Martian Moons eXploration: The scientific investigations of Mars andits moonsEditorial Board (March 2024)
Editor-in-Chief
Takeshi Sagiya, Nagoya University, Japan

Vice Editors-in-Chief
Masahito Nosé, Nagoya City University, Japan

Aitaro Kato, University of Tokyo, Japan

Editors
Koki Aizawa
Hideo Aochi
Elvira Astafyeva
Pascal Audet
Kiyoshi Baba
Toshitaka Baba
Joseph B.H. Baker
Maxwell C. Brown
Stephan Christoph Buchert
Sonia Calvari
Xiaowei ChenPeter Chi
Kuo-En Ching
Phil Cummins
Hao Dong
Guangyu Fu
Hidenori Genda
Alexander Grayver
Aditya Gusman

Takeshi Hasegawa
Stuart Henrys
Yuji Himematsu
Hauke Hussmann
Mie Ichihara
Hidekatsu Jin
Art Jolly
Nobuki Kame
Katsuya Kaneko
Ikuo Katayama
Yoko Kebukawa
Kunihiro Keika
Kostas Konstantinou
Juanjo Ledo
Koji Matsuo
Masaki Matsushima
Yasunobu Miyoshi
Hiroshi Nagaoka
Norihiro Nakamura

Atsuko Namiki
Yasuhito Narita
Kazunari Nawa
Kiwamu Nishida
Hiroyo Ohya
Duggirala Pallamraju
Severine Rosat
Susumu Saito
David Shelly
Wataru Suzuki
Youichiro Takada
Sunny Tam
Naoki Uchida
Yanbin Wang
Yih-Min Wu
Yusuke Yokota
Yohei Yukutake
Seiji Zenitani

Hiroo Kanamori
Jun'ichiro Kawaguchi
Hitoshi Mizutani
Yasuo Ogawa

Toshitaka Tsuda
Zhongliang Wu
Kiyoshi Yomogida

Advisory Board
Benjamin Fong Chao
Bernard Chouet
Yoshimori Honkura
Toshihiko Iyemori

Journal Scope
Earth, Planets and Space (EPS) is the official journal of Society of Geomagnetism and Earth, Planetary
and Space Sciences, The Seismological Society of Japan, The Volcanological Society of Japan, The
Geodetic Society of Japan, and The Japanese Society for Planetary Sciences.
EPS is a peer-reviewed, open-access journal published under SpringerOpen. It is an international journal
covering scientific articles in the entire field of earth and planetary sciences, particularly geomagnetism,aeronomy, space science, seismology, volcanology, geodesy, and planetary science. EPS also welcomesarticles in new and interdisciplinary subjects, and technical reports on instrumentation and software.
The journal was launched in 1998 and has since published over 4300 articles. All of them are available forfree on SpringerLink:
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Yours sincerely,
Prof. Takeshi Sagiya
Editor-in-Chief, Earth, Planets and Space
eic@earth-planets-space.org

Earth, Planets and Space(2024) 76:8
Genda et al. Earth, Planets and Space
https://doi.org/10.1186/s40623-023-01950-0

Open Access

PREFACESpecial issue “Martian Moons eXploration:
the scientific investigations of Mars and its
moons”
Hidenori Genda1*, Tomohiro Usui2, Nancy L. Chabot3, Ramses Ramirez4 and Keiji Ohtsuki5

RadiOmeter composed of CHromatic Imagers). Senshu
et al. (2021) presented a laser altimeter, LIDAR (LIgiht
Detection And Ranging). Barucci et al. (2021) presented
a near-infrared spectrometer, MIRS (MMX InfraRed
Spectrometer), which is built at LESIA-Paris Observatory. Chabot et al. (2021) presented a NASA-fundedgamma-ray and neutron spectrometer, MEGANE (Marsmoon Exploration with GAmma rays and NEutrons).
Yokota et al. (2021) described an ion mass spectrometer,
MSA (Mass Spectrum Analyzer). Kobayashi et al. (2018)
described a dust counter, CMDM (Circum-Martian Dust
Monitor), and its implication was presented in Krüger
et al. (2021). The MMX spacecraft is also equipped witha rover developed by CNES and DLR (Michel et al. 2022)with a Raman spectrometer, RAX (Cho et al. 2021). Two
independent sampling systems using coring and pneumatic samplers will be employed on the MMX spacecraft(Usui et al. 2020).
Nakamura et al. (2021) summarized the current scientific operation plan for 3 years, including the close-up
observations of Phobos, rover delivery to Phobos, twotouch down events for sample collection, observation ofMars (Ogohara et al. 2022), and the flyby observation of
Deimos. Matsumoto et al. (2021) reviewed recent geodetic observations of Phobos, and showed the strategies
for the geodetic observations during the MMX mission.
High-resolution shape models of Phobos and Deimos
were presented in Ernst et al. (2023). Fujiya et al. (2021)
presented the design of analytical protocols for the
returned Phobos samples to reveal the origin of the Martian moons as well as the evolution of the Mars-moons
system.

Martian Moons eXploration (MMX) marks the thirdsample return mission led by the Japan Aerospace
Exploration Agency (JAXA), succeeding the Hayabusa
and Hayabusa 2 missions. The MMX spacecraft aims toextensively observe two Martian moons (Phobos andDeimos) and Mars over 3 years, and collect samples from
Phobos for return to Earth. The major scientific objectives of the MMX mission are to solve the origin of thetwo moons, to elucidate the early Solar System evolution, and to explore the evolutionary processes of both
moons and Mars surface environment. This first special
issue for the MMX mission is dedicated to the current
status of the MMX mission, such as the science instruments aboard MMX, the mission plan, and the strategies
to achieve the scientific objectives.
Kuramoto et al. (2022) overviewed the current designof the MMX mission, focusing on the scientific objectives
and the mission requirements. To achieve those objectives, the MMX spacecraft is equipped with 7 scientificinstruments, 1 rover, and 2 sampling systems. Kameda et al. (2021) described a telescopic camera, TENGOO (TElescopic Nadir imager for GeOmOrphology),
and wide-angle multiband camera, OROCHI (Optical*Correspondence:
Hidenori Genda
genda@elsi.jp
1
Earth‑Life Science Institute (ELSI), Tokyo Institute of Technology, Tokyo,
Japan
2
Institute of Space and Astronautical Science (ISAS), Japan Aerospace
Exploration Agency (JAXA), Sagamihara, Japan
3
Johns Hopkins University Applied Physics Laboratory, Laure, MD, USA
4
University of Central Florida, Orlando, FL, USA
5
Kobe University, Kobe, Japan© The Author(s) 2024. Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which
permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to theoriginal author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images orother third party material in this article are included in the article’s Creative Commons licence, unless indicated otherwise in a credit line
to the material. If material is not included in the article’s Creative Commons licence and your intended use is not permitted by statutory
regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of thislicence, visit http://creativecommons.org/licenses/by/4.0/.

1

Martian Moons eXploration: The scientific investigations of Mars and its moons
Genda et al. Earth, Planets and Space(2024) 76:8

Page 2 of 2

In addition, Miyamoto et al. (2021) reviewed the surface environment of Phobos and showed the development of simulated soil materials of Phobos. Takemura
et al. (2021) summarized typical geological features of
Phobos and discussed the topographic irregularities andthe engineering safety for the landing sites. Sefton-Nashet al. (2021) discussed the possibility of Phobos for an
exploration platform on Phobos in the future.
While JAXA leads the MMX mission, some instruments, observational planning and execution are shapedby extensive international collaborations, fostering a collective effort in advancing our understanding of Marsand its moons system. The new knowledge brought forth
by the MMX mission is poised to carve out new horizons
in future research and exploration activities. The pursuitof the unknown will continue to drive the journey of science and exploration.

en route to Phobos. Earth Planets Space 73:93. https://doi.org/10.1186/
s40623‑021‑01412‑5
Kuramoto K, Kawakatsu Y, Fujimoto M et al (2022) Martian Moons Exploration
MMX: sample return mission to Phobos elucidating formation processesof habitable planets. Earth Planets Space 74:12. https://doi.org/10.1186/
s40623‑021‑01545‑7
Matsumoto K, Hirata N, Ikeda H et al (2021) MMX geodesy investigations: sci‑ence requirements and observation strategy. Earth Planets Space 73:226.
https://doi.org/10.1186/s40623‑021‑01500‑6Michel P, Ulamec S, Boettger U et al (2022) The MMX rover: performing in‑situ
surface investigations on Phobos. Earth Planets Space 74:2. https://doi.
org/10.1186/s40623‑021‑01464‑7
Miyamoto H, Niihara T, Wada K et al (2021) Surface environment of phobos
and phobos simulant UPTS. Earth Planets Space 73:214. https://doi.org/
10.1186/s40623‑021‑01406‑3
Nakamura T, Ikeda H, Kouyama T et al (2021) Science operation plan of Phobos
and Deimos from the MMX spacecraft. Earth Planets Space 73:227.
https://doi.org/10.1186/s40623‑021‑01546‑6
Ogohara K, Nakagawa H, Aoki S et al (2022) The Mars system revealed by theMartian Moons eXploration mission. Earth Planets Space 74:1. https://doi.
org/10.1186/s40623‑021‑01417‑0
Sefton‑Nash E, Thébault G, Witasse O et al (2021) Visibility analysis of Phobos tosupport a science and exploration platform. Earth Planets Space 73:215.
https://doi.org/10.1186/s40623‑021‑01542‑w
Senshu H, Mizuno T, Umetani K et al (2021) Light Detection and Rang‑ing (LIDAR) laser altimeter for the Martian Moons eXploration (MMX)
spacecraft. Earth Planets Space 73:219. https://doi.org/10.1186/
s40623‑021‑01537‑7
Takemura T, Miyamoto H, Hemmi R et al (2021) Small‑scale topographic irregu‑
larities on Phobos: image and numerical analyses for MMX mission. Earth
Planets Space 73:213. https://doi.org/10.1186/s40623‑021‑01463‑8
Usui T, Bajo KI, Fujiya W et al (2020) The importance of Phobos sample returnfor understanding the Mars‑moon system. Space Sci Rev 216:49. https://doi.org/10.1007/s11214‑020‑00668‑9
Yokota S, Terada N, Matsuoka A et al (2021) In situ observations of ions andmagnetic field around Phobos: the Mass Spectrum Analyzer (MSA) for theMartian Moons eXploration (MMX) mission. Earth Planets Space 73:216.
https://doi.org/10.1186/s40623‑021‑01452‑x

Author contribution
All authors of this article served as guest editors for this special issue. HG
drafted the manuscript. All authors read and approved the final manuscript.
Data availability
Not applicable.

Declarations
Competing interests
The authors declare that they have no competing interests.

Publisher’s NoteSpringer Nature remains neutral with regard to jurisdictional claims in pub‑lished maps and institutional affiliations.
References
Barruci MA, Reess JM, Bernardi P et al (2021) MIRS an imaging spectrometer for
the MMX mission. Earth Planets Space 73:211. https://doi.org/10.1186/
s40623‑021‑01423‑2
Chabot NL, Peplowski PN, Ernst CM et al (2021) MEGANE investigations ofphobos and the small body mapping tool. Earth Planets Space 73:217.
https://doi.org/10.1186/s40623‑021‑01509‑x
Cho Y, Bottger U, Rull F et al (2021) In‑situ science on Phobos with the Raman
spectrometer for MMX (RAX): preliminary design and feasibility of Raman
measurements. Earth Planets Space 73:232. https://doi.org/10.1186/
s40623‑021‑01496‑z
Ernst CM, Daly RT, Gaskell RW et al (2023) High‑resolution shape models of
Phobos and Deimos from stereophotoclinometry. Earth Planets Space75:103. https://doi.org/10.1186/s40623‑023‑01814‑7
Fujiya W, Furukawa Y, Sugahara H et al (2021) Analytical protocols for
Phobos regolith samples returned by the Martian Moons eXploration(MMX) mission. Earth Planet Space 73:120. https://doi.org/10.1186/
s40623‑021‑01438‑9
Kameda S, Ozaki M, Enya K et al (2021) Design of Telescopic Nadir Imager for
Geomorphology (TENGOO) and Observation of surface Reflectance by
Optical Chromatic Imager (OROCHI) for the MMX mission. Earth Planets
Space 73:218. https://doi.org/10.1186/s40623‑021‑01462‑9
Kobayashi M, Krüger H, Senshu H et al (2018) In situ observations of dust parti‑
cles in Martian dust belts using a large‑sensitive‑area dust sensor. Planet
Space Sci 156:41–46. https://doi.org/10.1016/j.pss.2017.12.011
Krüger H, Kobayashi M, Strub P et al (2021) Modelling cometary meteoroid
stream traverses of the Martian Moons eXploration (MMX) spacecraft2

Earth, Planets and SpaceFRONTIER LETTER

Open AccessMartian moons exploration MMX: sample return mission to Phobos
elucidating formation processes of habitable planets
Kiyoshi Kuramoto*, Yasuhiro Kawakatsu, Masaki Fujimoto, Akito Araya, Maria Antonietta Barucci,
Hidenori Genda, Naru Hirata, Hitoshi Ikeda, Takeshi Imamura, Jörn Helbert, Shingo Kameda,
Masanori Kobayashi, Hiroki Kusano, David J. Lawrence, Koji Matsumoto, Patrick Michel, Hideaki Miyamoto,
Tomokatsu Morota, Hiromu Nakagawa, Tomoki Nakamura, Kazunori Ogawa, Hisashi Otake, Masanobu Ozaki,
Sara Russell, Sho Sasaki, Hirotaka Sawada, Hiroki Senshu, Shogo Tachibana, Naoki Terada, Stephan Ulamec,
Tomohiro Usui, Koji Wada, Sei-ichiro Watanabe and Shoichiro Yokota
Earth, Planets and Space 2022, 74:12 DOI: 10.1186/s40623-021-01545-7
Received: 26 January 2021, Accepted: 11 November 2021, Published: 20 January 2022

Abstract
Martian moons exploration, MMX, is the new sample return mission planned by the Japan Aerospace Exploration Agency (JAXA)
targeting the two Martian moons with the scheduled launch in 2024 and return to the Earth in 2029. The major scientific objectives ofthis mission are to determine the origin of Phobos and Deimos, to elucidate
the early Solar System evolution in terms of volatile delivery across the snowline to the terrestrial planets having habitable surface environments, and to
explore the evolutionary processes of both moons and Mars surface
environment. To achieve these objectives, during a stay in circum-Martian
space over about 3 years MMX will collect samples from Phobos along withclose-up observations of this inner moon and carry out multiple flybys of
Deimos to make comparative observations of this outer moon.
Simultaneously, successive observations of the Martian atmosphere will also
be made by utilizing the advantage of quasi-equatorial spacecraft orbits
along the moons’ orbits.

Keywords: Phobos, Deimos, Mars, Sample return mission, Early Solar
System, Habitable planet

Fig. 2*Corresponding author: Kiyoshi Kuramoto, keikei@ep.sci.hokudai.ac.jp

FULL PAPER

Open Access

Modelling cometary meteoroid stream traverses of the MartianMoons eXploration (MMX) spacecraft en route to Phobos
Harald Krüger*, Masanori Kobayashi, Peter Strub, Georg-Moragas Klostermeyer,
Maximilian Sommer, Hiroshi Kimura, Eberhard Grün and Ralf Srama
Earth, Planets and Space 2021, 73:93 DOI: 10.1186/s40623-021-01412-5
Received: 27 November 2020, Accepted: 29 March 2021, Published: 16 April 2021

Abstract
The Martian Moons Exploration (MMX) spacecraft is a JAXA mission to Mars and its moons Phobos and Deimos. MMX will be equipped with
the Circum-Martian Dust Monitor (CMDM) which is a newly developed light-weight (650 g) large area (1 m2) dust impact detector. Cometarymeteoroid streams (also referred to as trails) exist along the orbits of comets, forming fine structures of the interplanetary dust cloud. The
streams consist predominantly of the largest cometary particles (with sizes of approximately 100 mm to 1 cm) which are ejected at low speeds
and remain very close to the comet orbit for several revolutions around the Sun. The Interplanetary Meteoroid Environment for eXploration(IMEX) dust streams in space model is a new and recently published universal model for cometary meteoroid streams in the inner Solar
System. We use IMEX to study the detection conditions of cometary dust stream particles with CMDM during the MMX mission in the time
period 2024 to 2028. The model predicts traverses of 12 cometary meteoroid streams with fluxes of 100 mm and bigger particles of at least
10−3m−2day−1 during a total time period of approximately 90 days. The highest flux of 0.15 m−2day−1 is predicted for comet 114P/Wiseman-Skiff
in October 2026. With its large detection area and high sensitivity
CMDM will be able to detect cometary meteoroid streams en route to
Phobos. Our simulation results for the Mars orbital phase of MMX also
predict the occurrence of meteor showers in the Martian atmospherewhich may be observable from the Martian surface with cameras on
board landers or rovers. Finally, the IMEX model can be used to study
the impact hazards imposed by meteoroid impacts onto large-area
spacecraft structures that will be particularly necessary for crewed
deep space missions.

Keywords: Comets, Meteoroid trails, Meteoroid streams,

Interplanetary dust, Martian moons, Phobos, Deimos,
Martian Moons Exploration, MMX

Graphical abstract*Corresponding author: Harald Krüger, krueger@mps.mpg.de3

Martian Moons eXploration: The scientific investigations of Mars and its moons

FULL PAPER

Open AccessAnalytical protocols for Phobos regolith samples returned by theMartian Moons eXploration (MMX) mission
Wataru Fujiya*, Yoshihiro Furukawa, Haruna Sugahara, Mizuho Koike, Ken-ichi Bajo,
Nancy L. Chabot, Yayoi N. Miura, Frederic Moynier, Sara S. Russell, Shogo Tachibana,
Yoshinori Takano, Tomohiro Usui and Michael E. Zolensky
Earth, Planets and Space 2021, 73:120 DOI: 10.1186/s40623-021-01438-9
Received: 3 December 2020, Accepted: 10 May 2021, Published: 1 June 2021

Abstract
Japan Aerospace Exploration Agency (JAXA) will launch a spacecraft in 2024 for a sample return mission from Phobos (Martian Moons
eXploration: MMX). Touchdown operations are planned to be performed twice at different landing sites on the Phobos surface to collect> 10 g of the Phobos surface materials with coring and pneumatic sampling systems on board. The Sample Analysis Working Team (SAWT) of
MMX is now designing analytical protocols of the returned Phobos samples to shed light on the origin of the Martian moons as well as theevolution of the Mars–moon system. Observations of petrology and mineralogy, and measurements of bulk chemical compositions andstable isotopic ratios of, e.g., O, Cr, Ti, and Zn can provide crucial information about the origin of Phobos. If Phobos is a captured asteroid
composed of primitive chondritic materials, as inferred from its reflectance spectra, geochemical data including the nature of organic matteras well as bulk H and N isotopic compositions characterize the volatile materials in the samples and constrain the type of the captured
asteroid. Cosmogenic and solar wind components, most pronounced in noble gas isotopic compositions, can reveal surface processes on
Phobos. Long- and short-lived radionuclide chronometry such as 53Mn–53Cr and 87Rb–87Sr systematics can date pivotal events like impacts,
thermal metamorphism, and aqueous alteration on Phobos. It should
be noted that the Phobos regolith is expected to contain a small
amount of materials delivered from Mars, which may be physicallyand chemically different from any Martian meteorites in our collection
and thus are particularly precious. The analysis plan will be designed
to detect such Martian materials, if any, from the returned samples
dominated by the endogenous Phobos materials in curation
procedures at JAXA before they are processed for further analyses.

Keywords: MMX, Sample analyses, Mineralogy, Petrology, Chemicalcomposition, Isotopic composition, Organic matter

Graphical abstract*Corresponding author: Wataru Fujiya, wataru.fujiya.sci@vc.ibaraki.ac.jp

FULL PAPER

Open Access

MIRS: an imaging spectrometer for the MMX mission
Maria Antonietta Barucci*, Jean-Michel Reess, Pernelle Bernardi, Alain Doressoundiram, Sonia Fornasier, Michel Le Du,
Takahiro Iwata, Hiromu Nakagawa, Tomoki Nakamura, Yves André, Shohei Aoki, Takehiko Arai, Elisa Baldit, Pierre Beck,
Jean-Tristan Buey, Elisabet Canalias, Matthieu Castelnau, Sebastien Charnoz, Marc Chaussidon, Fréderic Chapron,
Valerie Ciarletti, Marco Delbo, Bruno Dubois, Stephane Gauffre, Thomas Gautier, Hidenori Genda, Rafik Hassen-Khodja,
Gilles Hervet, Ryuki Hyodo, Christian Imbert, Takeshi Imamura, Laurent Jorda, Shingo Kameda, Driss Kouach,
Toru Kouyama, Takeshi Kuroda, Hiroyuki Kurokawa, Laurent Lapaw, Jeremie Lasue, Laetitia Le Deit,
Aurélien Ledot, Cedric Leyrat, Bertrand Le Ruyet, Moe Matsuoka, Frederic Merlin, Hideaki Miyamoto,Frederic Moynier, Napoleon Nguyen Tuong, Kazunori Ogohara, Takahito Osawa, Jérôme Parisot,
Laurie Pistre, Benjamin Quertier, Sean N. Raymond, Francis Rocard, Takeshi Sakanoi, Takao M. Sato,
Eric Sawyer, Fériel Tache, Sylvain Trémolières, Fuminori Tsuchiya, Pierre Vernazza and Didier Zeganadin
Earth, Planets and Space 2021, 73:211 DOI: 10.1186/s40623-021-01423-2
Received: 5 December 2020, Accepted: 23 April 2021, Published: 6 December 2021

Abstract
The 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 otherFrench 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 andDeimos containing compositional diagnostic spectral features thatwill be used to analyze the surface composition and to support the
sampling site selection. MIRS will also study Mars atmosphere, inparticular spatial and temporal changes such as clouds, dust andwater vapor.

Keywords: MIRS, MMX, Imaging spectrometer, Phobos, Deimos,
Mars

Graphical abstract*Corresponding author: Maria Antonietta Barucci, antonella.barucci@obspm.fr
4

Earth, Planets and Space

FULL PAPER

Open Access

Small-scale topographic irregularities on Phobos: image
and numerical analyses for MMX mission
Tomohiro Takemura, Hideaki Miyamoto*, Ryodo Hemmi, Takafumi Niihara and Patrick Michel
Earth, Planets and Space 2021, 73:213 DOI: 10.1186/s40623-021-01463-8
Received: 24 January 2021, Accepted: 14 June 2021, Published: 10 December 2021

Abstract
The mothership of the Martian Moons eXploration (MMX) will perform the first landing and sampling on the surface of
Phobos. For the safe landing, the 2.1-m-wide mothership of the MMX should find a smooth surface with at most 40 cm
topographic irregularity, however, whose abundance or even existence is not guaranteed based on current knowledge. We
studied the highest resolution (a few meters per pixel) images of Phobos for possible topographic irregularities in terms ofboulder (positive relief feature) and crater distributions. We find that the spatial number densities of positive relief featuresand craters can vary significantly, indicating that the surface irregularities vary significantly over the entire surface. We
extrapolate the size-frequency distributions of positive relief features to evaluate the surface roughness below the image
resolution limit. We find that the probabilities that topographic irregularities are < 40 cm for the areas of 4 × 4 m and 20 × 20 m
are > 33% and < 1% for boulder-rich areas and > 88% and > 13% for boulder-poor areas, respectively, even for the worst-caseestimates. The estimated probabilities largely increase when we reduce the assumed number of positive relief features, which
are more realistic cases. These indicate high probabilities
of finding a smooth enough place to land on Phobos’
surface safely.

Keywords: MMX, Phobos, Deimos, Landing,
Topography, Roughness

Graphical abstract*Corresponding author: Hideaki Miyamoto, hm@sys.t.u-tokyo.ac.jp

FULL PAPER

Open Access

Surface environment of Phobos and Phobos simulant UTPS
Hideaki Miyamoto*, Takafumi Niihara, Koji Wada, Kazunori Ogawa, Hiroki Senshu, Patrick Michel, Hiroshi Kikuchi,
Ryodo Hemmi, Tomoki Nakamura, Akiko M. Nakamura, Naoyuki Hirata, Sho Sasaki, Erik Asphaug, Daniel T. Britt,Paul A. Abell, Ronald-Louis Ballouz, Olivier S. Banouin, Nicola Baresi, Maria A. Barucci, Jens Biele, Matthias Grott,Hideitsu Hino, Peng K. Hong, Takane Imada, Shingo Kameda, Makito Kobayashi, Guy Libourel,
Katsuro Mogi, Naomi Murdoch, Yuki Nishio, Shogo Okamoto, Yuichiro Ota, Masatsugu Otsuki,
Katharina A. Otto, Naoya Sakatani, Yuta Shimizu, Tomohiro Takemura, Naoki Terada,
Masafumi Tsukamoto, Tomohiro Usui and Konrad Willner
Earth, Planets and Space 2021, 73:214 DOI: 10.1186/s40623-021-01406-3
Received: 15 January 2021, Accepted: 24 March 2021, Published: 10 December 2021

Abstract
The Martian Moons eXploration (MMX) mission will study the Martian moons Phobos and Deimos, Mars, and theirenvironments. The mission scenario includes both landing on the surface of Phobos to collect samples and deploying a smallrover for in situ observations. Engineering safeties and scientific planning for these operations require appropriate evaluationsof the surface environment of Phobos. Thus, the mission team organized the Landing Operation Working Team (LOWT) and
Surface Science and Geology Sub-Science Team (SSG-SST), whose view of the Phobos environment is summarized in thispaper. While orbital and large-scale characteristics of Phobos are
relatively well known, characteristics of the surface regolith, including
the particle size-distributions, the packing density, and the mechanicalproperties, are difficult to constrain. Therefore, we developed several
types of simulated soil materials (simulant), such as UTPS-TB(University of Tokyo Phobos Simulant, Tagish Lake based), UTPS-IB(Impact-hypothesis based), and UTPS-S (Simpler version) for
engineering and scientific evaluation experiments.

Keywords: MMX, Phobos, Deimos, Surface environment, Simulant
Graphical abstract*Corresponding author: Hideaki Miyamoto, hm@sys.t.u-tokyo.ac.jp
5Martian Moons eXploration: The scientific investigations of Mars and its moons

FULL PAPER

Open Access

Visibility analysis of Phobos to support a science andexploration platform
Elliot Sefton-Nash*, Guillaume Thébault, Olivier Witasse, Detlef Koschny, Beatriz Sánchez-Canoand Alejandro Cardesín-Moinelo
Earth, Planets and Space 2021, 73:215 DOI: 10.1186/s40623-021-01542-w
Received: 30 November 2020, Accepted: 6 November 2021, Published: 10 December 2021

Abstract
The surfaces of the Martian moons, Phobos and Deimos may offer a stable environment for long-term operation of platforms. We present a broad
assessment of potential scientific investigations, as well as strategic and operational opportunities offered by long-term operation of an instrumented
lander. Studies using observations of Mars’ moons, and the detailed new findings expected from the JAXA Martian Moons eXploration (MMX) mission,
International Mars Sample Return (MSR) Campaign and other upcoming Mars missions, provide a driver for feasibility and trade studies for follow-on
missions that would build on the knowledge gain from those missions. We discuss the scientific questions and operational objectives that may bepertinent for landed platforms on the martian moons, including (1) monitoring and scientific investigations of Mars’ surface and atmosphere, (2)scientific investigations of the martian moons, (3) monitoring and scientific investigations of the space environment, (4) data relay for Mars surface
assets or interplanetary missions and 5) use in a Mars navigation/positioning system. We present results from visibility calculations performed using the
SPICE observation geometry system for space science missions, and a Phobos shape model. We compute as a function of location on Phobos, visibility
quantities that are most relevant to science and operational objectives. These include visibility from Phobos of the Sun, Earth, Mars surface andatmosphere, Deimos, and Jupiter. We also consider occultation events by the Mars atmosphere of Earth and Deimos that may provide opportunities forradio science. Calculations are performed for a study period spanning one Mars year in a hypothetical future operational scenario (1 Jan 2030–18 Nov
2031). We combine visibility metrics to identify locations on Phobos most suitable for long-term
operation of a platform. We find the Mars-facing side of Phobos, and limited areas on the leading andtrailing sides, satisfy the most requirements defined for Mars and Phobos science, space environment
monitoring, and data relay/navigation. We demonstrate that compliance with requirements related tovisibility of Mars and its atmosphere are not mutually exclusive with those that are better satisfied on
Phobos’ anti-Mars side, such as those aided by maximizing their cumulative view factor to the ecliptic
plane (i.e. visibility to the Sun, Earth or outer solar system). Finally, our methodology allows to assess theextent to which combined visibility metrics can meet mission requirements. The process we describe canbe used to support landing site identification and selection on planets, moons and small bodies.

Keywords: Phobos, Deimos, Mars, Platform, Visibility

Graphical abstract*Corresponding author: Elliot Sefton-Nash, e.sefton-nash@uclmail.net

FULL PAPER

Open AccessIn situ observations of ions and magnetic field around Phobos:
the mass spectrum analyzer (MSA) for the Martian Moons
eXploration (MMX) mission
Shoichiro Yokota*, Naoki Terada, Ayako Matsuoka, Naofumi Murata, Yoshifumi Saito,
Dominique Delcourt, Yoshifumi Futaana, Kanako Seki, Micah J. Schaible, Kazushi Asamura,
Satoshi Kasahara, Hiromu Nakagawa, Masaki N. Nishino, Reiko Nomura, Kunihiro Keika,
Yuki Harada and Shun Imajo
Earth, Planets and Space 2021, 73:216 DOI: 10.1186/s40623-021-01452-x
Received: 10 December 2020, Accepted: 5 June 2021, Published: 13 December 2021

Abstract
The mass spectrum analyzer (MSA) will perform in situ observations of ions and magnetic fields around Phobos as part of theMartian Moons eXploration (MMX) mission to investigate the origin of the Martian moons and physical processes in theMartian environment. MSA consists of an ion energy mass spectrometer and two magnetometers which will measure velocity
distribution functions and mass/charge distributions of low-energy ions and magnetic field vectors, respectively. For the MMX
scientific objectives, MSA will observe solar wind ions, those scattered at the Phobos surface, water-related ions generated in
the predicted Martian gas torus, secondary ionssputtered from Phobos, and escaping ions from theMartian atmosphere, while monitoring thesurrounding magnetic field. MSA will be developed
from previous instruments for space plasma
missions such as Kaguya, Arase, and BepiColombo/
Mio to contribute to the MMX scientific objectives.

Keywords: Martian Moons eXploration (MMX),

Phobos, Mars, Mass spectrum analyzer,
Magnetometer

Graphical abstract*Corresponding author: Shoichiro Yokota, yokota@ess.sci.osaka-u.ac.jp
6Earth, Planets and Space

FULL PAPER

Open Access

MEGANE investigations of Phobos and the Small Body
Mapping Tool
Nancy L. Chabot*, Patrick N. Peplowski, Carolyn M. Ernst, Hari Nair, Michael Lucks, R. Josh Steele
and David J. Lawrence
Earth, Planets and Space 2021, 73:217 DOI: 10.1186/s40623-021-01509-x
Received: 15 January 2021, Accepted: 25 August 2021, Published: 13 December 2021

Abstract
The MEGANE instrument onboard the MMX mission will acquire gamma-ray and neutron spectroscopy data of Phobos todetermine the elemental composition of the martian moon and provide key constraints on its origin. To produce accuratecompositional results, the irregular shape of Phobos and its proximity to Mars must be taken into account during the analysis
of MEGANE data. The MEGANE team is adapting the Small Body Mapping Tool (SBMT) to handle gamma-ray and neutron
spectroscopy investigations, building on the demonstrated record of success of the SBMT being applied to scientificinvestigations on other spacecraft missions of irregularly shaped bodies. This is the first application of the SBMT to a gammaray and neutron spectroscopy dataset, and the native, three-dimensional foundation of the SBMT is well suited to MEGANE’sneeds. In addition, the SBMT will enable comparisons between the MEGANE datasets and other datasets of the martianmoons, including data from previous spacecraft missions and MMX’s multi-instrument suite.

Keywords: Phobos, MMX, MEGANE, Gamma-ray

spectroscopy, Neutron spectroscopy,
Martian moons

Graphical abstract*Corresponding author: Nancy L. Chabot, Nancy.Chabot@jhuapl.edu

FULL PAPER

Open Access

Design of telescopic nadir imager for geomorphology (TENGOO) andobservation of surface reflectance by optical chromatic imager(OROCHI) for the Martian Moons Exploration (MMX)
Shingo Kameda*, Masanobu Ozaki, Keigo Enya, Ryota Fuse, Toru Kouyama, Naoya Sakatani, Hidehiko Suzuki, Naoya Osada,
Hiroki Kato, Hideaki Miyamoto, Atsushi Yamazaki, Tomoki Nakamura, Takaya Okamoto, Takahiro Ishimaru,
Peng Hong, Ko Ishibashi, Takeshi Takashima, Ryoya Ishigami, Cheng-Ling Kuo, Shinsuke Abe, Yuya Goda,
Hajime Murao, Saori Fujishima, Tsubasa Aoyama, Keiji Hagiwara, Satoko Mizumoto, Noriko Tanaka,
Kousuke Murakami, Miho Matsumoto, Kenji Tanaka and Hironobu Sakuta
Earth, Planets and Space 2021, 73:218 DOI: 10.1186/s40623-021-01462-9
Received: 20 January 2021, Accepted: 12 June 2021, Published: 14 December 2021

Abstract
The JAXA’s Martian Moons Exploration (MMX) mission is planned to reveal the origin of Phobos and Deimos. It will remotely observeboth moons and return a sample from Phobos. The nominal instruments include the TElescopic Nadir imager for GeOmOrphology(TENGOO) and Optical RadiOmeter composed of CHromatic Imagers (OROCHI). The scientific objective of TENGOO is to obtain thegeomorphological features of Phobos and Deimos. The spatial resolution of TENGOO is 0.3 m at an altitude of 25 km in the quasi-satellite
orbit. The scientific objective of OROCHI is toobtain material distribution using spectral
mapping. OROCHI possesses seven wide-angle
bandpass imagers without a filter wheel and one
monochromatic imager dedicated to theobservation during the landing phase. Using
these two instruments, we plan to select landingsites and obtain information that supports theanalysis of return samples.

Keywords: MMX, TENGOO, OROCHI, Imager,
Phobos, Deimos, Mars

Graphical abstract*Corresponding author: Shingo Kameda, kameda@rikkyo.ac.jp
7Martian Moons eXploration: The scientific investigations of Mars and its moons

FULL PAPER

Open Access

MMX geodesy investigations: science requirements andobservation strategy
Koji Matsumoto*, Naru Hirata, Hitoshi Ikeda, Toru Kouyama, Hiroki Senshu, Keiko Yamamoto,
Hirotomo Noda, Hideaki Miyamoto, Akito Araya, Hiroshi Araki, Shunichi Kamata, Nicola Baresi
and Noriyuki Namiki
Earth, Planets and Space 2021, 73:226 DOI: 10.1186/s40623-021-01500-6
Received: 11 January 2021, Accepted: 16 August 2021, Published: 15 December 2021

Abstract
In order to investigate the origin of Phobos and Deimos, the Japanese Martian Moons eXploration (MMX) mission is scheduled
for launch in 2024. MMX will make comprehensive remote-sensing measurements of both moons and return regolith samples
from Phobos to Earth. Geodetic measurements of gravity, shape, and rotation parameter of a body provides constraints on its
internal structure reflecting its origin and evolution. Moments of inertia are important parameters to constrain the internalmass distribution, but they have not been well determined for the Martian moons yet. We discuss the mission requirements
related to the moments of inertia to detect a potential heterogeneity of the mass distribution inside Phobos. We introduce
mission instruments and operational strategies to meet the mission requirements. We present a preliminary imaging strategy
from a quasi-satellite orbit for a base shape model that is
expected to be created at the early stage of the mission.
Geodetic products including ephemeris, gravity field,
rotation parameter of Phobos, and spacecraft orbit are ofimportance not only for the geodetic study, but also forinterpreting data from various mission instruments andselecting possible landing sites.

Keywords: MMX, Gravity, Shape, Rotation, Internal
structure

Graphical abstract*Corresponding author: Koji Matsumoto, koji.matsumoto@nao.ac.jp

FULL PAPER

Open Access

Science operation plan of Phobos and Deimos from the MMX
spacecraft
Tomoki Nakamura*, Hitoshi Ikeda, Toru Kouyama, Hiromu Nakagawa, Hiroki Kusano, Hiroki Senshu, Shingo Kameda,
Koji Matsumoto, Ferran Gonzalez-Franquesa, Naoya Ozaki, Yosuke Takeo, Nicola Baresi, Yusuke Oki, David J. Lawrence,
Nancy L. Chabot, Patrick N. Peplowski, Maria Antonietta Barucci, Eric Sawyer, Shoichiro Yokota, Naoki Terada,
Stephan Ulamec, Patrick Michel, Masanori Kobayashi, Sho Sasaki, Naru Hirata, Koji Wada, Hideaki Miyamoto,Takeshi Imamura, Naoko Ogawa, Kazunori Ogawa, Takahiro Iwata, Takane Imada, Hisashi Otake,Elisabet Canalias, Laurence Lorda, Simon Tardivel, Stéphane Mary, Makoto Kunugi, Seiji Mitsuhashi,
Alain Doressoundiram, Frédéric Merlin, Sonia Fornasier, Jean-Michel Reess, Pernelle Bernardi,
Shigeru Imai, Yasuyuki Ito, Hatsumi Ishida, Kiyoshi Kuramoto and Yasuhiro Kawakatsu
Earth, Planets and Space 2021, 73:227 DOI: 10.1186/s40623-021-01546-6
Received: 15 April 2021, Accepted: 12 November 2021, Published: 15 December 2021

Abstract
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 stayaround 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 forlanding 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 ofDeimos over as large an area as possible.

Keywords: MMX mission, Phobos, Deimos, QSO, Flyby

Graphical abstract*Corresponding author: Tomoki Nakamura, tomoki.nakamura.a8@tohoku.ac.jp
8Earth, Planets and Space

FULL PAPER

Open AccessIn situ science on Phobos with the Raman spectrometer for MMX(RAX): preliminary design and feasibility of Raman measurements
Yuichiro Cho*, Ute Böttger, Fernando Rull, Heinz-Wilhelm Hübers, Tomàs Belenguer, Anko Börner, Maximilian Buder,
Yuri Bunduki, Enrico Dietz, Till Hagelschuer, Shingo Kameda, Emanuel Kopp, Matthias Lieder, Guillermo Lopez-Reyes,
Andoni Gaizka Moral Inza, Shoki Mori, Jo Akino Ogura, Carsten Paproth, Carlos Perez Canora, Martin Pertenais,
Gisbert Peter, Olga Prieto-Ballesteros, Steve Rockstein, Selene Rodd-Routley, Pablo Rodriguez Perez,
Conor Ryan, Pilar Santamaria, Thomas Säuberlich, Friedrich Schrandt, Susanne Schröder,Claudia Stangarone, Stephan Ulamec, Tomohiro Usui, Iris Weber, Karsten Westerdorff and Koki Yumoto
Earth, Planets and Space 2021, 73:232 DOI: 10.1186/s40623-021-01496-z
Received: 15 January 2021, Accepted: 11 August 2021, Published: 19 December 2021

Abstract
Mineralogy is the key to understanding the origin of Phobos and its position in the evolution of the Solar System. In situ Raman spectroscopy on
Phobos is an important tool to achieve the scientific objectives of the Martian Moons eXploration (MMX) mission, and maximize the scientificmerit of the sample return by characterizing the mineral composition and heterogeneity of the surface of Phobos. Conducting in situ Raman
spectroscopy in the harsh environment of Phobos requires a very sensitive, compact, lightweight, and robust instrument that can be carried by
the compact MMX rover. In this context, the Raman spectrometer for MMX (i.e., RAX) is currently under development via international
collaboration between teams from Japan, Germany, and Spain. To demonstrate the capability of a compact Raman system such as RAX, we built
an instrument that reproduces the optical performance of the flight model using
commercial off-the-shelf parts. Using this performance model, we measured mineral
samples relevant to Phobos and Mars, such as anhydrous silicates, carbonates, and hydrous
minerals. Our measurements indicate that such minerals can be accurately identified usinga RAX-like Raman spectrometer. We demonstrated a spectral resolution of approximately
10 cm−1, high enough to resolve the strongest olivine Raman bands at ~ 820 and ~ 850
cm−1, with highly sensitive Raman peak measurements (e.g., signal-to-noise ratios up to100). These results strongly suggest that the RAX instrument will be capable of determining
the minerals expected on the surface of Phobos, adding valuable information to address
the question of the moon’s origin, heterogeneity, and circum-Mars material transport.

Keywords: Raman spectroscopy, Raman spectrometer for MMX (RAX), Phobos,

Mineralogy, In situ analysis, Sample return, Martian Moons eXploration (MMX)

Graphical abstract*Corresponding author: Yuichiro Cho, cho@eps.s.u-tokyo.ac.jp

FULL PAPER

Open Access

The Mars system revealed by the Martian Moons eXploration mission
Kazunori Ogohara*, Hiromu Nakagawa, Shohei Aoki, Toru Kouyama, Tomohiro Usui, Naoki Terada,
Takeshi Imamura, Franck Montmessin, David Brain, Alain Doressoundiram, Thomas Gautier, Takuya Hara,
Yuki Harada, Hitoshi Ikeda, Mizuho Koike, François Leblanc, Ramses Ramirez, Eric Sawyer, Kanako Seki,
Aymeric Spiga, Ann Carine Vandaele, Shoichiro Yokota, Antonella Barucci and Shingo Kameda
Earth, Planets and Space 2022, 74:1 DOI: 10.1186/s40623-021-01417-0
Received: 27 November 2020, Accepted: 9 April 2021, Published: 3 January 2022

Abstract
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 strategiesof 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 thereturned 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 theinfrared spectrometer onboard the spacecraft can monitor rapid transport processes ofwater vapor, dust, ice clouds, and other species, which could not be traced by theprevious satellites on the sun-synchronous polar orbit. Such time-resolved pictures of
the atmospheric phenomena should be an important clue to understand both theprocesses of water exchange between the surface/underground reservoirs and theatmosphere and the drivers of efficient material transport to the upper atmosphere. The
mass spectrometer with unprecedented mass resolution can observe ions escaping tospace 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 cantransport tracers (e.g., H2O) upward and enhance the atmospheric escape.

Keywords: Mars, Mars system, Paleoclimate, Atmospheric escape, Water cycle, Dust
cycle, Transport process

Graphical abstract*Corresponding author: Kazunori Ogohara, ogohara@cc.kyoto-su.ac.jp9Martian Moons eXploration: The scientific investigations of Mars and its moons

FULL PAPER

Open Access

The MMX rover: performing in situ surface investigations on Phobos
Patrick Michel*, Stephan Ulamec, Ute Böttger, Matthias Grott, Naomi Murdoch, Pierre Vernazza,
Cecily Sunday, Yun Zhang, Rudy Valette, Romain Castellani, Jens Biele, Simon Tardivel,
Olivier Groussin, Laurent Jorda, Jörg Knollenberg, Jan Thimo Grundmann, Denis Arrat,
Gabriel Pont, Stephane Mary, Markus Grebenstein, Hirdy Miyamoto, Tomoki Nakamura,
Koji Wada, Kent Yoshikawa and Kiyoshi Kuramoto
Earth, Planets and Space 2022, 74:2 DOI: 10.1186/s40623-021-01464-7
Received: 1 January 2021, Accepted: 18 June 2021, Published: 3 January 2022

Abstract
The Japanese MMX sample return mission to Phobos by JAXA will carry a rover developed by CNES and DLR that will be
deployed on Phobos to perform in situ analysis of the Martian moon’s surface properties. Past images of the surface of Phobos
show that it is covered by a layer of regolith. However, the mechanical and compositional properties of this regolith are poorly
constrained. In particular, from current remote images, very little is known regarding the particle sizes, their chemicalcomposition, the packing density of the regolith as well as other parameters such as friction and cohesion that influence
surface dynamics. Understanding the properties and dynamics of the regolith in the low-gravity environment of Phobos isimportant to trace back its history and surface evolution. Moreover, this information is also important to support theinterpretation of data obtained by instruments onboard the main MMX
spacecraft, and to minimize the risks involved in the spacecraft sampling
operations. The instruments onboard the Rover are a Raman spectrometer (RAX),
an infrared radiometer (miniRad), two forward-looking cameras for navigationand science purposes (NavCams), and two cameras observing the interactions ofregolith and the rover wheels (WheelCams). The Rover will be deployed before
the MMX spacecraft samples Phobos’ surface and will be the first rover to driveon the surface of a Martian moon and in a very low gravity environment.

Keywords: Camera, Numerical modelling, Phobos, Radiometer, Raman

spectrometer, Regolith, Regolith dynamics, Thermal inertia, RoverGraphical abstract*Corresponding author: Patrick Michel, michelp@oca.eu

FULL PAPER

Open Access

High-resolution shape models of Phobos and Deimos fromstereophotoclinometry
Carolyn M. Ernst*, R. Terik Daly, Robert W. Gaskell, Olivier S. Barnouin, Hari Nair, Benjamin A. Hyatt,
Manar M. Al Asad and Kielan K. W. HochEarth, Planets and Space 2023, 75:103 DOI: 10.1186/s40623-023-01814-7
Received: 28 January 2021, Accepted: 6 April 2023, Published: 25 June 2023

Abstract
We created high-resolution shape models of Phobos and Deimos using stereophotoclinometry and united images from Viking
Orbiter, Phobos 2, Mars Global Surveyor, Mars Express, and Mars Reconnaissance Orbiter into a single coregistered collection.
The best-fit ellipsoid to the Phobos model has radii of (12.95 ± 0.04) km × (11.30 ± 0.04) km × (9.16 ± 0.03) km, with an averageradius of (11.08 ± 0.04) km. The best-fit ellipsoid to the Deimos model has radii of (8.04 ± 0.08) km × (5.89 ± 0.06)
km × (5.11 ± 0.05) km with an average radius of (6.27 ± 0.07) km. The new shape models offer substantial improvements inresolution over existing shape models, while remaining globally consistent with them. The Phobos model resolves grooves,craters, and other surface features ~ 100 m in size across the entire surface. The Deimos model is the first to resolve geologicalsurface features. These models, associated data products, and a searchable, coregistered collection of images across six
spacecraft are publicly available in the Small Body Mapping Tool, and will be archived with the NASA Planetary Data System.
These products enable an array of future studies to advancethe understanding of Phobos and Deimos, facilitate
coregistration of other past and future datasets, and set thestage for planning and operating future missions to themoons, including the upcoming Martian Moons eXploration(MMX) mission.

Keywords: Phobos, Deimos, Martian moons, Small bodies,
Shape, Topography, Stereophotoclinometry,
Martian Moons eXploration

Graphical abstract*Corresponding author: Carolyn M. Ernst, carolyn.ernst@jhuapl.edu
10Earth, Planets and SpaceTECHNICAL REPORT

Open Access

Light detection and ranging (LIDAR) laser altimeter for the MartianMoons Exploration (MMX) spacecraft
Hiroki Senshu*, Takahide Mizuno, Kazuhiro Umetani, Toru Nakura, Akihiro Konishi, Akihiko Ogawa,Hirokazu Ikeda, Koji Matsumoto, Hirotomo Noda, Yoshiaki Ishihara, Sho Sasaki, Naoki Tateno,
Yasuyuki Ikuse, Katsunori Mayuzumi, Teiji Kase and Hisayoshi Kashine
Earth, Planets and Space 2021, 73:219 DOI: 10.1186/s40623-021-01537-7
Received: 15 January 2021, Accepted: 24 October 2021, Published: 14 December 2021

Abstract
An altimeter is a critical instrument in planetary missions, for both safe operations and science activities. We present required
specifications and link budget calculations for light detection and ranging (LIDAR) onboard the Martian Moons Exploration(MMX) spacecraft. During the mission phase, this LIDAR will continuously measure the distance between the spacecraft and its
target. The time-series distance provides important diagnostic information for safe spacecraft operations and important
information for geomorphological studies. Because MMX is a sample return mission, its LIDAR must accommodate physicaldisturbances on the Martian satellite surface. This resulted inchanges to the optical system design.

Keywords: LIDAR, MMX, Phobos

Graphical abstract*Corresponding author: Hiroki Senshu, senshu@perc.it-chiba.ac.jp

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Continued from back cover

Science operation plan of Phobos and Deimos from the MMX spacecraft. . . . . . . . . . . . . . . .  Tomoki Nakamura, Hitoshi Ikeda, Toru Kouyama, Hiromu Nakagawa, Hiroki Kusano, Hiroki Senshu, Shingo Kameda,

Koji Matsumoto, Ferran Gonzalez-Franquesa, Naoya Ozaki, Yosuke Takeo, Nicola Baresi, Yusuke Oki, David J. Lawrence,
Nancy L. Chabot, Patrick N. Peplowski, Maria Antonietta Barucci, Eric Sawyer, Shoichiro Yokota, Naoki Terada,
Stephan Ulamec, Patrick Michel, Masanori Kobayashi, Sho Sasaki, Naru Hirata, Koji Wada, Hideaki Miyamoto,Takeshi Imamura, Naoko Ogawa, Kazunori Ogawa, Takahiro Iwata, Takane Imada, Hisashi Otake,Elisabet Canalias, Laurence Lorda, Simon Tardivel, Stéphane Mary, Makoto Kunugi, Seiji Mitsuhashi,
Alain Doressoundiram, Frédéric Merlin, Sonia Fornasier, Jean-Michel Reess, Pernelle Bernardi,
Shigeru Imai, Yasuyuki Ito, Hatsumi Ishida, Kiyoshi Kuramoto and Yasuhiro Kawakatsu    8In situ science on Phobos with the Raman spectrometer for MMX (RAX): preliminary design and feasibility of Raman
measurements . . . . . . . . . . . . . . . . . . Yuichiro Cho, Ute Böttger, Fernando Rull, Heinz-Wilhelm Hübers, Tomàs Belenguer, Anko Börner,







Maximilian Buder, Yuri Bunduki, Enrico Dietz, Till Hagelschuer, Shingo Kameda, Emanuel Kopp,
Matthias Lieder, Guillermo Lopez-Reyes, Andoni Gaizka Moral Inza, Shoki Mori, Jo Akino Ogura,
Carsten Paproth, Carlos Perez Canora, Martin Pertenais, Gisbert Peter, Olga Prieto-Ballesteros,
Steve Rockstein, Selene Rodd-Routley, Pablo Rodriguez Perez, Conor Ryan, Pilar Santamaria,
Thomas Säuberlich, Friedrich Schrandt, Susanne Schröder, Claudia Stangarone, Stephan Ulamec,
Tomohiro Usui, Iris Weber, Karsten Westerdorff and Koki Yumoto    9The Mars system revealed by the Martian Moons eXploration mission. . . . . . . . . . . . . . . .  Kazunori Ogohara, Hiromu Nakagawa, Shohei Aoki, Toru Kouyama, Tomohiro Usui, Naoki Terada, Takeshi Imamura,Franck Montmessin, David Brain, Alain Doressoundiram, Thomas Gautier, Takuya Hara, Yuki Harada, Hitoshi Ikeda,
Mizuho Koike, François Leblanc, Ramses Ramirez, Eric Sawyer, Kanako Seki, Aymeric Spiga, Ann Carine Vandaele,
Shoichiro Yokota, Antonella Barucci and Shingo Kameda    9The MMX rover: performing in situ surface investigations on Phobos. . . . . . . . . . . . . . . . . . . . . . . Patrick Michel, Stephan Ulamec, Ute Böttger, Matthias Grott, Naomi Murdoch, Pierre Vernazza, Cecily Sunday,

Yun Zhang, Rudy Valette, Romain Castellani, Jens Biele, Simon Tardivel, Olivier Groussin, Laurent Jorda,
Jörg Knollenberg, Jan Thimo Grundmann, Denis Arrat, Gabriel Pont, Stephane Mary, Markus Grebenstein,
Hirdy Miyamoto, Tomoki Nakamura, Koji Wada, Kent Yoshikawa and Kiyoshi Kuramoto   10High-resolution shape models of Phobos and Deimos from stereophotoclinometry. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .  Carolyn M. Ernst, R. Terik Daly, Robert W. Gaskell, Olivier S. Barnouin, Hari Nair,

Benjamin A. Hyatt, Manar M. Al Asad and Kielan K. W. Hoch   10Light detection and ranging (LIDAR) laser altimeter for the Martian Moons Exploration (MMX) spacecraft. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Hiroki Senshu, Takahide Mizuno, Kazuhiro Umetani, Toru Nakura, Akihiro Konishi, Akihiko Ogawa,Hirokazu Ikeda, Koji Matsumoto, Hirotomo Noda, Yoshiaki Ishihara, Sho Sasaki, Naoki Tateno,
Yasuyuki Ikuse, Katsunori Mayuzumi, Teiji Kase and Hisayoshi Kashine   11Cover image: Kuramoto, K. et al., Earth, Planets and Space 2022, 74:12 DOI: 10.1186/s40623-021-01545-7

Contents
Special issue “Martian Moons eXploration: the scientific investigations of Mars and its moons”. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Hidenori Genda, Tomohiro Usui, Nancy L. Chabot, Ramses Ramirez and Keiji Ohtsuki
Martian moons exploration MMX: sample return mission to Phobos elucidating formation processes of habitable planets. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Kiyoshi Kuramoto, Yasuhiro Kawakatsu, Masaki Fujimoto, Akito Araya, Maria Antonietta Barucci,
Hidenori Genda, Naru Hirata, Hitoshi Ikeda, Takeshi Imamura, Jörn Helbert, Shingo Kameda,
Masanori Kobayashi, Hiroki Kusano, David J. Lawrence, Koji Matsumoto, Patrick Michel,
Hideaki Miyamoto, Tomokatsu Morota, Hiromu Nakagawa, Tomoki Nakamura, Kazunori Ogawa,
Hisashi Otake, Masanobu Ozaki, Sara Russell, Sho Sasaki, Hirotaka Sawada, Hiroki Senshu,
Shogo Tachibana, Naoki Terada, Stephan Ulamec, Tomohiro Usui, Koji Wada,
Sei-ichiro Watanabe and Shoichiro Yokota

Modelling cometary meteoroid stream traverses of the Martian Moons eXploration (MMX) spacecraft en route to Phobos. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Harald Krüger, Masanori Kobayashi, Peter Strub, Georg-Moragas Klostermeyer,
Maximilian Sommer, Hiroshi Kimura, Eberhard Grün and Ralf Srama

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Analytical protocols for Phobos regolith samples returned by the Martian Moons eXploration (MMX) mission. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Wataru Fujiya, Yoshihiro Furukawa, Haruna Sugahara, Mizuho Koike, Ken-ichi Bajo, Nancy L. Chabot,
Yayoi N. Miura, Frederic Moynier, Sara S. Russell, Shogo Tachibana, Yoshinori Takano,
Tomohiro Usui and Michael E. Zolensky

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MIRS: an imaging spectrometer for the MMX mission. . . . . . . . . . . . . . . . . . . . . . . Maria Antonietta Barucci, Jean-Michel Reess, Pernelle Bernardi, Alain Doressoundiram, Sonia Fornasier,Michel Le Du, Takahiro Iwata, Hiromu Nakagawa, Tomoki Nakamura, Yves André, Shohei Aoki,
Takehiko Arai, Elisa Baldit, Pierre Beck, Jean-Tristan Buey, Elisabet Canalias, Matthieu Castelnau,
Sebastien Charnoz, Marc Chaussidon, Fréderic Chapron, Valerie Ciarletti, Marco Delbo, Bruno Dubois,
Stephane Gauffre, Thomas Gautier, Hidenori Genda, Rafik Hassen-Khodja, Gilles Hervet, Ryuki Hyodo,
Christian Imbert, Takeshi Imamura, Laurent Jorda, Shingo Kameda, Driss Kouach, Toru Kouyama,
Takeshi Kuroda, Hiroyuki Kurokawa, Laurent Lapaw, Jeremie Lasue, Laetitia Le Deit, Aurélien Ledot,
Cedric Leyrat, Bertrand Le Ruyet, Moe Matsuoka, Frederic Merlin, Hideaki Miyamoto, Frederic Moynier,
Napoleon Nguyen Tuong, Kazunori Ogohara, Takahito Osawa, Jérôme Parisot, Laurie Pistre,
Benjamin Quertier, Sean N. Raymond, Francis Rocard, Takeshi Sakanoi, Takao M. Sato,
Eric Sawyer, Fériel Tache, Sylvain Trémolières, Fuminori Tsuchiya,
Pierre Vernazza and Didier Zeganadin

Small-scale topographic irregularities on Phobos: image and numerical analyses for MMX mission. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Tomohiro Takemura, Hideaki Miyamoto, Ryodo Hemmi, Takafumi Niihara and Patrick Michel
Surface environment of Phobos and Phobos simulant UTPS
. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Hideaki Miyamoto, Takafumi Niihara, Koji Wada, Kazunori Ogawa, Hiroki Senshu, Patrick Michel,

Hiroshi Kikuchi, Ryodo Hemmi, Tomoki Nakamura, Akiko M. Nakamura, Naoyuki Hirata,
Sho Sasaki, Erik Asphaug, Daniel T. Britt, Paul A. Abell, Ronald-Louis Ballouz, Olivier S. Banouin,
Nicola Baresi, Maria A. Barucci, Jens Biele, Matthias Grott, Hideitsu Hino, Peng K. Hong, Takane Imada,
Shingo Kameda, Makito Kobayashi, Guy Libourel, Katsuro Mogi, Naomi Murdoch, Yuki Nishio,
Shogo Okamoto, Yuichiro Ota, Masatsugu Otsuki, Katharina A. Otto, Naoya Sakatani,
Yuta Shimizu, Tomohiro Takemura, Naoki Terada, Masafumi Tsukamoto,Tomohiro Usui and Konrad Willner

Visibility analysis of Phobos to support a science and exploration platform. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Elliot Sefton-Nash, Guillaume Thébault, Olivier Witasse, Detlef Koschny, Beatriz Sánchez-Canoand Alejandro Cardesín-Moinelo

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In situ observations of ions and magnetic field around Phobos: the mass spectrum analyzer (MSA) for the Martian Moons
eXploration (MMX) mission. . . . . . . . . . . . . . . . . . Shoichiro Yokota, Naoki Terada, Ayako Matsuoka, Naofumi Murata, Yoshifumi Saito,

Dominique Delcourt, Yoshifumi Futaana, Kanako Seki, Micah J. Schaible, Kazushi Asamura,
Satoshi Kasahara, Hiromu Nakagawa, Masaki N. Nishino, Reiko Nomura, Kunihiro Keika,
Yuki Harada and Shun Imajo

MEGANE investigations of Phobos and the Small Body Mapping Tool
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R. Josh Steele and David J. Lawrence

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Design of telescopic nadir imager for geomorphology (TENGOO) and observation of surface reflectance by opticalchromatic imager (OROCHI) for the Martian Moons Exploration (MMX). . . . . . . . . . . . . . . . . . Shingo Kameda, Masanobu Ozaki, Keigo Enya, Ryota Fuse, Toru Kouyama, Naoya Sakatani, Hidehiko Suzuki,

Naoya Osada, Hiroki Kato, Hideaki Miyamoto, Atsushi Yamazaki, Tomoki Nakamura, Takaya Okamoto,
Takahiro Ishimaru, Peng Hong, Ko Ishibashi, Takeshi Takashima, Ryoya Ishigami, Cheng-Ling Kuo, Shinsuke Abe,
Yuya Goda, Hajime Murao, Saori Fujishima, Tsubasa Aoyama, Keiji Hagiwara, Satoko Mizumoto, Noriko Tanaka,
Kousuke Murakami, Miho Matsumoto, Kenji Tanaka and Hironobu Sakuta

MMX geodesy investigations: science requirements and observation strategy. . . . . . . . . . . . . . . . . . . . . . . . Koji Matsumoto, Naru Hirata, Hitoshi Ikeda, Toru Kouyama, Hiroki Senshu, Keiko Yamamoto, Hirotomo Noda,
Hideaki Miyamoto, Akito Araya, Hiroshi Araki, Shunichi Kamata, Nicola Baresi and Noriyuki Namiki

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