scholarly journals MIRS: an imaging spectrometer for the MMX mission

2021 ◽  
Vol 73 (1) ◽  
Author(s):  
Maria Antonietta Barucci ◽  
Jean-Michel Reess ◽  
Pernelle Bernardi ◽  
Alain Doressoundiram ◽  
Sonia Fornasier ◽  
...  
Keyword(s):  
Site Selection ◽  
Near Infrared ◽  
Surface Composition ◽  
Sampling Site ◽  
Close Collaboration ◽  
Imaging Spectrometer ◽  
Mars Atmosphere ◽  
Infrared Spectral ◽  
Infrared Spectrometer ◽  
Moon Exploration

AbstractThe MMX infrared spectrometer (MIRS) is an imaging spectrometer onboard MMX JAXA mission. MMX (Martian Moon eXploration) is scheduled to be launched in 2024 with sample return to Earth in 2029. MIRS is built at LESIA-Paris Observatory in collaboration with four other French laboratories, collaboration and financial support of CNES and close collaboration with JAXA and MELCO. The instrument is designed to fully accomplish MMX’s scientific and measurement objectives. MIRS will remotely provide near-infrared spectral maps of Phobos and Deimos containing compositional diagnostic spectral features that will be used to analyze the surface composition and to support the sampling site selection. MIRS will also study Mars atmosphere, in particular spatial and temporal changes such as clouds, dust and water vapor. Graphical Abstract

scholarly journals Photometric Normalization of Chang’e-4 Visible and Near-Infrared Imaging Spectrometer Datasets: A Combined Study of In-Situ and Laboratory Spectral Measurements

2020 ◽  
Vol 12 (19) ◽  
pp. 3211
Author(s):  
Xiaobin Qi ◽  
Zongcheng Ling ◽  
Jiang Zhang ◽  
Jian Chen ◽  
Haijun Cao ◽  
...  
Keyword(s):  
Near Infrared ◽  
Infrared Imaging ◽  
Landing Site ◽  
Near Infrared Imaging ◽  
Imaging Spectrometer ◽  
Quantitative Mineralogy ◽  
Infrared Spectral ◽  
Phase Functions ◽  
Phase Angles

Until 29 May 2020, the Visible and Near-Infrared Imaging Spectrometer (VNIS) onboard the Yutu-2 Rover of the Chang’e-4 (CE-4) has acquired 96 high-resolution surface in-situ imaging spectra. These spectra were acquired under different illumination conditions, thus photometric normalization should be conducted to correct the introduced albedo differences before deriving the quantitative mineralogy for accurate geologic interpretations. In this study, a Lommel–Seeliger (LS) model and Hapke radiative transfer (Hapke) model were used and empirical phase functions of the LS model were derived. The values of these derived phase functions exhibit declining trends with the increase in phase angles and the opposition effect and phase reddening effect were observed. Then, we discovered from in-situ and laboratory measurements that the shadows caused by surface roughness have significant impacts on reflectance spectra and proper corrections were introduced. The validations of different phase functions showed that the maximum discrepancy at 1500 nm of spectra corrected by the LS model was less (~3.7%) than that by the Hapke model (~7.4%). This is the first time that empirical phase functions have been derived for a wavelength from 450 to 2395 nm using in-situ visible and near-infrared spectral datasets. Generally, photometrically normalized spectra exhibit smaller spectral slopes, lower FeO contents and larger optical maturity parameter (OMAT) than spectra without correction. In addition, the band centers of the 1 and 2 μm absorption features of spectra after photometric normalization exhibit a more concentrated distribution, indicating the compositional homogeneity of soils at the CE-4 landing site.

scholarly journals Near-Infrared Spectral Geometric Albedos of Charon and Pluto: Constraints on Charon's Surface Composition

Icarus ◽  
1996 ◽  
Vol 119 (1) ◽  
pp. 214-218 ◽  
Author(s):  
Ted L. Roush ◽  
Dale P. Cruikshank ◽  
James B. Pollack ◽  
Eliot F. Young ◽  
Mary J. Bartholomew
Keyword(s):  
Near Infrared ◽  
Surface Composition ◽  
Infrared Spectral

The surface composition of asteroid 162173 Ryugu from Hayabusa2 near-infrared spectroscopy

Science ◽  
2019 ◽  
pp. eaav7432 ◽  
Author(s):  
K. Kitazato ◽  
R. E. Milliken ◽  
T. Iwata ◽  
M. Abe ◽  
M. Ohtake ◽  
...  
Keyword(s):  
Near Infrared ◽  
Surface Composition ◽  
Parent Body ◽  
Absorption Feature ◽  
Direct Measurements ◽  
Band Position ◽  
Infrared Spectrometer ◽  
Sample Return Mission ◽  
Near Infrared Spectrometer ◽  
Rubble Pile

The near-Earth asteroid 162173 Ryugu, the target of Hayabusa2 sample return mission, is thought to be a primitive carbonaceous object. We report reflectance spectra of Ryugu’s surface acquired with the Near Infrared Spectrometer (NIRS3) on Hayabusa2, to provide direct measurements of the surface composition and geological context for the returned samples. A weak, narrow absorption feature centered at 2.72 μm was detected across the entire observed surface, indicating that hydroxyl (OH)-bearing minerals are ubiquitous there. The intensity of the OH feature and low albedo are similar to thermally- and/or shock-metamorphosed carbonaceous chondrite meteorites. There are few variations in the OH-band position, consistent with Ryugu being a compositionally homogeneous rubble-pile object, generated from impact fragments of an undifferentiated aqueously altered parent body.

Phobos composition: a reappraisal, based on Omega/MEx observations

2020 ◽  
Author(s):  
Brigitte Gondet ◽  
Jean-Pierre Bibring
Keyword(s):  
Spatial Resolution ◽  
Spectral Range ◽  
Near Infrared ◽  
Compositional Data ◽  
Data Sets ◽  
Imaging Spectrometer ◽  
Mars Express ◽  
Infrared Spectral Range ◽  
Infrared Spectral ◽  
Spectral Channels

<p>The imaging spectrometer OMEGA [1] operates in the VIS-NIR range, covering the (0.35 µm to 5.1 µm) range in 352 contiguous spectral channels.  This spectral range has been chosen as it includes diagnostic signatures of most surface mafic and hydrated minerals, frosts and ices. With a 1.2 mrad IFOV, the footprint varies from 40 m when imaging from 40 kms, up to 4.8 km from an altitude of 4000 km: this allows a global spectral coverage of Phobos to be achieved, at various spatial resolution.</p><p>Along its 16 years of orbital operations, Mars Express has performed tens of close flybys of Phobos, at altitudes down to ~ 50 kms. OMEGA has acquired unprecedented compositional data sets, in both the visible and the near-infrared spectral range. We shall present and discuss these observations, as witnesses of Phobos origin, with their relevance to the upcoming MMX JAXA mission.</p>

scholarly journals Mineralogical characterization of Martian Jezero crater from MRO CRISM hyperspectral images

2014 ◽  
Vol XL-4 ◽  
pp. 117-119 ◽  
Author(s):  
S. Jin ◽  
Y. Yang
Keyword(s):  
Near Infrared ◽  
Chemical Induction ◽  
Martian Surface ◽  
Large Area ◽  
Mineralogical Characterization ◽  
Imaging Spectrometer ◽  
Spectral Angle Mapper ◽  
Mineral Components ◽  
Infrared Spectrometer ◽  
Near Infrared Spectrometer

Martian mineral detection and mapping can provide important information and constraints on Martian aqueous history, which can be used to assess the potential habitability of Mars. The key parameters to Martian aqueous alteration are the depth and extent of the Martian hydrous mineral. Therefore, it is important to know detailed minerals and chemical induction of the existence of water on the Martian surface at past or present. The Jezero crater located in the Nili Fossae region of Mars is the once-flooded crater, which has rich fan-delta deposit clays. It is a good case to study the clays and mineral components at Jezero crater, so as to know the geogloical processes and evolution on Mars. The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) aboard the Mars Reconnaissance Orbiter (MRO) is a visible and near infrared spectrometer with enhanced spectral resolution, which provides an opportunity to map detailed and large-area mineralogy on Mars. In this paper, CRISM nearinfrared spectral data are analyzed using the mixture tuned filtering (MTMF) along with spectral angle mapper (SAM), and mineral components at Martian Jezero region are recognized, including the phyllosilicate, carbonate, nitrates and tectosil. Some detailed characteristics and implications of minerals at Martian Jezero crater are further studied and discussed, including implications on Martian climate change and geological evolution.

scholarly journals O2 signature in thin and thick O2−H2O ices

2018 ◽  
Vol 620 ◽  
pp. A46 ◽  
Author(s):  
B. Müller ◽  
B. M. Giuliano ◽  
L. Bizzocchi ◽  
A. I. Vasyunin ◽  
P. Caselli
Keyword(s):  
Near Infrared ◽  
Pure Water ◽  
Future Mission ◽  
Infrared Spectral ◽  
Infrared Spectrometer ◽  
The One ◽  
Dust Grain ◽  
Comet 67P ◽  
O 10

Aims. In this paper we investigate the detectability of the molecular oxygen in icy dust grain mantles towards astronomical objects. Methods. We present a systematic set of experiments with O2−H2O ice mixtures designed to disentangle how the molecular ratio affects the O2 signature in the mid- and near-infrared spectral regions. All the experiments were conducted in a closed-cycle helium cryostat coupled to a Fourier transform infrared spectrometer. The ice mixtures comprise varying thicknesses from 8 × 10−3 to 3 μm. The absorption spectra of the O2−H2O mixtures are also compared to the one of pure water. In addition, the possibility to detect the O2 in icy bodies and in the interstellar medium is discussed. Results. We are able to see the O2 feature at 1551 cm−1 even for the most diluted mixture of H2O:O2 = 9:1, comparable to a ratio of O2/H2O = 10% which has already been detected in situ in the coma of the comet 67P/Churyumov-Gerasimenko. We provide an estimate for the detection of O2 with the future mission of the James Webb Space Telescope (JWST).

Quantum Ring Infrared Photodetector Based On Droplet Epitaxy Technique

2009 ◽  
Vol 1208 ◽  
Author(s):  
Dali Shao ◽  
Jiang Wu ◽  
Zhenghua Li ◽  
Omar Manasreh ◽  
Vasyl P Kunets ◽  
...  
Keyword(s):  
Near Infrared ◽  
Droplet Epitaxy ◽  
Quantum Ring ◽  
Infrared Photodetector ◽  
Mid Infrared ◽  
Quantum Rings ◽  
Force Microscopy ◽  
Atomic Force ◽  
Infrared Spectral ◽  
Infrared Spectrometer

AbstractIn this work, we design and fabricate a GaAs quantum ring infrared photodetector. The lattice matched GaAs/Al0.3Ga0.7As quantum rings are grown by using molecular beam epitaxy technique. The morphology of the quantum rings are characterized by an atomic force microscopy. Normal incident configured photodetectors are fabricated by standard photolithography. The photoresponse spectra are measured by a Fourier transform infrared spectrometer and exhibit two broad bands in visible-near-infrared and mid-infrared spectral range. Using quantum rings as absorption medium, we observed visible-near-infrared response at a temperature as high as 300 K while mid-infrared response up to 140 K.

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