1
|
Oliva F, D’Aversa E, Bellucci G, Carrozzo FG, Ruiz Lozano L, Altieri F, Thomas IR, Karatekin O, Cruz Mermy G, Schmidt F, Robert S, Vandaele AC, Daerden F, Ristic B, Patel MR, López‐Moreno J, Sindoni G. Martian CO 2 Ice Observation at High Spectral Resolution With ExoMars/TGO NOMAD. J Geophys Res Planets 2022; 127:e2021JE007083. [PMID: 35865508 PMCID: PMC9286783 DOI: 10.1029/2021je007083] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 10/04/2021] [Revised: 04/16/2022] [Accepted: 04/19/2022] [Indexed: 06/15/2023]
Abstract
The Nadir and Occultation for MArs Discovery (NOMAD) instrument suite aboard ExoMars/Trace Gas Orbiter spacecraft is mainly conceived for the study of minor atmospheric species, but it also offers the opportunity to investigate surface composition and aerosols properties. We investigate the information content of the Limb, Nadir, and Occultation (LNO) infrared channel of NOMAD and demonstrate how spectral orders 169, 189, and 190 can be exploited to detect surface CO2 ice. We study the strong CO2 ice absorption band at 2.7 μm and the shallower band at 2.35 μm taking advantage of observations across Martian Years 34 and 35 (March 2018 to February 2020), straddling a global dust storm. We obtain latitudinal-seasonal maps for CO2 ice in both polar regions, in overall agreement with predictions by a general climate model and with the Mars Express/OMEGA spectrometer Martian Years 27 and 28 observations. We find that the narrow 2.35 μm absorption band, spectrally well covered by LNO order 189, offers the most promising potential for the retrieval of CO2 ice microphysical properties. Occurrences of CO2 ice spectra are also detected at low latitudes and we discuss about their interpretation as daytime high altitude CO2 ice clouds as opposed to surface frost. We find that the clouds hypothesis is preferable on the basis of surface temperature, local time and grain size considerations, resulting in the first detection of CO2 ice clouds through the study of this spectral range. Through radiative transfer considerations on these detections we find that the 2.35 μm absorption feature of CO2 ice clouds is possibly sensitive to nm-sized ice grains.
Collapse
Affiliation(s)
- F. Oliva
- Istituto di Astrofisica e Planetologia Spaziali (IAPS/INAF)RomeItaly
| | - E. D’Aversa
- Istituto di Astrofisica e Planetologia Spaziali (IAPS/INAF)RomeItaly
| | - G. Bellucci
- Istituto di Astrofisica e Planetologia Spaziali (IAPS/INAF)RomeItaly
| | - F. G. Carrozzo
- Istituto di Astrofisica e Planetologia Spaziali (IAPS/INAF)RomeItaly
| | - L. Ruiz Lozano
- Université Catholique de Louvain‐la‐Neuve (UCLouvain)Louvain‐la‐NeuveBelgium
- Royal Observatory of BelgiumBrusselsBelgium
| | - F. Altieri
- Istituto di Astrofisica e Planetologia Spaziali (IAPS/INAF)RomeItaly
| | - I. R. Thomas
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | | | | | - F. Schmidt
- CNRSGEOPSUniversité Paris‐SaclayOrsayFrance
- Institut Universitaire de France (IUF)ParisFrance
| | - S. Robert
- Université Catholique de Louvain‐la‐Neuve (UCLouvain)Louvain‐la‐NeuveBelgium
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | - A. C. Vandaele
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | - F. Daerden
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | - B. Ristic
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | - M. R. Patel
- School of Physical SciencesThe Open UniversityMilton KeynesUK
| | - J.‐J. López‐Moreno
- Instituto de Astrofìsica de Andalucia (IAA)Consejo Superior de Investigaciones Científicas (CSIC)GranadaSpain
| | - G. Sindoni
- Agenzia Spaziale Italiana (ASI)RomeItaly
| |
Collapse
|
2
|
Rousseau B, De Sanctis MC, Raponi A, Ciarniello M, Ammannito E, Scarica P, Fonte S, Frigeri A, Carrozzo FG, Tosi F. Correction of the VIR-visible dataset from the Dawn mission at Vesta. Rev Sci Instrum 2020; 91:123102. [PMID: 33379964 DOI: 10.1063/5.0022902] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/27/2020] [Accepted: 11/15/2020] [Indexed: 06/12/2023]
Abstract
This work describes the correction method applied to the dataset acquired at the asteroid (4) Vesta by the visible channel of the visible and infrared mapping spectrometer. The rising detector temperature during data acquisitions in the visible wavelengths leads to a spectral slope increase over the whole spectral range. This limits the accuracy of the studies of the Vesta surface in this wavelength range. Here, we detail an empirical method to correct for the visible detector temperature dependency while taking into account the specificity of the Vesta dataset.
Collapse
Affiliation(s)
- B Rousseau
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - M C De Sanctis
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - A Raponi
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - M Ciarniello
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - E Ammannito
- Italian Space Agency (ASI), Via del Politecnico, 00133 Rome, Italy
| | - P Scarica
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - S Fonte
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - A Frigeri
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - F G Carrozzo
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - F Tosi
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| |
Collapse
|
3
|
Rousseau B, Raponi A, Ciarniello M, Ammannito E, Carrozzo FG, De Sanctis MC, Fonte S, Frigeri A, Tosi F. Correction of the VIR-visible data set from the Dawn mission. Rev Sci Instrum 2019; 90:123110. [PMID: 31893819 DOI: 10.1063/1.5123362] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/05/2019] [Accepted: 11/24/2019] [Indexed: 06/10/2023]
Abstract
Data acquired at Ceres by the visible channel of the Visible and InfraRed mapping spectrometer (VIR) on board the NASA Dawn spacecraft are affected by the temperatures of both the visible (VIS) and the infrared (IR) sensors, which are, respectively, a charged coupled device and a HgCdTe array. The variations of the visible channel temperatures measured during the sessions of acquisitions are correlated with the variations in the spectral slope and shape for all the mission phases. The IR channel temperature is more stable during the acquisitions; nonetheless, it is characterized by a bimodal distribution whether the cryocooler (and, therefore, the IR channel) is used or not during the visible channel operations. When the infrared channel temperature is high (175 K, i.e., not in use and with the cryocooler off), an additional negative slope and a distortion are observed in the spectra of the visible channel. We developed an empirical correction based on a reference spectrum for the whole dataset; it is designed to correct the two issues related to the sensor temperatures that we have identified. The reference spectrum is calculated to be representative of the global Ceres' surface. It is also made of the data acquired when the visible and infrared channel temperatures are equal to the ones measured during an observation of the Arcturus star by VIR, which is consistent with several ground-based observations. The developed correction allows reliable analysis and mapping to be performed by minimizing the artifacts induced by fluctuations of the VIS temperature. Thanks to this correction, a direct comparison between different mission phases during which the VIR experienced different visible and infrared channel temperatures is now possible.
Collapse
Affiliation(s)
- B Rousseau
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - A Raponi
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - M Ciarniello
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - E Ammannito
- Italian Space Agency (ASI), Via del Politecnico, 00133 Rome, Italy
| | - F G Carrozzo
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - M C De Sanctis
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - S Fonte
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - A Frigeri
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - F Tosi
- IAPS-INAF, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| |
Collapse
|
4
|
De Sanctis MC, Ammannito E, McSween HY, Raponi A, Marchi S, Capaccioni F, Capria MT, Carrozzo FG, Ciarniello M, Fonte S, Formisano M, Frigeri A, Giardino M, Longobardo A, Magni G, McFadden LA, Palomba E, Pieters CM, Tosi F, Zambon F, Raymond CA, Russell CT. Localized aliphatic organic material on the surface of Ceres. Science 2017; 355:719-722. [PMID: 28209893 DOI: 10.1126/science.aaj2305] [Citation(s) in RCA: 132] [Impact Index Per Article: 18.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/16/2016] [Accepted: 01/17/2017] [Indexed: 11/02/2022]
Abstract
Organic compounds occur in some chondritic meteorites, and their signatures on solar system bodies have been sought for decades. Spectral signatures of organics have not been unambiguously identified on the surfaces of asteroids, whereas they have been detected on cometary nuclei. Data returned by the Visible and InfraRed Mapping Spectrometer on board the Dawn spacecraft show a clear detection of an organic absorption feature at 3.4 micrometers on dwarf planet Ceres. This signature is characteristic of aliphatic organic matter and is mainly localized on a broad region of ~1000 square kilometers close to the ~50-kilometer Ernutet crater. The combined presence on Ceres of ammonia-bearing hydrated minerals, water ice, carbonates, salts, and organic material indicates a very complex chemical environment, suggesting favorable environments to prebiotic chemistry.
Collapse
Affiliation(s)
- M C De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - E Ammannito
- Earth Planetary and Space Sciences, University of California-Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA.,Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - H Y McSween
- Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996-1410, USA
| | - A Raponi
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - S Marchi
- Southwest Research Institute, Boulder, CO 80302, USA.,Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - F Capaccioni
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M T Capria
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - F G Carrozzo
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M Ciarniello
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - S Fonte
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M Formisano
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - A Frigeri
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M Giardino
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - A Longobardo
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - G Magni
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - L A McFadden
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - E Palomba
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - C M Pieters
- Brown University, Department of Earth, Environmental, and Planetary Sciences, Providence, RI 02912, USA
| | - F Tosi
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - F Zambon
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - C A Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA
| | - C T Russell
- Earth Planetary and Space Sciences, University of California-Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA
| |
Collapse
|
5
|
Carrozzo FG, Raponi A, De Sanctis MC, Ammannito E, Giardino M, D'Aversa E, Fonte S, Tosi F. Artifacts reduction in VIR/Dawn data. Rev Sci Instrum 2016; 87:124501. [PMID: 28040950 DOI: 10.1063/1.4972256] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/06/2023]
Abstract
Remote sensing images are generally affected by different types of noise that degrade the quality of the spectral data (i.e., stripes and spikes). Hyperspectral images returned by a Visible and InfraRed (VIR) spectrometer onboard the NASA Dawn mission exhibit residual systematic artifacts. VIR is an imaging spectrometer coupling high spectral and spatial resolutions in the visible and infrared spectral domain (0.25-5.0 μm). VIR data present one type of noise that may mask or distort real features (i.e., spikes and stripes), which may lead to misinterpretation of the surface composition. This paper presents a technique for the minimization of artifacts in VIR data that include a new instrument response function combining ground and in-flight radiometric measurements, correction of spectral spikes, odd-even band effects, systematic vertical stripes, high-frequency noise, and comparison with ground telescopic spectra of Vesta and Ceres. We developed a correction of artifacts in a two steps process: creation of the artifacts matrix and application of the same matrix to the VIR dataset. In the approach presented here, a polynomial function is used to fit the high frequency variations. After applying these corrections, the resulting spectra show improvements of the quality of the data. The new calibrated data enhance the significance of results from the spectral analysis of Vesta and Ceres.
Collapse
Affiliation(s)
- F G Carrozzo
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - A Raponi
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - M C De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - E Ammannito
- Institute of Geophysics and Planetary Physics, University of California Los Angeles, 595 Charles Young Drive East, Los Angeles, California 90095-1567, USA
| | - M Giardino
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - E D'Aversa
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - S Fonte
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - F Tosi
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, Via Fosso del Cavaliere 100, 00133 Rome, Italy
| |
Collapse
|
6
|
Ammannito E, DeSanctis MC, Ciarniello M, Frigeri A, Carrozzo FG, Combe JP, Ehlmann BL, Marchi S, McSween HY, Raponi A, Toplis MJ, Tosi F, Castillo-Rogez JC, Capaccioni F, Capria MT, Fonte S, Giardino M, Jaumann R, Longobardo A, Joy SP, Magni G, McCord TB, McFadden LA, Palomba E, Pieters CM, Polanskey CA, Rayman MD, Raymond CA, Schenk PM, Zambon F, Russell CT. Distribution of phyllosilicates on the surface of Ceres. Science 2016; 353:353/6303/aaf4279. [PMID: 27701086 DOI: 10.1126/science.aaf4279] [Citation(s) in RCA: 146] [Impact Index Per Article: 18.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/05/2016] [Accepted: 07/29/2016] [Indexed: 11/02/2022]
Abstract
The dwarf planet Ceres is known to host phyllosilicate minerals at its surface, but their distribution and origin have not previously been determined. We used the spectrometer onboard the Dawn spacecraft to map their spatial distribution on the basis of diagnostic absorption features in the visible and near-infrared spectral range (0.25 to 5.0 micrometers). We found that magnesium- and ammonium-bearing minerals are ubiquitous across the surface. Variations in the strength of the absorption features are spatially correlated and indicate considerable variability in the relative abundance of the phyllosilicates, although their composition is fairly uniform. These data, along with the distinctive spectral properties of Ceres relative to other asteroids and carbonaceous meteorites, indicate that the phyllosilicates were formed endogenously by a globally widespread and extensive alteration process.
Collapse
Affiliation(s)
- E Ammannito
- Earth Planetary and Space Sciences, University of California-Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA.
| | - M C DeSanctis
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M Ciarniello
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - A Frigeri
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - F G Carrozzo
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - J-Ph Combe
- The Bear Fight Institute, Winthrop, WA 98862, USA
| | - B L Ehlmann
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - S Marchi
- Southwest Research Institute, Boulder, CO 80302, USA
| | - H Y McSween
- Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996-1410, USA
| | - A Raponi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M J Toplis
- Institut de Recherche en Astrophysique et Planétologie (UMR 5277), Université de Toulouse, F-31400 Toulouse, France
| | - F Tosi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - J C Castillo-Rogez
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - F Capaccioni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M T Capria
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - S Fonte
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M Giardino
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - R Jaumann
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt, 12489 Berlin, Germany
| | - A Longobardo
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - S P Joy
- Earth Planetary and Space Sciences, University of California-Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA
| | - G Magni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - T B McCord
- The Bear Fight Institute, Winthrop, WA 98862, USA
| | - L A McFadden
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - E Palomba
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - C M Pieters
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - C A Polanskey
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - M D Rayman
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - C A Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - P M Schenk
- Lunar and Planetary Institute, Houston, TX 77058, USA
| | - F Zambon
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - C T Russell
- Earth Planetary and Space Sciences, University of California-Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA
| |
Collapse
|