Martian moons exploration MMX: sample return mission to Phobos elucidating formation processes of habitable planets

Kuramoto, Kiyoshi; Kawakatsu, Yasuhiro; Fujimoto, Masaki; Araya, Akito; Barucci, Maria Antonietta; Genda, Hidenori; Hirata, Naru; Ikeda, Hitoshi; Imamura, Takeshi; Helbert, Jörn; Kameda, Shingo; Kobayashi, Masanori; Kusano, Hiroki; Lawrence, David J.; Matsumoto, Koji; Michel, Patrick; Miyamoto, Hideaki; Morota, Tomokatsu; Nakagawa, Hiromu; Nakamura, Tomoki; Ogawa, Kazunori; Otake, Hisashi; Ozaki, Masanobu; Russell, Sara; Sasaki, Sho; Sawada, Hirotaka; Senshu, Hiroki; Tachibana, Shogo; Terada, Naoki; Ulamec, Stephan; Usui, Tomohiro; Wada, Koji; Watanabe, Sei-ichiro; Yokota, Shoichiro

doi:10.1186/s40623-021-01545-7

Earth, Planets and Space

Table 4 Instruments onboard MMX for scientific observations

From: Martian moons exploration MMX: sample return mission to Phobos elucidating formation processes of habitable planets

Name: function	Major specifications	Roles
Name: function	Major specifications	Moons’ origin	Sampling assist	Mars system
LIDAR:^a laser altimeter	Laser wavelength 1064 nm	Characterization of geologic structures and bedrock exposed areas	Selection and characterization of sampling sites in terms of safety for landing, geologic context, and representativeness as pieces of bedrock	Measurement of surface morphology for the geologic history of the moons
	Ranging distance: 100 m—100 km
	Ranging resolution: < 22 m @ 100 km
	Footprint 50 m from 100 km altitude
TENGOO:^b telescopic camera	FOV: 1.1° × 0.82°	included above	included above	included above and below
	Wavelength: a part of visible light
	Spatial resolution: ~ 40 cm @ 20 km alt
OROCHI:^c wide-angle multiband camera	FOV: 66° × 53°	Determination of global surface composition (Hydrous minerals, Fe/Si, H₂O release rate, etc.)	ditto	Observation of H₂O and dust circulation in the Martian climate system
	Wavelength (width): 390 (50), 480 (30), 550 (30), 650 (10), 700 (10), 800 (40), 950 (60) nm, and 400–900 nm (monochromatic)
	Spatial resolution: 20 m @ 20 km alt., 10 cm for an area of 100 × 100 m² around landing sites, 1 mm for an area of 1 × 1 m² around sampling sites
MIRS:^d near-infrared spectrometer	FOV:3.3° (in the direction of spectrometer slit)	included above	ditto	included above
	Wavelength: 0.9–3.6 μm
	Spectral sampling: 10 nm
	Spatial resolution: < 20 m @ 20 km alt
MSA:^e ion mass spectrometer	Geometric factor: ≥ 10⁴ cm² sr eV/eV	ditto	ditto	Searching for the gas torus and escaping Martian atmosphere
	Ion energy: ~ 5 eV/q- ~ 30 keV/q, Energy resolution: ΔE/E ~ 10%
	Ion mass: 1–100 amu, Mass resolution: M/ΔM > 100
MEGANE:^f gamma-ray and neutron spectrometer	Gamma-ray energy: 0.4–8 MeV with energy resolution: < 5.1 keV (FWHM) @ 1454 keV	ditto	ditto	(not assigned)
MEGANE:^f gamma-ray and neutron spectrometer	Neutron energy: thermal (0.01–0.5 eV), epithermal (0.5–0.5 MeV), fast (0.5–7 MeV)	ditto	ditto	(not assigned)
MMX Rover: solar powered rover	Laser Raman spectrometer	In situ measurement of mineralogy and physical properties of regolith	ditto	ditto
	Thermal radiometer
	Navigation cameras
	Wheel cameras
CMDM:^g dust counter	Dust size: > 10–20 μm	Detecting dust flux and ring to reveal the weathering process on the moons’ surface by micrometeoroid bombardments
CMDM:^g dust counter	Dust velocity: > 0.16 km/s

^aLIght DEtection and Ranging
^bTElescopic Nadir imager for GeOmOrphology (name after long-nosed goblin in Japanese folklore)
^cOptical RaidOmeter composed of CHromatic Imagers (after giant snake with eight heads in Japanese folklore)
^dMMX InfraRed Spectrometer
^eMass Spectrum Analyzer
^fMars moons Exploration with GAmma rays and NEutrons (after eyeglasses in Japanese)
^gCircum Martian Dust Monitor

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