Ikeshita/MEF/JAXA-ISAS

Editorial Board (Oct. 2015)
Editor-in-Chief
Yasuo Ogawa, Tokyo Institute of Technology, Japan

Editorial Board
Yosuke Aoki, University of Tokyo, Japan
Stephen Bannister, GNS Science, New Zealand
Benjamin Fong Chao, Academia Sinica, Taiwan
Nobuo Geshi, Geological Survey of Japan, AIST,Japan
Lin-Ni Hau, National Central University, Taiwan
Hauke Hussmann, German Aerospace Center,
Germany
Alexey Kuvshinov, Institute for Geophysics,
Switzerland
Hiroo Kanamori, California Institute ofTechnology, U.S.A.
Kristine M. Larson, University of Colorado, U.S.A.
Takuto Maeda, University of Tokyo, Japan
Koji Matsumoto, National Astronomical
Observatory, Japan
Yasuhiro Nariyuki, University of Toyama, Japan

Nozomu Nishitani, Nagoya University, Japan
Azusa Nishizawa, Japan Coast Guard, Japan
Keiji Ohtsuki, Kobe University, Japan
Taku Ozawa, National Research Institute for Earth
Science and Disaster Prevention, Japan
Takeshi Sakanoi, Tohoku University, Japan
Martha Savage, Victoria University of Wellington,
New Zealand
Shanaka de Silva, Oregon State University, U.S.A.
Hiroshi Takenaka, Okayama University, Japan
Hiroaki Toh, Kyoto University, Japan
Yih-Min Wu, National Taiwan University, Taiwan
Zhongliang Wu, China Earthquake Administration,
China
Toshitsugu Yamazaki, University of Tokyo, Japan
Akimasa Yoshikawa, Kyushu University, Japan

Journal Scope
Earth, Planets and Space (EPS) is the official journal of the 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.
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Yours sincerely,
Prof. Yasuo Ogawa
Editor-in-Chief, Earth, Planets and SpaceEarth, Planets and Space
Okada et al. Earth, Planets and Space (2015) 67:116
DOI 10.1186/s40623-015-0235-x

PREFACEOpen Access

The Earth, Planets and Space Special Issue:“Science of solar system materials examinedfrom Hayabusa and future missions”
Tatsuaki Okada1*, Michael E. Zolensky2, Trevor R. Ireland3 and Toru Yada1
inside wall of the catcher with a Teflon spatula and tapping on the chamber. These samples are consistent withchondritic composition as shown by scanning electron
microscopy (SEM) with energy-dispersive X-ray spectroscopy (EDS). The removal of tens of micron-sized particles(up to 300 μm) in the catcher was started using the newly
developed electrostatic control manipulator. So far, about
500 particles have been catalogued for initial description
about size, shape, SEM images, and representative elemental and mineral composition from EDS spectra (e.g.,
Yada et al. 2014), and part of those catalogued particles
have been delivered for more advanced research including
preliminary examinations and through an international
announcement of opportunity.
The preliminary examination of Hayabusa-returned
samples has successfully unveiled the mineralogical,
petrographic, chemical, and isotopic relationships between an S(IV)-type asteroid and ordinary LL chondrite
meteorites as predicted by ground-based observation(e.g., Binzel et al. 2001, 2010) and provided the first direct evidence that meteorites originate from asteroids(Ebihara et al. 2011; Nakamura et al. 2011; Noguchi
et al. 2011; Tsuchiyama et al. 2011; Yurimoto et al.
2011). The particle-size distribution and existence ofrounded grains (Tsuchiyama et al. 2011) as well as thenoble gas isotopic compositions (Nagao et al. 2011)
have also recorded asteroid surface processes such as
meteoroid impacts, possible granular flow, and solar
wind irradiation on the asteroid surface, which were
not observed in meteorites. Organic analyses have been
also performed (Kitajima et al. 2011; Naraoka et al.
2012), but indigenous organic compounds have notbeen identified from the samples to date.
Investigation of Hayabusa-returned samples has expanded to any interested researchers by applying to theInternational Announcement of Opportunity, and thesuccessful winners started their advanced and sophisticated research. Hayabusa 2013: 1st Symposium of Solar

It is our great pleasure to present the special issue of thejournal Earth, Planets and Space, entitled “Science of
solar system materials examined from Hayabusa and future missions.” We would like to start with a brief introduction of the Hayabusa mission and its story of sample
collection on the asteroid, followed by the curation anddelivery of returned samples to researchers. All of the 14
manuscripts published in this special issue are also
reviewed here.
Hayabusa was the Japan Aerospace Exploration Agency(JAXA) engineering mission to explore and return a sample from a near-Earth asteroid. It was launched in 2003 by
5th M-V launch vehicle, visited and explored asteroid
25143 Itokawa in 2005, and finally returned surface materials from there to Earth in 2010. The purpose of thismission was an engineering experiment of a round-trip
journey to the asteroid, as well as scientific experiments
for understanding the origin and evolution of the earlysolar system by exploring a primitive body. The S-type,sub-kilometer-sized asteroid Itokawa was found to bechondritic in composition and low-density rubble-pilein structure (e.g., Fujiwara et al. 2006). Its surface wasbasically rough and covered with boulders, but smoothterrains such as MUSES-C Regio also existed where thefirst and second touchdown operations were conducted
for sample collection (see Fig. 1).
The returned samples have been curated in JAXA’s
Extraterrestrial Sample Curation Center. These samples
are of small amount and very fine grained, because theimpact-sampling method failed to shoot projectiles forsample acquisition and only floating dust grains enteredinto the sample catcher (see Fig. 2). Thousands ofmicron-sized silicate-dominated grains other than artificial contaminants were found by scraping them from the* Correspondence: okada@planeta.sci.isas.jaxa.jp
1
Institute of Space and Astronautical Science, Japan Aerospace Exploration
Agency, Sagamihara 252-5210, Japan
Full list of author information is available at the end of the article© 2015 Okada et al. Open Access This article is distributed under the terms of the Creative Commons Attribution 4.0
International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, andreproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide alink to the Creative Commons license, and indicate if changes were made.

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Science of solar system materials examined from Hayabusa and future missions
Okada et al. Earth, Planets and Space (2015) 67:116

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after preparing ultrathin-sectioned specimens using ultramicrotomy and focused ion beam techniques.
Keller and Berger (2014) report on their detailed structural and elemental analysis by scanning and transmission electron microscopy of two particles returned by
Hayabusa, which have a 50- to 100-nm-thick disorderedolivine rim surrounding the particles. This evidence of
space weathering by irradiation of solar wind ions andthe number density of ion particle track in the rim suggest the short exposure age of 103 to 104 years. Noguchi
et al. (2014) report results of detailed mineralogical investigation of four Itokawa particles collected from thefirst touchdown site by micro-Raman spectroscopy, scanning electron microscopy, electron microprobe analysis,
X-ray absorption spectroscopy, and transmission electron
microscopy and conclude that those particles are consistent with LL6 and that space weathering (space-weathered
rim and number densities of solar flare tracks) at thissite was less severe than at the second touchdown site
reported in the initial analysis (Noguchi et al. 2011),
which suggests uncertainty in the previously reported exposure history of the surface, and 103 years rather than
104 years of exposure age. Thompson et al. (2014) reportdetailed microchemical and microstructural features indicative of space weathering in a Hayabusa-returned
particle using transmission electron microscopy of the
microtomed ultrathin section of rim regions. They suggestthat solar wind irradiation is likely responsible for thesurface amorphous regions and the multi-layered rims
with a nano-crystalline outer layer underlain by an amorphous inner layer are derived both from micrometeorite
impacts and solar wind irradiation, indicating multiple
surface-processing events on the asteroid. Langenhorst
et al. (2014) report detailed analytical scanning andtransmission electron microscopic investigations on one
olivine-dominated Itokawa particle, which suggests thatthe particle is of LL-chondrite origin as previously reported
and that even regolith particles lacking visible microcraters on their surfaces might have still experienced
shock metamorphism and were involved in collisional
fragmentation. In Harries and Langenhorst (2014), analysis of another Itokawa particle suggests a lower abundance of shock metamorphism relative to the one byLangenhorst et al. (2014), indicating heterogeneity ofshock events on Itokawa or on its parent body. A thinpolycrystalline olivine rim on one face of the particle
may have originated by solar wind irradiation, followedby annealing and recrystallization, which may have occurred due to the warmer surface temperature of Itokawa
near perihelion distances by dynamical orbital evolution.
New analyses and discussion also strengthen the previous results and contribute to building the new prospectsof asteroid and solar system science. Mikouchi et al.
(2014) report the results of a mineralogical investigation

Fig. 1 Digital image of asteroid 25143 Itokawa and the estimatedfirst (high-latitude region) and second (equatorial region) touchdown
sites. Both sites are inside a flat terrain MUSES-C Regio. The image wastaken from Home Position with ONC-T imager on 10 October 2005.
(ST_2448357351_v, http://darts.isas.jaxa.jp/planet/project/hayabusa/
amica.pl)

System Materials was held for these researchers to cometogether and discuss their latest results, giving new prospects to understanding the asteroid-meteorite connection and the early solar system origin and evolution. All
the papers presented in the symposium were invited forsubmission to this EPS special issue, and any papers related to the topics were also welcomed. In the end, 14
manuscripts were successfully completed for publicationin this special issue.
Among the important topics discussed here are thesurface processes discovered in the ultrafine structuresof Hayabusa-returned samples, influenced by space
weathering or shock or thermal alteration mechanism.
This was enabled by advanced analytical techniques forultrafine grains using transmission electron microscopy

Fig. 2 An artist view of the Hayabusa spacecraft just a moment before
the touchdown on the surface of asteroid 25143 Itokawa for samplingwith the horn-shaped sampler (Ikeshita/MEF/JAXA-ISAS). Actual result
was that the impact sampling failed to shoot the projectile for excavating
the surface materials and collecting part of them into the sample
catcher, but only the dusts floating around there were obtained
and consequently returned to Earth

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Kitajima et al. (2015) performed micro-Raman and infrared analysis of the same three particles as measured
by Ito et al. (2014). They found that the Raman spectra
show disordered parameters associated with a low-maturity
level, and hence, the particles are not associated with the
Itokawa asteroid particles. Naraoka et al. (2015) report
TOF-SIMS analysis of three category 3 particles [only one
in common with Ito et al. (2014) and Kitajima et al. (2015)]
in order to determine elemental compositions. These analyses have proven to be difficult because the particles havebeen part of an extended analytical program, and inparticular, the Cs primary ion beam used in the nanoSIMS analysis has pervaded the grain. Nevertheless,
Naraoka et al. (2015) found organic carbon associatedwith nitrogen, fluorine, and silicon, which are uncommon
in nature but quite common in man-made materials. They
concluded that the category 3 particles are likely manmade rather than natural organic matter. Based on thesestudies, it appears that the category 3 particles are notassociated with Itokawa but their specific site of origin
is difficult to determine. On the other hand, Yabuta et al.
(2014) report results of analyses by scanning transmission X-ray microscopy using carbon-, nitrogen-, oxygen-,fluorine-, and calcium-X-ray absorption near-edge structure (XANES) spectroscopy for different kinds of two
carbonaceous particles removed from the Hayabusa spacecraft sample catcher. These were distinct from commercial
or biologic fresh materials, but they were unable to ruleout an extraterrestrial origin for some of these particles.
Additional featured topics discussed in the symposium
and also in this special issue are instrumentation andmethods for sample analysis, as well as remote sensing
or ground-based observations for asteroids, comets, andmeteors. The only such manuscript published in this special issue is by Mediedo (2014), which reports the newly
developed ground robotic spectroscopic observation
system for determining the composition of fireballs, thesolar system materials ablating during atmosphere entry.
The derived physico-chemical data are expected to contribute to a systematic characterization of materials coming from different comets and asteroids.
All the 14 manuscripts in this special issue are fruitfuland constructive for discussion about the asteroid-meteorite
connection and the early solar system origin and evolution.
Detailed analysis of Hayabusa-returned samples is not
yet complete and will continue with more sophisticatedand more statistically significant analyses and techniques.
In the near future, sample returns from C-type asteroid
1999JU3 by Hayabusa 2 in 2020 and from B-type asteroid
Bennu by OSIRIS-Rex in 2023 are expected to advanceasteroid and solar system science, and we believe thatthe developed methodology and lessons learned fromthe analysis of the Hayabusa-returned samples will playa significant role in these missions.

of seven Itokawa particles collected from the first touchdown site of Itokawa through field emission secondary
electron microscopy, synchrotron radiation X-ray diffraction, and X-ray absorption near-edge structure analysis andconcluded that the particles are slightly shocked equilibrated LL chondrite, as suggested in the preliminary examination. Connolly et al. (2015) discussed the formation ofrounded shape grains included in the samples returned by
Hayabusa (e.g., Tsuchiyama et al. 2011) and argued that the
Itokawa surface was in a high-energy environment possibly
caused by the YORP effect to raise a continuous granularflow. In their hypothesis, the portion of rounded to angulargrains is higher for C-type relative to S-type asteroids,
which could be verified by samples returned by Hayabusa
2 or OSIRIS-REx. Takeda et al. (2015) report on themineralogy of three LL chondrites (possibly related to
Itokawa) that partial melts found in them indicate thateven a primitive solar system parent body of such as LL
chondrites experienced partial melting and suggests that
granulitic materials may have been formed at depths
within their parent body by an impact event.
Discussions concerning the category 3 particles are
specially featured topics in this special issue. Hayabusareturned samples are classified into four categories.
Category 1 and 2 particles consist of silicate minerals
without or with a metallic component, respectively,
and most of them are considered to have been indigenous
to Itokawa. Category 4 includes artificial materials frominside the sample catcher or from the sampling tools.
Category 3 particles from Itokawa represent a numberof samples that are predominantly composed of carbon
or carbon compounds. The lack of carbon in any of thetype I or II grains that have been proven to originate on
Itokawa has raised suspicion that the category 3 particles
are contaminants of possibly terrestrial origin or arematerials that may have originated from the surface ofthe Hayabusa spacecraft. In a series of five studies inthis issue, the possible origins of category 3 particles
are addressed.
Uesugi et al. (2014) report preliminary results of theanalyses of five category 3 (carbonaceous) materials removed from the Hayabusa spacecraft sample catcher andconclude that differences in their microstructure andelemental distributions suggest multiple origins. They also
inform the summary of damage occurring on thosesamples by each analytical process as lessons learned
for future sample return analysis of carbonaceous materials expected by the Hayabusa 2 and OSIRIS-REx
missions. Ito et al. (2014) have measured H, C, and N
isotopic compositions of three category 3 particles
with ion imaging on a nanoSIMS ion microprobe. Isotopic
compositions of these elements are quite variable in extraterrestrial samples; however, they have found that theisotopic compositions are all within error of terrestrial.

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Author details
1
Institute of Space and Astronautical Science, Japan Aerospace Exploration
Agency, Sagamihara 252-5210, Japan. 2Astromaterials Research andExploration Science, NASA Johnson Space Center, Houston, TX 77058, USA.
3
Research School of Earth Sciences, The Australian National University,
Canberra ACT 0200, Australia.

SA, Ishibashi Y, Abe M, Okada T, Ueno M, Mukai T, Yoshikawa M, Kawaguchi J(2011) Itokawa dust particles: a direct link between S-type asteroids andordinary chondrites. Science 333:1113–1116
Naraoka H, Mita H, Hamase K, Mita M, Yabuta H, Saito K, Fukushima K, Kitajima F,
Sandford SA, Nakamura T, Noguchi T, Okazaki R, Nagao K, Ebihara M,
Yurimoto H, Tsuchiyama A, Abe M, Shirai K, Ueno M, Yada T, Ishibashi Y,
Okada T, Fujimura A, Mukai T, Yoshikawa M, Kawaguchi J (2012) Preliminaryorganic compound analysis of microparticles returned from asteroid 25143
Itokawa by the Hayabusa mission. Geochem J 46:61–72
Naraoka H, Aoki D, Fukushima K, Uesugi M, Ito M, Kitajima F, Mita H, Yabuta H,
Takano Y, Yada T, Ishibashi Y, Okada T, Abe M (2015) ToF-SIMS analysis ofcarbonaceous particles in the sample capsule of the Hayabusa mission, Earth
Planet Space in press
Noguchi T, Nakamura T, Kimura M, Zolensky ME, Tanaka M, Hashimoto T, Konno M,
Nakato A, Ogami T, Fujimura A, Abe M, Yada T, Mukai T, Ueno M, Okada T,
Shirai K, Ishibashi Y, Okazaki R (2011) Incipient space weathering observedon the surface of Itokawa dust particles. Science 333:1121–1125
Noguchi T, Bridges JC, Hicks LJ, Gurman SJ, Kimura M, Hashimoto T, Konno M,
Bradley JP, OkazakiR UM, Yada T, Karouji Y, Abe M, Okada T, Mitsunari T,
Nakamura T, Kagi H (2014) Mineralogy of four Itokawa particles collectedfrom the first touchdown site. Earth Planets Space 66:124
Takeda H, Nagaoka H, Yamaguchi A, Karouji Y, Yazawa Y (2015) Mineralogy ofsome evolved LL chondrites with reference to asteroid materials and solar
system evolution. Earth Planets Space 67:5
Thompson MS, Christoffersen R, Zega TJ, Keller LP (2014) Microchemical andstructural evidence for space weathering in soils from asteroid Itokawa. Earth
Planets Space 66:89
Tsuchiyama A, Uesugi M, Matsushima T, Michikami T, Kadono T, Nakamura T,
Uesugi K, Nakano T, Sandford SA, Noguchi R, Matsumoto T, Matsuno J,
Nagano T, Imai Y, Takeuchi A, Suzuki Y, Ogami T, Katagiri J, Ebihara M, Ireland TR,
Kitajima F, Nagao K, Naraoka H, Noguchi T, Okazaki R, Yurimoto H, Zolensky ME,
Mukai T, Abe M, Yada T et al (2011) Three-dimensional structure of Hayabusa
samples: origin and evolution of Itokawa regolith. Science 333:1121–1125
Uesugi M, Naraoka M, Ito M, Yabuta H, Kitajima F, Takano Y, Mita H, Ohnishi I,
Kebukawa Y, Yada T, Karouji Y, Ishibashi Y, Okada T, Abe M (2014) Sequential
analysis of carbonaceous materials in Hayabusa-returned samples for thedetermination of their origin. Earth Planets Space 66:102
Yabuta H, Uesugi M, Naraoka H, Ito M, Kilcoyne ALD, Sandford SA, Kitajima F,
Mita H, Takano Y, Yada T, Karouji Y, Ishibashi Y, Okada T, Abe M (2014) X-ray
absorption near edge structure spectroscopic study of Hayabusa category 3
carbonaceous particles. Earth Planets Space 66:156
Yada T, Fujimura A, Abe M, Nakamura T, Noguchi T, Okazaki R, Nagao K, Ishibashi Y,
Shirai K, Zolensky ME, Sandford S, Okada T, Uesugi M, Karouji Y, Ogawa M,
Yakame S, Ueno M, Mukai T, Yoshikawa M, Kawaguchi J (2014) Hayabusa
returned sample curation in the planetary material sample curation facility of
JAXA. Meteorit Planet Sci 49:135–153
Yurimoto H, Abe K, Abe M, Ebihara M, Fujimura A, Hashiguchi M, Hashizume K,
Ireland TR, Itoh S, Katayama J, Kato C, Kawaguchi J, Kawasaki N, Kitajima F,
Kobayashi S, Meike T, Mukai T, Nagao K, Nakamura T, Naraoka H, Noguchi T,
Okazaki R, Park C, Sakamoto N, Seto Y, Takei M, Tsuchiyama A, Uesugi M,
Wakaki S, Yada T et al (2011) Oxygen isotopic compositions of asteroidal
materials returned from Itokawa by the Hayabusa mission. Science
333:1116–1119

Received: 19 April 2015 Accepted: 19 April 2015

References
Binzel RP, Rivkin AS, Bus SJ, Sunshine JM, Burbine TH (2001) MUSES‐C target
asteroid (25143) 1998 SF36: a reddened ordinary chondrite. Meteorit PlanetSci 36:1167–1172
Binzel RP, Morbidelli A, Merouane S, DeMeo FE, Birlan M, Vernazza P, Thomas CA,
Rivkin AS, Bus SJ, Tokunaga AT (2010) Earth encounters as the origin of fresh
surfaces on near-Earth asteroids. Nature 463:331–334
Connolly HC Jr, Lauretta DS, Walsh KJ, Tachibana S, Bottke WF Jr (2015) Towards
understanding the dynamical evolution of asteroid 25143 Itokawa: constraints
from sample analysis. Earth Planets Space 67:12. doi:10.1186/s40623-015-0185-3
Ebihara M, Sekimoto S, Shirai N, Hamajima Y, Yamamoto M, Kumagai K, Oura Y,
Ireland TR, Kitajima F, Nagao K, Nakamura T, Naraoka H, Noguchi T, Okazaki R,
Tsuchiyama A, Uesugi M, Yurimoto H, Zolensky ME, Abe M, Fujimura A,
Mukai T, Yada T (2011) Neutron activation analysis of a particle returned fromasteroid Itokawa. Science 333:1119–1121
Fujiwara A, Kawaguchi J, Yeomans DK, Abe M, Mukai T, Okada T, Saito J, Yano H,
Yoshikawa M, Scheeres DJ, Barnouin-Jha O, Cheng AF, Demura H, Gaskell RW,
Hirata N, Ikeda H, Kominato T, Miyamoto H, Nakamura AM, Nakamura R, Sasaki S,
Uesugi K (2006) The rubble-pile asteroid Itokawa as observed by Hayabusa.
Science 312:1330–1334
Harries D, Langenhorst F (2014) The mineralogy and space weathering of aregolith grain from 25143 Itokawa and the possibility of annealed solar winddamage. Earth Planets Space 66:163
Ito M, Uesugi M, Naraoka H, Yabuta H, Kitajima F, Mita H, Takano Y, Karouji Y,
Yada T, Ishibashi Y, Okada T, Abe M (2014) H, C, and N isotopic compositionsof Hayabusa category 3 organic samples. Earth Planets Space 66:91
Keller L, Berger E (2014) A transmission electron microscope study of Itokawa
regolith grains. Earth Planets Space 66:71
Kitajima F, Kotsugi M, Ohkochi T, Naraoka H, Ishibashi Y, Abe M, Fujimura A,
Okazaki R, Yada T, Nakamura T, Noguchi T, Nagao K, Tsuchiyama A, Mukai T,
Sandford SA, Okada T, Shirai K, Ueno M, Yoshikawa M, Kawaguchi J (2011) A
micro-spectroscopic approach to the carbonaceous matter in the particles
recovered by the Hayabusa mission, (Abstract #1855), 42nd Lunar andPlanetary Science Conference
Kitajima F, Kotsugi M, Ohkochi T, Naraoka H, Ishibashi Y, Uesugi M, Karouji Y, Abe M,
Fujimura A, Yada T, Okazaki R, Nakamura T, Noguchi T, Nagao K, Tsuchiyama A,
Yurimoto H, Ebihara M, Ito M, Yabuta H, Mita H, Takano Y, Mukai T, Sandford SA,
Okada T, Shirai K, Ueno M, Yoshikawa M, Kawaguchi J (2015) A micro-Raman
and infrared spectroscopic approach to the several stony and organic(category 3) particles recovered by the Hayabusa mission. Earth Planets
Space 67:20
Langenhorst F, Harries D, Pollok P, van Aken A (2014) Mineralogy and defectmicrostructure of an olivine-dominated Itokawa dust particle: evidence forshock metamorphism, collisional fragmentation, and LL chondrite origin.
Earth Planets Space 66:118
Mediedo JM (2014) Robotic systems for the determination of the composition ofsolar system materials by means of fireball spectroscopy. Earth Planets Space
66:70
Mikouchi T, Komatsu M, Hagiya K, Ohsumi K, Zolensky ME, Hoffmann V, Martinez J,
Hochleitner R, Kaliwoda M, Terada Y, Yagi N, Takata M, Satake W, Aoyagi Y,
Takenouchi A, Karouji Y, Uesugi M, Yada T (2014) Mineralogy andcrystallography of some Itokawa particles returned by the Hayabusa
asteroidal sample return mission. Earth Planets Space 66:82
Nagao K, Okazaki R, Nakamura T, Miura YN, Osawa T, Bajo K, Matsuda S, Ebihara M,
Ireland TR, Kitajima F, Naraoka H, Noguchi T, Tsuchiyama A, Yurimoto H,
Zolensky ME, Uesugi M, Shirai K, Abe M, Yada T, Ishibashi Y, Fujimura A, Mukai T,
Ueno M, Okada T, Yoshikawa M, Kawaguchi J (2011) Irradiation history of
Itokawa regolith material deduced from noble gases in the Hayabusa samples.
Science 333:1128–1131
Nakamura T, Noguchi T, Tanaka M, Zolensky ME, Kimura M, Tsuchiyama A, Nakato A,
Ogami T, Ishida H, Uesugi M, Yada T, Shirai S, Fujimura A, Okazaki R, Sandford

4Earth, Planets and SpaceFRONTIER LETTER

Open Access

Mineralogy and crystallography of some Itokawa particles returnedby the Hayabusa asteroidal sample return mission
Takashi Mikouchi*, Mutsumi Komatsu, Kenji Hagiya, Kazumasa Ohsumi, Michael E Zolensky, Viktor Hoffmann,
James Martinez, Rupert Hochleitner, Melanie Kaliwoda, Yasuko Terada, Naoto Yagi, Masaki Takata, Wataru Satake,Yuya Aoyagi, Atsushi Takenouchi, Yuzuru Karouji, Masayuki Uesugi and Toru Yada
Earth, Planets and Space 2014, 66:82 doi:10.1186/1880-5981-66-82
Received: 30 April 2014, Accepted: 21 July 2014, Published: 1 August 2014

Abstract
We studied seven Itokawa particles provided by the Japan Aerospace Exploration Agency (JAXA) as first International Announcement ofOpportunity (AO) study mainly using electron and synchrotron radiation X-ray beam techniques. All the analyzed particles were collectedfrom the first-touchdown site and composed of olivine and plagioclase with traces of Ca phosphate and chromite, and do not containpyroxenes. Optical microscopy of these particles shows minor undulatory extinction of olivine and plagioclase, suggesting minor shock
metamorphism (shock stage: S2). The electron microprobe analysis shows that olivine is Fo70-73 and plagioclase is An13-10Or5-7. The synchrotron
radiation X-ray diffraction (SR-XRD) analysis of olivine crystals gives cell dimensions of a = 4.708 to 4.779 Å, b = 10.271 to 10.289 Å, c = 6.017 to
6.024 Å, corresponding to the Fo content of Fo~70 by Vegard’s law. This composition matches theresult obtained by the electron microprobe analysis. The olivine compositions of the analyzed
3 2 -43 1 -6
RA-QD02-0036
QD020036-1(a)particles are consistent with those of LL chondrites. The cell dimensions of two plagioclase
Olivine
3 2 -5crystals (a = 8.180 to 8.194 Å, b = 12.53 to 12.893 Å, c = 7.125 to 7.23 Å, α = 92.6° to 93.00°,
3 3 -12 1 -54 4 -13 3 -3β = 116.36° to 116.75°, γ = 90.03° to 90.17°) indicate that their equilibration temperatures are330
2 2 -3800°C ± 10°C. This temperature is near the peak metamorphic temperature recorded by441
1 0 -5331
equilibrated ordinary chondrites. The size of plagioclase crystals and the homogeneity of olivine
1 1 -3compositions indicate that their petrologic type is ≥5. We also analyzed plagioclase by SR iron
10 m
222
X-ray absorption near-edge structure (SR-XANES) and found that its Fe3+/(Fe2+ + Fe3+) ratio is
3 2 -4
3+
approximately 0.5. Such high Fe abundance indicates the formation under a relatively
214-2 -2 -4oxidizing environment. Thus, all these analyses have reconfirmed that the Itokawa particles-2 -5 -3
returned by the Hayabusa spacecraft are very weakly shocked equilibrated LL chondrites, which-1 -2 1
1 -1 5-2 -5 -2
matches the results of the preliminary examination team.
diffraction image
0 -2 4taken at 30 keV

Keywords: Itokawa; Hayabusa; Olivine; Plagioclase; SR-XRD; SR-XANES; LL chondrites*Corresponding author: Takashi Mikouchi, mikouchi@eps.s.u-tokyo.ac.jp-1 -3 3Figure 1 8 0 -4

RA-QD02-0036
QD020036-1

Plagioclase(b)
8 0 -3

6 0 -7

9 1 -1710

5 -1 -4

10 m

FRONTIER LETTER

5 -1 -3

Open Access
0 0 -3

Microchemical and structural evidence for space weathering in soils
from asteroid Itokawa-1 1 -4

diffraction image
taken at 25-30 keV-2 2 3-5 3 0-5 3 1Michelle S Thompson*, Roy Christoffersen, Thomas J Zega and Lindsay P Keller
Earth, Planets and Space 2014, 66:89 doi:10.1186/1880-5981-66-89
Received: 7 March 2014, Accepted: 30 July 2014, Published: 13 August 2014

Abstract
Here we report microchemical and microstructural features indicative of space weathering in a particle returned from thesurface of asteroid Itokawa by the Hayabusa mission. Space weathering features include partially and completely amorphousrims, chemically and structurally heterogeneous multilayer rims, amorphous surface islands, vesiculated rim textures, andnanophase iron particles. Solar-wind irradiation is likely responsible for the amorphization as well as the associatedvesiculation of grain rims. The multilayer rims contain a nanocrystalline outer layer that is underlain by an amorphous inner
layer, and both have compositions that are distinct from the underlying, crystalline orthopyroxene grain. The multilayer rim
features could be derived from either radiation-induced sputter deposition or vapor deposition from micrometeorite impact
events. The amorphous islands on grain surfaces have a distinctive morphology andcomposition suggesting that they represent surface deposits of melt derived frommicrometeorite impact events. These observations indicate that both irradiation
damage and micrometeorite impacts play a role in surface modification and space
weathering on asteroid Itokawa.

Keywords: Hayabusa; Itokawa; Space weathering; Irradiation; Micrometeorite

impact; Airless body; Transmission electron microscopy; Sample return
analysis

Figure 1*Corresponding author: Michelle S Thompson, mst@lpl.arizona.edu
5

Science of solar system materials examined from Hayabusa and future missions

FRONTIER LETTER

Open Access

Mineralogy and defect microstructure of an olivine-dominatedItokawa dust particle: evidence for shock metamorphism, collisional
fragmentation, and LL chondrite origin
Falko Langenhorst*, Dennis Harries, Kilian Pollok and Peter A van Aken
Earth, Planets and Space 2014, 66:118 doi:10.1186/1880-5981-66-118
Received: 28 February 2014, Accepted: 4 September 2014, Published: 17 September 2014

Abstract
We report here detailed analytical scanning and transmission electron microscopic investigations on an olivine-dominated dust particle(RB-QD04-0042) from the surface of asteroid 25143 Itokawa. The dust particle was returned to Earth by the Hayabusa spacecraft and wasmade available in the context of the first announcement of opportunity for Hayabusa sample investigation. Multiple thin slices wereprepared from the precious particle by means of focused ion beam thinning, providing a unique three-dimensional access to its interior.
The 40 × 50 μm sized olivine particle contains a spherical diopside inclusion and an intimate intergrowth of troilite and tetrataenite. The
compositions of olivine (Fo69Fa31) and diopside (En48Wo42Fs10), as well as the high Ni content of the sulfide-metal alloy, indicate a LL
ordinary chondrite origin in accord with previous classifications. Although no impact crater
exists at the surface of RB-QD04-0042, transmission electron microscopy revealed thepresence of various shock defects in constituent minerals. These defects are planar fracturesand [001] screw dislocations in olivine, multiple {101} deformation twins in tetrataenite andbasal (0001) stacking faults in troilite. These diagnostic shock indicators occur only in a smallzone on one concave side of the dust particle characterized by a high fracture density. Theseobservations can be explained by a collisional event that spalled off material from theparticle’s surface. Alternatively, the dust particle itself could be a spallation fragment of an
impact into a larger regolith target. This suggests that Itokawa dust particles lacking visible
microcraters on their surfaces might have still experienced shock metamorphism and wereinvolved in collisional fragmentation that resulted in the formation of regolith.

Keywords: Hayabusa; Itokawa; Shock metamorphism; Collisional fragmentation;
Ordinary chondrite; Olivine; Tetrataenite; Troilite; Diopside

Figure 1*Corresponding author: Falko Langenhorst, Falko.Langenhorst@uni-jena.de

FULL PAPER 

Open Access

Mineralogy of four Itokawa particles collected from the first
touchdown site
Takaaki Noguchi*, John C Bridges, Leon J Hicks, Steven J Gurman, Makoto Kimura, Takahito Hashimoto,
Mitsuru Konno, John P Bradley, Ryuji Okazaki, Masayuki Uesugi, Toru Yada, Yuzuru Karouji, Masanao Abe,
Tatsuaki Okada, Takuya Mitsunari, Tomoki Nakamura and Hiroyuki Kagi
Earth, Planets and Space 2014, 66:124 doi:10.1186/1880-5981-66-124
Received: 23 May 2014, Accepted: 4 September 2014, Published: 9 October 2014

Abstract
Four Itokawa particles collected from the first touchdown site were mineralogically investigated by optical microscopy,
micro-Raman (μ-Raman) spectrometry, scanning electron microscopy (SEM), electron microprobe analysis (EPMA), X-ray
absorption spectroscopy (XAS), and transmission electron microscopy (TEM). Their mineralogy has an affinity to that of LL6
chondrites based on micro-Raman spectroscopy, EPMA, and XAS analyses. However, the space weathering rims on them areless developed than those observed on the Itokawa particles collected from the second touchdown site. Solar flare tracks are
rarely observed in the four particles, whose number densities were lower than those observed in the Itokawa particles fromthe second touchdown site.

Keywords: Itokawa; XANES; EPMA; TEM; Space weathering; Solar flare tracks

Figure 1*Corresponding author: Takaaki Noguchi, tnoguchi@artsci.kyushu-u.ac.jp
6Earth, Planets and SpaceLETTER

Open Access

Robotic systems for the determination of the composition of solar
system materials by means of fireball spectroscopy
José M Madiedo
Earth, Planets and Space 2014, 66:70 doi:10.1186/1880-5981-66-70
Received: 31 December 2013, Accepted: 30 June 2014, Published: 15 July 2014

Abstract
The operation of the automated CCD spectrographs deployed by the University of Huelva at different observatories along
Spain is described. These devices are providing information about the chemical nature of meteoroids ablating in theatmosphere. In this way, relevant physico-chemical data are being obtained from the ground for materials coming fromdifferent bodies in the Solar System (mainly asteroids and comets). The spectrographs, which work in a fully autonomous way
by means of software developed for this purpose, are being employed to perform asystematic fireball spectroscopic campaign since 2006. Some examples of meteor
spectra obtained by these devices are also presented and discussed.

Keywords: Meteors; Meteoroids; Meteorites; Asteroids; Comets

Figure 1

Corresponding author: José M Madiedo, madiedo@cica.es

LETTER

Open AccessA transmission electron microscope study of Itokawa regolith grains
Lindsay P Keller* and Eve L Berger
Earth, Planets and Space 2014, 66:71 doi:10.1186/1880-5981-66-71
Received: 27 February 2014, Accepted: 10 June 2014, Published: 15 July 2014

Abstract
Analyses of two olivine-rich particles from asteroid 25143 Itokawa returned by the Hayabusa mission (RA-QD02-0125 andRA-QD02-0211) show evidence for space weathering processes that occurred in the Itokawa regolith. Submicrometer impactderived crystalline and glassy grains are observed adhering to the surfaces of the particles, including albite, orthopyroxene,
olivine, augite, pyrrhotite, troilite, melt splashes, and melt spherules. Both particles are surrounded by 50- to 100-nm-thickdisordered rims that are nanocrystalline, not amorphous, and compositionally similar to the grain cores. A pyrrhotite grain
attached to RA-QD02-0125 also shows a disordered rim that is sulfur-depleted with nanophase Fe metal grains decorating theoutermost surface. The structurally disordered rims on the Hayabusa particles likely result from atomic displacement damage
from solar wind ions given the similarity of the rim thickness compared to the implantation depth of solar wind ions. The
outermost few nanometers of the disordered rims are more Si-rich and Mg- and Fe-depleted relative to the cores of the grains
and likely represent a minor accumulation of impact-generated vapors or sputter deposits. Nanophase Fe metal particles arepresent in the rim on RA-QD02-0211 but were not detected in the rim on RA-QD02-0125. Solar flare particle tracks areobserved in RA-QD02-0211 but were not observed in RA-QD02-0125, suggesting short surface exposure times for theparticles, on the order of approximately 103 to 104 years. This result implies thatthe optical effects of space weathering develop far more rapidly than waspreviously recognized.

Keywords: Hayabusa; Itokawa; Space weathering; Irradiation; Micrometeorite
impact; Solar flare tracks; Transmission electron microscopy

Figure 1*Corresponding author: Lindsay P Keller, Lindsay.P.Keller@nasa.gov
7

Science of solar system materials examined from Hayabusa and future missions

LETTER

Open Access

H, C, and N isotopic compositions of Hayabusa category 3 organic
samples
Motoo Ito*, Masayuki Uesugi, Hiroshi Naraoka, Hikaru Yabuta, Fumio Kitajima, Hajime Mita, Yoshinori Takano,
Yuzuru Karouji, Toru Yada, Yukihiro Ishibashi, Tatsuaki Okada and Masanao Abe
Earth, Planets and Space 2014, 66:91 doi:10.1186/1880-5981-66-91
Received: 25 March 2014, Accepted: 7 August 2014, Published: 13 August 2014

Abstract
Since isotopic ratios of H, C, and N are sensitive indicators for determining extraterrestrial organics, we have measured theseisotopes of Hayabusa category 3 organic samples of RB-QD04-0047-02, RA-QD02-0120, and RB-QD04-0001 with ion imaging
using a NanoSIMS ion microprobe. All samples have H, C, and N isotopic compositions that are terrestrial within errors(approximately ±50‰ for H, approximately ±9‰ for C, and approximately ±2‰ for N).
None of these samples contain micrometer-sized hot spots with anomalous H, C, and N
isotopic compositions, unlike previous isotope data for extraterrestrial organic materials, i.e.,
insoluble organic matters (IOMs) and nano-globules in chondrites, interplanetary dust
particles (IDPs), and cometary dust particles. We, therefore, cannot conclude whether these
Hayabusa category 3 samples are terrestrial contaminants or extraterrestrial materials
because of the H, C, and N isotopic data. A coordinated study using microanalysis
techniques including Fourier transform infrared spectrometry (FT-IR), time-of-flightsecondary ion mass spectrometry (ToF-SIMS), NanoSIMS ion microprobe, Raman
spectroscopy, X-ray absorption near edge spectroscopy (XANES), and transmission electron
microscopy/scanning transmission electron microscopy (TEM/STEM) is required tocharacterize Hayabusa category 3 samples in more detail for exploring their origin andnature.

Keywords: H, C, and N isotopes; Ion imaging with NanoSIMS; Hayabusa organic samples

Figure 1*Corresponding author: Motoo Ito, motoo@jamstec.go.jp

LETTER

Open Access

Sequential analysis of carbonaceous materials in Hayabusa-returned
samples for the determination of their origin
Masayuki Uesugi*, Hiroshi Naraoka, Motoo Ito, Hikaru Yabuta, Fumio Kitajima, Yoshinori Takano, Hajime Mita,
Ichiro Ohnishi, Yoko Kebukawa, Toru Yada, Yuzuru Karouji, Yukihiro Ishibashi, Takaaki Okada and Masanao Abe
Earth, Planets and Space 2014, 66:102 doi:10.1186/1880-5981-66-102
Received: 30 March 2014, Accepted: 19 August 2014, Published: 26 August 2014

Abstract
Preliminary results of the analyses of five carbonaceous materials (particle size of approximately 50 μm) from the Hayabusa
spacecraft sample catcher, including their texture, chemistry, and chemical/isotopic compositions, are summarized. The
carbonaceous particles underwent sequential analysis using a series of microanalytical instruments located at several research
institutes and universities. Collected particles were initially classified into four categories: two categories containing
extraterrestrial silicate particles, one category containing metal and quartz particles consistent with contamination from thesample catcher or sample manipulation tools, and a final category containing carbonaceous particles. Analysis of this final
category was the main focus of this study. Through examination of the carbonaceous
materials, the appropriate analytical processes for sample transportation andhandling were optimized to minimize sample damage and terrestrial contamination.
Particles were investigated by transmission electron microscopy/scanningtransmission electron microscopy, and Ca-carbonate inclusions were found in one
particle. In a different particle, a heterogeneous distribution of silicon in a uniform C,
N, and O matrix was found. Though further analysis is required for a strict
determination of particle origin, the differences in the microstructure and elemental
distribution of the carbonaceous particles suggest multiple origins.

Keywords: Hayabusa; Carbonaceous material; Sequential analysis; Microstructuralobservation by TEM/STEM

Figure 1*Corresponding author: Masayuki Uesugi, uesugi@planeta.sci.isas.jaxa.jp
8

Earth, Planets and SpaceLETTER

Open Access

X-ray absorption near edge structure spectroscopic study ofHayabusa category 3 carbonaceous particles
Hikaru Yabuta*, Masayuki Uesugi, Hiroshi Naraoka, Motoo Ito, A L David Kilcoyne, Scott A Sandford, Fumio Kitajima,
Hajime Mita, Yoshinori Takano, Toru Yada, Yuzuru Karouji, Yukihiro Ishibashi, Tatsuaki Okada and Masanao Abe
Earth, Planets and Space 2014, 66:156 doi:10.1186/s40623-014-0156-0
Received: 30 April 2014, Accepted: 12 November 2014, Published: 3 December 2014

Abstract
Analyses with a scanning transmission x-ray microscope (STXM) using x-ray absorption near edge structure (XANES)
spectroscopy were applied for the molecular characterization of two kinds of carbonaceous particles of unknown origin,termed category 3, which were collected from the Hayabusa spacecraft sample catcher. Carbon-XANES spectra of thecategory 3 particles displayed typical spectral patterns of heterogeneous organic macromolecules; peaks corresponding toaromatic/olefinic carbon, heterocyclic nitrogen and/or nitrile, and carboxyl carbon were all detected. Nitrogen-XANES spectraof the particles showed the presence of N-functional groups such as imine, nitrile, aromatic nitrogen, amide, pyrrole, andamine. An oxygen-XANES spectrum of one of the particles showed a ketone group. Differences in carbon- and nitrogenXANES spectra of the category 3 particles before and after transmission electron microscopic (TEM) observations wereobserved, which demonstrates that the carbonaceous materials are electron beam sensitive. Calcium-XANES spectroscopy
and elemental contrast mapping identified a calcium carbonate grain from one of
the category 3 particles. No fluorine-containing molecular species were detected influorine-XANES spectra of the particles. The organic macromolecular features of thecategory 3 particles were distinct from commercial and/or biological ‘fresh (nondegraded)’ polymers, but the category 3 molecular features could possibly reflectdegradation of contaminant polymer materials or polymer materials used on the
Hayabusa spacecraft. However, an extraterrestrial origin for these materials cannot
currently be ruled out.

Keywords: Hayabusa; Category 3 carbonaceous particles; STXM; XANES; Organic
macromolecule

Figure 1*Corresponding author: Hikaru Yabuta, hyabuta@ess.sci.osaka-u.ac.jp

LETTER

Open Access

The mineralogy and space weathering of a regolith grain from 25143
Itokawa and the possibility of annealed solar wind damage
Dennis Harries* and Falko Langenhorst
Earth, Planets and Space 2014, 66:163 doi:10.1186/s40623-014-0163-1
Received: 30 April 2014, Accepted: 26 November 2014, Published: 16 December 2014

Abstract
We report the results of detailed mineralogical investigations by analytical scanning and transmission electron microscopy of particle
RA-QD02-0115 recovered from the surface of asteroid 25143 Itokawa. We divided the 65 μm × 50 μm small particle into eightindividual subsample slices via the focused ion beam method. The particle dominantly consists of olivine and contains inclusions ofmerrillite, tetrataenite/taenite, troilite, chromite, kamacite, and Cl-bearing apatite (in approx. decreasing order of frequency). The
composition of olivine (fayalite 29.8 ± 1.1 mol% and molar Fe/Mn ratio of 57 ± 2) as well as the Ni-rich metal assemblage indicates an
LL-type affinity in accord with previous classifications. The particle shows effects of solar wind irradiation on one of its principal faces.
Olivine developed an approximately 34 nm wide rim composed of low-angle misoriented, nanometer-sized crystallites accompanied
by a small amount of amorphous material. Exposed troilite developed a 4 to 8 nm wide
polycrystalline rim with large-angle misorientations of the iron sulfide nanocrystallites.
Merrilite shows marginally discernable surface damage but was too unstable under theelectron beam for a detailed study. Cl-bearing apatite was found fully crystalline with nodiscernable rim structure. We discuss the unusual polycrystalline nature of the olivine rim
in terms of possible annealing and recrystallization effects, which may have occurred
during periods of time when Itokawa’s surface temperature may have been warmer due tocloser perihelion distances. Model calculations show that the dynamical orbital evolutionof near-Earth asteroids could lead to complex space weathering processes, arising fromthe competing interplay between irradiation-induced damaging and thermally driven
annealing.

Keywords: Hayabusa; Itokawa; Olivine; Troilite; Phosphates; Space weathering;
Orbital evolution; Irradiation; Annealing; Recrystallization*Corresponding author: Dennis Harries, Dennis.Harries@uni-jena.de
9

Figure 1

Science of solar system materials examined from Hayabusa and future missions

LETTER

Open Access

Mineralogy of some evolved LL chondrites with reference to asteroid
materials and solar system evolution
Hiroshi Takeda*, Hiroshi Nagaoka, Akira Yamaguchi, Yuzuru Karouji and Yuuki Yazawa
Earth, Planets and Space 2015, 67:5 doi:10.1186/s40623-014-0167-x
Received: 13 February 2014, Accepted: 4 December 2014, Published: 13 January 2015

Abstract
Mineralogy of three LL chondrites including Y-981971, Y-793214, and Y-790782 indicates that granulitic materials may havebeen formed in some depth of their parent body by an impact event. This process of high-temperature episodes is different
from the records in the differentiated achondrites (howardite-eucrite-diogenite (HED)) possibly from the Vesta-like asteroid.

Keywords: LL chondrite; Partial melting; Metamorphism; Differentiation; Pyroxene;
OlivineFigure 1*Corresponding author: Hiroshi Takeda, takeda.hiroshi@it-chiba.ac.jp

LETTER

Open AccessTowards understanding the dynamical evolution of asteroid 25143
Itokawa: constraints from sample analysis
Harold C Connolly Jr*, Dante S Lauretta, Kevin J Walsh, Shogo Tachibana and William F Bottke Jr
Earth, Planets and Space 2015, 67:12 doi:10.1186/s40623-015-0185-3
Received: 16 April 2014, Accepted: 13 January 2015, Published: 27 January 2015

Abstract
The data from the analysis of samples returned by Hayabusa from asteroid 25143 Itokawa are used to constrain thepreaccretion history, the geological activity that occurred after accretion, and the dynamical history of the asteroid from themain belt to near-Earth space. We synthesize existing data to pose hypotheses to be tested by dynamical modeling and theanalyses of future samples returned by Hayabusa 2 and OSIRIS-REx. Specifically, we argue that the Yarkosky-O’KeefeRadzievskii-Paddack (YORP) effect may be responsible for producing geologically high-energy environments on Itokawa andother asteroids that process regolith and essentially affect regolith gardening.

Keywords: Asteroids; Hayabusa; Itokawa; Cosmic-ray exposure ages; Chondrites

Figure 1*Corresponding author: Harold C Connolly Jr, hconnolly@gc.cuny.edu
10Earth, Planets and SpaceLETTER

Open AccessA micro-Raman and infrared study of several Hayabusa
category 3 (organic) particles
Fumio Kitajima*, Masayuki Uesugi, Yuzuru Karouji, Yukihiro Ishibashi, Toru Yada, Hiroshi Naraoka, Masanao Abe,
Akio Fujimura, Motoo Ito, Hikaru Yabuta, Hajime Mita, Yoshinori Takano and Tatsuaki Okada
Earth, Planets and Space 2015, 67:20 doi:10.1186/s40623-015-0182-6
Received: 1 May 2014, Accepted: 6 January 2015, Published: 11 February 2015

Abstract
Three category 3 (organic) particles (RB-QD04-0001, RB-QD04-0047-02, and RA-QD02-0120) and so-called ‘white object’ foundin the sample container have been examined by micro-Raman and infrared (IR) spectroscopy. In addition, several artificial
substances that could occur as possible contaminants and chondritic insoluble organic matter (IOM) prepared from the
Murchison CM2 chondrite were analyzed. The Raman spectra of the particles show broad G-band and weak D-band. The
G-band parameters plot in the disordered region and close to the artifact produced from a Viton
glove after laser exposure rather than chondritic IOM. The particles were therefore originally at
low maturity level, suggesting that they have not experienced strong heating and are therefore
not related to the LL4-6 parent body. The IR spectra are not similar to that of chondritic IOM.
Furthermore, the particles cannot be identified as some artificial carbonaceous substances,including the white object, which are the possible contaminants, examined in this investigation.
Although it cannot be determined exactly whether the three category 3 particles are
extraterrestrial, the limited IR and Raman results in this investigation strongly suggest theirterrestrial origin. Although they could not be directly related to the artificial contaminants
examined in this investigation, they may yet be reaction products from similar substances thatflew on the mission. In particular, RB-QD04-0047-02 shows several infrared spectral absorption
bands in common with the ‘white object.’ This may relate to the degradation of a polyimide/
polyamide resin.
a

b

c

d

e

f

g

Keywords: The Hayabusa spacecraft; Carbonaceous material; Category 3 particle; Micro-Raman

Skeletal structures ofspectroscopy; Micro-infrared spectroscopy; Insoluble organic matter

Figure 1*Corresponding author: Fumio Kitajima, kitajima@geo.kyushu-u.ac.jp

LETTER

Open Access

ToF-SIMS analysis of carbonaceous particles in the sample catcher ofthe Hayabusa spacecraft
Hiroshi Naraoka*, Dan Aoki, Kazuhiko Fukushima, Masayuki Uesugi, Motoo Ito, Fumio Kitajima, Hajime Mita,
Hikaru Yabuta, Yoshinori Takano, Toru Yada, Yukihiro Ishibashi, Yuzuru Karouji, Takaaki Okada and Masanao Abe
Earth, Planets and Space 2015, 67:67 doi:10.1186/s40623-015-0224-0
Received: 30 April 2014, Accepted: 20 February 2015, Published: 10 May 2015

Abstract
Three carbonaceous category 3 particles (RA-QD02-0180, RB-QD04-0037-01, and RB-QD04-0047-02) returned in the sample
catcher from the Hayabusa spacecraft were analyzed by time of flight-secondary ion mass spectrometry (ToF-SIMS) toestablish an analytical procedure for determination of their origins. By the different analytical schemes, the three particles
gave distinct elemental and molecular ions, in which the organic carbons commonly appear to be associated with nitrogen,silicon, and/or fluorine. The particles could be debris of silicon rubber and fluorinated compounds and are therefore manmade artifacts rather than natural organic matter.

Keywords: Hayabusa spacecraft; Category 3 particle; Carbonaceous material; ToF-SIMS analysis

50 µm

132.91: Cs (+)

Total (+)

Total (-)

91.05 (+)

145.06 (+)

Figure 1*Corresponding author: Hiroshi Naraoka, naraoka@geo.kyushu-u.ac.jp
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Contents
The Earth, Planets and Space Special Issue: “Science of solar system materials examined from Hayabusa and future
missions” . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Tatsuaki Okada, Michael E. Zolensky, Trevor R. Ireland and Toru Yada
Mineralogy and crystallography of some Itokawa particles returned by the Hayabusa asteroidal sample return mission. . . . . Takashi Mikouchi, Mutsumi Komatsu, Kenji Hagiya, Kazumasa Ohsumi, Michael E Zolensky, Viktor Hoffmann, James Martinez,

Rupert Hochleitner, Melanie Kaliwoda, Yasuko Terada, Naoto Yagi, Masaki Takata, Wataru Satake, Yuya Aoyagi,
Atsushi Takenouchi, Yuzuru Karouji, Masayuki Uesugi and Toru Yada

Microchemical and structural evidence for space weathering in soils from asteroid Itokawa. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Michelle S Thompson, Roy Christoffersen, Thomas J Zega and Lindsay P Keller
Mineralogy and defect microstructure of an olivine-dominated Itokawa dust particle: evidence for shock
metamorphism, collisional fragmentation, and LL chondrite origin. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Falko Langenhorst, Dennis Harries, Kilian Pollok and Peter A van Aken
Mineralogy of four Itokawa particles collected from the first touchdown site
. . . . . . . . . . . . . Takaaki Noguchi, John C Bridges, Leon J Hicks, Steven J Gurman, Makoto Kimura, Takahito Hashimoto, Mitsuru Konno,

John P Bradley, Ryuji Okazaki, Masayuki Uesugi, Toru Yada, Yuzuru Karouji, Masanao Abe, Tatsuaki Okada,
Takuya Mitsunari, Tomoki Nakamura and Hiroyuki Kagi

Robotic systems for the determination of the composition of solar system materials by means of fireball spectroscopy. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . José M Madiedo
A transmission electron microscope study of Itokawa regolith grains . . . . . . . . . . . . . . . . . . . . . . . . . Lindsay P Keller and Eve L Berger
H, C, and N isotopic compositions of Hayabusa category 3 organic samples. . . . . . . . . . . . . . . . . . . . . . . . Motoo Ito, Masayuki Uesugi, Hiroshi Naraoka, Hikaru Yabuta, Fumio Kitajima, Hajime Mita, Yoshinori Takano,
Yuzuru Karouji, Toru Yada, Yukihiro Ishibashi, Tatsuaki Okada and Masanao Abe

Sequential analysis of carbonaceous materials in Hayabusa-returned samples for the determination of their origin. . . . . . . Masayuki Uesugi, Hiroshi Naraoka, Motoo Ito, Hikaru Yabuta, Fumio Kitajima, Yoshinori Takano, Hajime Mita, Ichiro Ohnishi,
Yoko Kebukawa, Toru Yada, Yuzuru Karouji, Yukihiro Ishibashi, Takaaki Okada and Masanao Abe

X-ray absorption near edge structure spectroscopic study of Hayabusa category 3 carbonaceous particles. . . . . . . . . . . . . . . . . Hikaru Yabuta, Masayuki Uesugi, Hiroshi Naraoka, Motoo Ito, A L David Kilcoyne, Scott A Sandford, Fumio Kitajima,
Hajime Mita, Yoshinori Takano, Toru Yada, Yuzuru Karouji, Yukihiro Ishibashi, Tatsuaki Okada and Masanao Abe

1

5
5

6

6
7
7

8

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The mineralogy and space weathering of a regolith grain from 25143 Itokawa and the possibility of annealed solar
wind damage . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Dennis Harries and Falko Langenhorst 9
Mineralogy of some evolved LL chondrites with reference to asteroid materials and solar system evolution. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Hiroshi Takeda, Hiroshi Nagaoka, Akira Yamaguchi, Yuzuru Karouji and Yuuki Yazawa 10
Towards understanding the dynamical evolution of asteroid 25143 Itokawa: constraints from sample analysis. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Harold C Connolly Jr, Dante S Lauretta, Kevin J Walsh, Shogo Tachibana and William F Bottke Jr 10
A micro-Raman and infrared study of several Hayabusa category 3 (organic) particles. . . . . . . . . . . . . . . . . . . . . Fumio Kitajima, Masayuki Uesugi, Yuzuru Karouji, Yukihiro Ishibashi, Toru Yada, Hiroshi Naraoka, Masanao Abe,
Akio Fujimura, Motoo Ito, Hikaru Yabuta, Hajime Mita, Yoshinori Takano and Tatsuaki Okada

ToF-SIMS analysis of carbonaceous particles in the sample catcher of the Hayabusa spacecraft. . . . . . . . Hiroshi Naraoka, Dan Aoki, Kazuhiko Fukushima, Masayuki Uesugi, Motoo Ito, Fumio Kitajima, Hajime Mita, Hikaru Yabuta,
Yoshinori Takano, Toru Yada, Yukihiro Ishibashi, Yuzuru Karouji, Takaaki Okada and Masanao Abe

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Cover image: Okada, T. et al., Earth, Planets and Space 2015, 67:116 doi:10.1186/s40623-015-0235-x