Design of telescopic nadir imager for geomorphology (TENGOO) and observation of surface reflectance by optical chromatic imager (OROCHI) for the Martian Moons Exploration (MMX)

Kameda, Shingo; Ozaki, Masanobu; Enya, Keigo; Fuse, Ryota; Kouyama, Toru; Sakatani, Naoya; Suzuki, Hidehiko; Osada, Naoya; Kato, Hideki; Miyamoto, H.; Yamazaki, Atsushi; Nakamura, Tomoki; Okamoto, Tsukasa; Ishimaru, Takahiro; Peng, Hong; Ishibashi, Ko; Takashima, Takeshi; Ishigami, Ryoya; Kuo, Cheng-Ling; Abe, Shinsuke; Goda, Yuya; Murao, Hajime; Fujishima, Saori; Aoyama, Tsubasa; Hagiwara, Keiji; Mizumoto, Satoko; Tanaka, Noriko; Murakami, Kousuke; Matsumoto, Miho; Tanaka, Kenji; Sakuta, Hironobu

doi:10.1186/s40623-021-01462-9

Cited by 18 publications

(17 citation statements)

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“…Optical radiometer composed of chromatic imagers (OROCHI) is designed for capturing spectral features of Phobos from ultraviolet to near-infrared wavelengths with 7 wide-angle bandpass imagers and 1 panchromatic imager. Detailed information of design and performance of OROCHI is introduced in Kameda et al (2021).…”

Section: Instrumentsmentioning

confidence: 99%

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The Mars system revealed by the Martian Moons eXploration mission

Ogohara

Nakagawa

Aoki

et al. 2022

Earth Planets Space

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Japan Aerospace Exploration Agency (JAXA) plans a Phobos sample return mission (MMX: Martian Moons eXploration). In this study, we review the related works on the past climate of Mars, its evolution, and the present climate and weather to describe the scientific goals and strategies of the MMX mission regarding the evolution of the Martian surface environment. The MMX spacecraft will retrieve and return a sample of Phobos regolith back to Earth in 2029. Mars ejecta are expected to be accumulated on the surface of Phobos without being much shocked. Samples from Phobos probably contain all types of Martian rock from sedimentary to igneous covering all geological eras if ejecta from Mars could be accumulated on the Phobos surface. Therefore, the history of the surface environment of Mars can be restored by analyzing the returned samples. Remote sensing of the Martian atmosphere and monitoring ions escaping to space while the spacecraft is orbiting Mars in the equatorial orbit are also planned. The camera with multi-wavelength filters and the infrared spectrometer onboard the spacecraft can monitor rapid transport processes of water vapor, dust, ice clouds, and other species, which could not be traced by the previous satellites on the sun-synchronous polar orbit. Such time-resolved pictures of the atmospheric phenomena should be an important clue to understand both the processes of water exchange between the surface/underground reservoirs and the atmosphere and the drivers of efficient material transport to the upper atmosphere. The mass spectrometer with unprecedented mass resolution can observe ions escaping to space and monitor the atmospheric escape which has made the past Mars to evolve towards the cold and dry surface environment we know today. Together with the above two instruments, it can potentially reveal what kinds of atmospheric events can transport tracers (e.g., H2O) upward and enhance the atmospheric escape. Graphical Abstract

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Section: Instrumentsmentioning

confidence: 99%

“…The center wavelengths of the OROCHI bandpass filters are 390 nm, 480 nm, 550 nm, 650 nm, 730 nm, 860 nm, and 950 nm, and designed signal-to-noise (S/N) ratio for spectral analysis (i.e., band ratios) is 100 (Kameda et al 2021). For Mars observation, the blue and red bands will be mainly used for monitoring atmospheric dynamics.…”

Section: Instrumentsmentioning

confidence: 99%

The Mars system revealed by the Martian Moons eXploration mission

Ogohara

Nakagawa

Aoki

et al. 2022

Earth Planets Space

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“…MMX near-infrared spectrometer (MIRS) equipped with a scanning mirror to follow the along-track direction of ± 20° capacity will obtain reflectance spectra with a wavelength range from 0.9 to 3.6 µm to characterize surface minerals of Phobos and Deimos (Barucci et al 2021). Observation of surface Reflectance by Optical Chromatic Imager (OROCHI) is composed of seven wide-angle bandpass imagers with center wavelengths of 390 nm, 480 nm, 550 nm, 650 nm, 730 nm, 860 nm, and 950 nm (Kameda et al 2021), and the main objective is to acquire spectral mapping. Telescopic Nadir Imager for Geomorphology (TENGOO) is a visible telescope camera that obtains high resolution images to reveal the geomorphological feature of Phobos and Deimos (Kameda et al 2021).…”

Section: Scientific Observation Plan For Phobos By Individual Apparatus In Phase 1 Andmentioning

confidence: 99%

“…Observation of surface Reflectance by Optical Chromatic Imager (OROCHI) is composed of seven wide-angle bandpass imagers with center wavelengths of 390 nm, 480 nm, 550 nm, 650 nm, 730 nm, 860 nm, and 950 nm (Kameda et al 2021), and the main objective is to acquire spectral mapping. Telescopic Nadir Imager for Geomorphology (TENGOO) is a visible telescope camera that obtains high resolution images to reveal the geomorphological feature of Phobos and Deimos (Kameda et al 2021). Mars-moon Exploration with GAmma rays and Neutrons (MEGANE) is a gamma-ray and neutron spectrometer that measures major element composition of Phobos (Lawrence et al 2019).…”

Section: Scientific Observation Plan For Phobos By Individual Apparatus In Phase 1 Andmentioning

confidence: 99%

“…Similar to MIRS, OROCHI observation aims to provide a global spectroscopic mapping by seven cameras with different band-pass filters with sufficient signal to noise level (> 100, Kameda et al 2021) to understand visible spectral variation and material distribution of Phobos. Because OROCHI has a wide field of view (Table 2), each image can cover from south to north polar regions from QSO-H and at the same time OROCHI observes Phobos with a sufficient spatial resolution similar to MIRS (Fig.…”

Section: Qso-hmentioning

confidence: 99%

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Science operation plan of Phobos and Deimos from the MMX spacecraft

Nakamura

Ikeda

Kouyama³

et al. 2021

Earth Planets Space

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The science operations of the spacecraft and remote sensing instruments for the Martian Moon eXploration (MMX) mission are discussed by the mission operation working team. In this paper, we describe the Phobos observations during the first 1.5 years of the spacecraft’s stay around Mars, and the Deimos observations before leaving the Martian system. In the Phobos observation, the spacecraft will be placed in low-altitude quasi-satellite orbits on the equatorial plane of Phobos and will make high-resolution topographic and spectroscopic observations of the Phobos surface from five different altitudes orbits. The spacecraft will also attempt to observe polar regions of Phobos from a three-dimensional quasi-satellite orbit moving out of the equatorial plane of Phobos. From these observations, we will constrain the origin of Phobos and Deimos and select places for landing site candidates for sample collection. For the Deimos observations, the spacecraft will be injected into two resonant orbits and will perform many flybys to observe the surface of Deimos over as large an area as possible. Graphical Abstract

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Comet Interceptor Mission

Jones

Snodgrass

Tubiana

et al. 2021

Encyclopedia of Astrobiology

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Here we describe the novel, multi-point Comet Interceptor mission. It is dedicated to the exploration of a little-processed long-period comet, possibly entering the inner Solar System for the first time, or to encounter an interstellar object originating at another star. The objectives of the mission are to address the following questions: What are the surface composition, shape, morphology, and structure of the target object? What is the composition of the gas and dust in the coma, its connection to the nucleus, and the nature of its interaction with the solar wind? The mission was proposed to the European Space Agency in 2018, and formally adopted by the agency in June 2022, for launch in 2029 together with the Ariel mission. Comet Interceptor will take advantage of the opportunity presented by ESA's F-Class call for fast, flexible, low-cost missions to which it was proposed. The call required a launch to a halo orbit around the Sun-Earth L2 point. The mission can take advantage of this placement to wait for the discovery of a suitable comet reachable with its minimum ΔV capability of 600 ms −1 . Comet Interceptor will be unique in encountering and studying, at a nominal closest approach distance of 1000 km, a comet that represents a near-pristine sample of material from the formation of the Solar System. It will also add a capability that no previous cometary mission has had, which is to deploy two sub-probes -B1, provided by the Japanese space agency, JAXA, and B2 -that will follow different trajectories through the coma. While the main probe passes at a nominal 1000 km distance, probes B1 and B2 will follow different chords through the coma at distances of 850 km and 400 km, respectively. The result will be unique, simultaneous, spatially resolved information of the 3-dimensional properties of the target comet and its interaction with the space environment. We present the mission's science background leading to these objectives, as well as an overview of the scientific instruments, mission design, and schedule.

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Design of telescopic nadir imager for geomorphology (TENGOO) and observation of surface reflectance by optical chromatic imager (OROCHI) for the Martian Moons Exploration (MMX)

Cited by 18 publications

References 13 publications

The Mars system revealed by the Martian Moons eXploration mission

The Mars system revealed by the Martian Moons eXploration mission

Science operation plan of Phobos and Deimos from the MMX spacecraft

Comet Interceptor Mission

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