s landing site. [2]我們通過 ExoMars 示踪氣體軌道器顏色和立體表面成像系統 (CaSSIS) 4 展示了該技術的廣泛適用性。 [1] 描述了該方法的技術細節，並使用 4 m/像素的示踪氣體軌道器彩色和立體表面成像系統 (CaSSIS) 全色圖像和重疊的 6 m/像素火星偵察軌道器上下文相機 (CTX) 立體對來演示結果為火星上 Oxia Planum 上的不同區域（未來的 ESA ExoMars 2022 Rosalind Franklin 漫遊者的著陸點）生成 1 m/像素的 CaSSIS 超分辨率恢復 (SRR) DTM。 [2]