The samples recoveries from the Hayabusa sample catcher in the past and the future
T. Yada1, K. Sakamoto1, M. Yoshitake1, K. Kumagai1, Y. Nakano1, T. Matsumoto1, N. Kawasaki1, M. Nishimura2, S. Matsui1,
T. Okada1, M. Abe1, H. Yurimoto1,3, and M. Fujimoto1, 4
1Inst. Space Astronaut. Sci., Japan Aerosp. Explor. Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210,
Japan.
2
Marine Works Japan Ltd., 3-54-1 Oppamahigashi, Yokosuka, Kanagawa 237-0063, Japan.
3
Dept. Earth Sci., Sch. Science, Hokkaido Univ., Kita 8, Nishi 5, Kita-ku, Sapporo, Hokkaido 060-0808, Japan.
4
Earth-Life Sci. Inst., Tokyo Inst. Technol., 2-12-1-1E-1 Ookayama, Meguro, Tokyo 152-8550, Japan.
Introduction:
Hayabusa spacecraft returned the first regolith samples from S-type near Earth asteroid 25143 Itokawa in 2010 [1, 2].
It had tried touchdown sampling twice on the largest smooth terrain called Muses Sea regio of the asteroid, although it did notshoot a Ta bullet to excavate its surface at that time [3]. After returning the recovered samples, they have been extracted from asample container, handpicked one by one, analyzed with an FE-SEM/EDS for identification, and given ID [4]. Note that the
samples have not been exposed to the atmosphere, handled in purified N2 condtion and analyzed in low vacuum condtion. Here,
we describe detail of processes and results of the sample extraction we did and also mention to their future plan and lessons
learned from Hayabusa.
Sample extraction methods from the sample catcher:
The returned samples were situated inside a sample catcher in the sample container. The sample catcher is composedof room A and B (RA and RB) and rotational cylinder (RC) (Fig. 1). Those recovered by the first touchdown should be captured
inside the RB, and the second one inside the RA, and both of them should be left inside the RC because it was a passage to both
the RA and the RB. So far, samples inside them were extracted by four methods, partially described in [4]. At first, the particles
inside the RA were directly handpicked with an electrostatically controlled micromanipulator, although it was so inefficientbecause of its uneven inner structure (Fig. 1). The next, a specially designed Teflon spatula was used for sample recovery fromthe RA to be scooped its inner surface and analyzed directly with the FE-SEM/EDS [2]. It was successful in recovering small
particles inside the RA, although it was difficult to release them from the spatula because they were stuck to its surface made ofTeflon tightly. The third method we tried was to put a quartz glass disk to the opening of the room of the catcher, turn upside
down and tap it on its outside in order to let particles inside fall onto the disk. After the tapping, we reversed it to recover the
disk by tweezers and place it in a quartz petri dish. We performed this method once for both RA and RB, and also recover thecover of RB, an original part of the catcher, in the same way. Then the particles on the disks were handpicked one by one withthe micromanipulator to be analyzed with the FE-SEM/EDS for their initial descriptions. Practically, most of the samples
distributed to preliminary examination, NASA and international announcement of opportunity (AO) have been recovered withthis method. The total number of those described for RA and RB count up more than 700, and almost 200 particles have been
distributed for 51 accepted research proposals in four times of international AOs.
Recently, we developed a metal disk for the sample recovery from the RC. The concept is basically same as the quartz
disks, but a good thing about it is to be able to let the disk stay in the upright position, never turn it upside down in the recovery

Fig. 1. A cross section of a sample container of
Hayabusa. Blown-up samples entering its sampler horn
go into a rotational cylinder at first and then captured ineither Room A or B of the sample catcher.

process, so that large particles which might fall back into the catcher as it would be reversed must stay on the disk. We are now
handpicking particles from the metal disk of the RC and analyzed them with the FE-SEM/EDS.
Future plan and lessons learned for the sample extractions:Now, we are preparing new metal disks for the RA and RB, and will try final recoveries from them in the next year.
Then we will continue to handpick from them to finish describing in 2020, until the sample return of Hayabusa2.
In the viewpoint of lessons learned from a series of implements of sample extractions experienced in the Hayabusa
mission, we should consider a method to extract samples from a sample catcher in designing a new sampling system for a newspacecraft of a sample return mission. It is partially realized in designing Hayabusa2 sampling system, as three rooms of its
sample catcher can be decomposed into each part, which is shaped like a container. However, detail processes of the sample
extraction, which is partially mentioned in [5], was not discussed in its designation. Ideally, a whole sample extraction processes
after its return to the Earth must be discussed and designed in developing a sample recovery system for the future sample return
mission, such as the Martian Moons Exploration, MMX [6].
References:[1] Abe M. et al. 2011. Abstract #1638. 42nd LPSC. [2] Nakamura T. et al. 2011. Science 333: 1113. [3] Yano H. et al. 2006.
Science 312: 1350. [4] Yada T. et al. 2014. Meteoritics & Planetary Science 49:135. [5] Nakano Y. et al. 2017. in this symposium.
[6] Kuramoto K. et al. 2017. Abstract #2086. 48th LPSC.

Readiness of Receiving and Curation facility for Hayabusa2 Asteroid Sample Return Mission
M. Abe1,2, T. Yada1, T. Okada1,3, K. Sakamoto1, M. Yoshitake1, Y. Nakano1, T. Matsumoto1,
N. Kawasaki1, K. Kumagai1, S. Matsui1, M. Nishimura4, and H. Yurimoto5,1
1Institute of Space and Astronautical Science,
2
SOKENDAI,
3
University of Tokyo,
4
Marine Works Japan LTD,
5
Hokkaido University.
Introduction: Astromaterials Science Research Group (ASRG), established in 2015, is continuing curatorial work for
Hayabusa returned samples and developing the curation facility for Hayabusa2 returned samples. JAXA curation facility ofExtraterrestrial Sample Curation Center (ESCuC) was completed in 2008 for Hayabusa returned samples acceptance. Its
conceptual examination was started in 2005, and its specification was decided in 2007 by the advisory committee of theCuration Facility [1]. After receiving the Hayabusa returned samples and curatorial work for them, we are going to researchusing these samples, such as international announcement of opportunity.
Special feature of JAXA curation facility: The feature of JAXA curation facility is the ability to be able to observe, andtake out and keep a precious return sample scientifically, without being exposed to the atmosphere. Thereby, for example,
noble-gas analysis and space weathering observation were enabled while they are difficult in the meteorite research due to the
influence of terrestrial contamination. Moreover, in this facility the handling of the 10-micrometer sized particle is also
possible using electrostatically controlled micromanipulation system installed in a clean chamber under N 2 atmosphere. The
curation facility in which handling of such small samples without exposing to the atmosphere is available is the only one in theworld [1].
Hayabusa2 mission: Hayabusa2 spacecraft will bring back surface samples of the near-Earth C-type asteroid (162173)
Ryugu at the end of 2020. Because the C-type asteroids, of which reflectance spectra are similar to carbonaceous chondrites,
are highly likely to record the long history of the solar system from the beginning to planet formation including the supply ofvolatiles to terrestrial planets, the main scientific goals of the Hayabusa2 mission are the investigations of (a) the origin andevolution of the solar system, and (b) the formation process and structure of the asteroid.
Curatorial work of Hayabusa2 returned samples: After receiving the returned samples of the Hayabusa2 mission,prior to the initial analysis, the phase-1 curation (sample description) will be done at the JAXA receiving and curation facility.
Along with the initial analysis, the phase-2 curation of returned samples will be done for integrated thorough analysis anddescription of samples to build a sample database and to obtain new scientific perspective from thorough analysis of samples.
The phase-2 curation will be done both in JAXA and also in several research institutes outside JAXA led by the JAXA
curation facility.
Preparation of receiving and curation facility for Hayabusa2: We have started examination of receiving facility of
Hayabusa2 returned sample in 2015. Since Hayabusa2 is a sample return mission from C-type asteroid, it is necessary toensure recovery of the volatile matter from the samples containing an organic components and water. Moreover, since
recovery of the mm-sized particles which was not able to be performed by Hayabusa is expected, the technical development
for the description and the handling method for large particles is required.
In Hayabusa2 mission, more attention is paid to contamination control than Hayabusa mission. Final cleaning of the sample
catcher is executed in the curation facility and cleaning level is known. Moreover, the contamination coupon is monitoring thecontaminant during the construction of the sampling devices.
Conceptual design of clean chamber for Hayabusa2: After examination of receiving facility for Hayabusa2, we had
fixed the specification and conceptual design of the clean chambers for Hayabusa2 in this year. The clean chambers are
consisted of mainly two part. One is CC3 in vacuum environment, the other one is CC4 in ultra-pure nitrogen gas environment.
CC3 is separated to 3 rooms, one is used for opening sample container, second one is used for sampling in high vacuum
environment, and third one is used for sample storage. CC4 is separated to 2 rooms, one is micrometer-size samples handlingand sealing of sample holders similar to Hayabusa CC2 clean chamber, second one is millimeter-size samples handling.
Schedule until receiving of returned samples: We have started the production of clean cambers and clean room for thereceiving facility from this year. Clean room had already been completed in this summer and the clean chambers will be
installed by the next summer. After the manufacturing of the curation facility for Hayabusa2, we will execute the rehearsal of
the operation to succeed the curatorial work of the retuned samples of Hayabusa2 until the return of the Hayabusa2 spacecraft
to the Earth.
References[1] Yada T. et al. 2014. . Meteoritics & Planetary Science 49:135.

A REPORT ON THE PREPARATION STATUS OF THE CURATION PROTOCOL FOR HAYABUSA2 SAMPLE
Y. Nakano1, T. Yada1, M. Abe1, T. Okada1 and S. Watanabe2
1Japan Aerospace Exploration Agency (JAXA) and 2Nagoya University
We present an interim report on the returned sample curation protocol of Hayabusa2 project.
Hayabusa2 spacecraft was launched in 2014, and currently en route to a C type asteroid, called Ryugu, that is expected tobe rich in organic compounds and water-bearing minerals. Hayabusa2 is the second asteroid sampling project of JAXA and has
the following scientific and engineering objectives. The scientific objectives are to investigate chemical characteristics of the Ctype asteroid, especially the mineral – water – organic interactions by researching and analyzing its subsurface materials, andthereby to gain insight into its internal structure and reaccumulation process in its formation history. The engineering objectives
are to mature the technology, which had been developed for the past Hayabusa mission, by improving its robustness, reliability
and operability, and to execute the first impact experiment on the asteroid surface [1]. In 2018, Hayabusa2 will begin remotesensing observations over the surface of Ryugu, fire metal impactors to excavate its surface and perform touchdowns forcollecting its surface and/or subsurface materials. Hayabusa2 will leave Ryugu by 2019 and carry the sample, stored in vacuumtight containers, back to Earth in December 2020. Later, the containers will be transported to the Extraterrestrial Sample Curation
Center (ESCuC) in JAXA.
ESCuC is fully responsible for curating all the returned sample of Hayabusa2 and contribute to the Hayabusa2 projectthrough the curation work. We believe that the curation of extraterrestrial samples is a critical interface between sample return
missions and international science communities [2]. To accomplish our role, we have set following goals in our curation protocol:• Handling the returned sample without any contamination as possible;• Providing primary information about bulk returned sample and Ryugu grains obtained in the curation for the
Hayabusa2 project researchers and other scientists;• Creating the database of collected Ryugu grains.
The first goal is obvious, but is most important for ensuring a correctness and maximum output of scientific information
about the asteroid to be obtained from the returned sample. Especially so, since the source of the sample is identified
unambiguously unlike meteorites, which is an utmost advantage of the sample return mission. The goal depends seriously on
the curating work in ESCuC. Therefore, the curation protocol must reduce risk of terrestrial contamination as possible, as wellas prepare for every conceivable contingency.
Primary information about the returned sample, including the total weight and the size distribution of Ryugu grains andtheir physical and chemical states are very important for scientists to properly plan their researches and request suitable samples.
In case any contamination was detected in the returned sample, the level of contamination and when it happened is critical not
only to the scientists but also to the engineers who designed the spacecraft to improve the sampling system for future missions.
The chemical and physical properties of Ryugu sample are necessary information for us to optimize the allocation procedure of
the sample and would be interesting and informative to the scientists when they are designing research plans. We are planning
to use 5% of the returned sample for preliminary examination to obtain necessary data to characterize physical and chemical
properties of the returned sample. The sample allocation on request will also inform researchers of the size, weight and surface
state (e.g., IR spectra) of the requested samples. We have just started selecting analytical instruments and designing analyticalprocedures in our curation protocol. Part of the analysis should be consistent with the Goal-1 defined previously and/or ensure
no interruption in the allocation process.
As already noted, we are responsible for curating all the returned Ryugu sample. We are now developing a nomenclature
for pieces of the sample or grains that are collected from the container. We will create a database for the grains, including
necessary information such as their names, physical properties and histories of removing procedure that occurred during curation
and after allocation as well. Such database would facilitate management of the collected grains and allow scientists to access all
information they need.
We are still considering the best way to curate the returned sample of Hayabusa2 and recognize that there is room forfurther improvement in the current curation protocol.
References: [1] M. Yoshikawa, S. Watanabe and M. Abe (2012) Mission planning document of Hayabusa2, Section 2.3
the Mission Objectives. in Japanese; [2] C. Allen, J. Allton, G. Lofgren, K. Righter, R. Zeigler, and M. Zolensky (2013) Curating
NASA’s Extraterrestrial Samples. EOS Transactions American Geophysical Union., 94, 253-260.

Initial analysis of Ryugu samples
Shogo Tachibana1
1
Department of Natural History Sciences, Hokkaido University

Hayabusa2 spacecraft will bring back surface samples of a near-Earth C-type asteroid Ryugu late 2020. The Hayabusa2
returned-samples will be classified into (1) millimeter-sized coarse grains, (2) <100 µm-sized fine grains, and (3) volatiles
components that will be extracted from the sample container prior to its opening [1–3]. After the first characterization at the
curation facility of Institute of Space and Astronautical Science (ISAS), JAXA, the initial analysis of Ryugu samples will bedone by the Hayabusa2 mission to maximize the scientific achievement of the project for 12 months to prove the potential of
the samples.
Initial analysis of returned samples will focus on revealing the formation and evolution of Ryugu in the early Solar System.
The scientific objectives of sample analysis are listed in the following table, which covers from the presolar history to thecurrent geological activity of the near-Earth asteroid [1].
The initial analysis team will consist of six sub-teams for 1) chemistry (elements and isotopes), 2) petrology andmineralogy of coarse grains (mm-sized grains), 3) petrology and mineralogy of fine grains (<100 µm-sized grains), 4) volatiles,
5) macromolecular organics (insoluble organic matter), and 6) organic molecules (soluble organic matter).
Each sub-team will be an international analysis team led by a researcher who can have a research base in Japan at least ayear before the delivery of the samples (the end of 2020) and throughout the initial analysis phase (2021–2022). The sub-teamleaders will make an analysis and work flow plan in their sub-teams with the IAT members to make the best effort in fulfillingthe scientific goals of the mission through integration of analytical results from each sub-team and on- site remote-sensing data.
The Hayabusa2 project opened a call for nomination of the sub-team leaders in October 2016. All the nominations were
thoroughly reviewed by the Hayabusa2 Sample Allocation Committee (HSAC). The HSAC recommended candidates of the
sub-team leaders to the Hayabusa2 Joint Science Team (HJST) for approval. The initial analysis plan of Ryugu samples will
be presented with the names of approved sub-team leaders at the symposium.

References[1] Tachibana, S., Abe M., Arakawa M., Fujimoto M., Iijima Y., Ishiguro M., K. Kitazato, Kobayashi N., Namiki N., Okada T.,
Okazaki R., Sawada H., Sugita S., Takano Y., Tanaka S., Watanabe S., Yoshikawa M., Kuninaka H. and the Hayabusa2
Project Team (2014) Hayabusa2: Scientific importance of samples returned from C-type near-Earth asteroid (162173) 1999
JU3. Geochem. J. 48, 571-587. doi:10.2343/geochemj.2.0350 [2] Okazaki R., Sawada H., Yamanouchi S., Tachibana S., Miura
Y. N., Sakamoto K., Takano Y., Abe M., Itoh S., Yamada K., Yabuta H., Okamoto C., Yano H., Noguchi T., Nakamura T.,
Nagao K. and The Hayabusa2 SMP Team (2016) Hayabusa2 sample catcher and container: Metal-seal system for vacuum
encapsulation of returned samples with volatiles and organic compounds recovered from C-type asteroid Ryugu. Space Sci.
Rev. 208, 107-124. doi:10.1007/s11214-016-0289-5 [3] Sawada H., Okazaki R., Tachibana, S., Sakamoto K., Takano Y.,
Okamoto C., Yano H., Miura Y. N., Abe M., Hasegawa, S., Noguchi T. and the Hayabusa2 SMP Team (2017) Hayabusa2
sampler: Collection of asteroidal surface material. Space Sci. Rev. 208, 81-106. doi:10.1007/s11214-017-0338-8

Advanced Curation Activities at NASA: Preparing to Receive, Process, and Distribute Samples
Returned from Future Missions
Francis M. McCubbin and Ryan A. Zeigler
NASA Johnson Space Center, 2101 NASA Parkway, mailcode XI2, Houston TX 77058 USA
Introduction: The Astromaterials Acquisition and Curation Office (henceforth referred to herein as NASA Curation
Office) at NASA Johnson Space Center (JSC) is responsible for curating all of NASA’s extraterrestrial samples. Under thegoverning document, NASA Policy Directive (NPD) 7100.10F JSC is charged with curation of all extraterrestrial material
under NASA control, including future NASA missions. The Directive goes on to define Curation as including documentation,
preservation, preparation, and distribution of samples for research, education, and public outreach. Here we briefly describe
NASA’s astromaterials collections and our ongoing efforts related to enhancing the utility of our current collections as well as
our efforts to prepare for future sample return missions. We collectively refer to these efforts as advanced curation.
NASA Curation: The NASA Curation Office presently curates nine different astromaterials collections: (1) Apollo
samples, (2) Luna samples (Soviet Union), (3) Antarctic meteorites, (4) Cosmic dust particles, (5) Microparticle Impact
Collection [formerly called Space Exposed Hardware], (6) Genesis solar wind atoms, (7) Stardust comet Wild-2 particles, (8)Stardust interstellar particles, and (9) Hayabusa asteroid Itokawa particles (JAXA).
In addition, the next missions bringing samples back to Earth are Hayabusa 2/ asteroid Ryugu (JAXA) and OSIRIS-Rex/
asteroid Bennu (NASA), in 2021 and 2023, respectively. We currently house contamination knowledge (CK) witness plates for
OSIRIS-REx, and we will soon begin curating CK witness plates for the Mars 2020 mission, which is going to collect andcache martian samples for possible future return to Earth.
Advanced Curation at NASA: The NASA Curation Office plans for the requirements of future collections in an“Advanced Curation” program. Advanced Curation is tasked with conducting research to develop, invent, integrate, test, andevaluate new and innovative technologies for sample collection, contamination control, clean handling, characterization,
analysis, and curation of astromaterials collected by human and non-human explorers – protecting the scientific integrity ofeach sample from the point of mission inception through long-term preservation and distribution on Earth. As each new sample
collection is returned, new facilities are added to accommodate them.
Advanced Curation at NASA is founded as a cross-disciplinary field of advanced research and development under the
auspices of the Astromaterials Acquisition and Curation Office at NASA Johnson Space Center. Advanced curation conducts
research, explores and invents new innovative technologies and techniques for collection, handling, characterization, analysis,
and curation of astromaterials that could be used in next generation human and robotic space exploration missions and current
collections. Advanced Curation has a primary goal of expanding the sample processing and storage capabilities of NASA’s
astromaterials curation facilities to prepare for future sample return missions as well as maximizing the science returns of ourexisting sample collections. In addition, the program integrates, tests, and evaluates new technologies and operational
procedures for future sample return missions through human and robotic analog studies. These goals are aimed at improving
our core curation functions of protecting the scientific integrity of NASA’s astromaterials collections and serving as
responsible distributors of astromaterials to the global community of sample scientists and educators in a fair, timely, andprofessional manner. The primary result of advanced curation is to reduce contamination to astromaterials and preserve thescientific integrity of all samples from mission inception and through ATLO, sample collection, preliminary examination on
Earth, curation, and secure delivery of the samples to Earth-based laboratories for in-depth scientific analyses.
Curation starts at the inception of a sample return mission, and Advanced Curation is an ever-evolving field with specificfoci that start at the inception of a sample return concept. If we look only at improving upon our current curation capabilities,
we will not be prepared when returned samples require care that is very different from those within our current collections. At
present, most of the samples we curate are geologic in nature, with the exception of the Genesis solar wind atoms that are
implanted within a number of inorganic substrates. All of the samples are kept close to room temperature, and we do not curate
gases, liquids, ices, or biologic materials. However, future sample return missions may bring back samples that require storage
and handling conditions outside of our current capability, so we must prepare for such instances. Additionally, many of oursamples, when kept in the pristine environments of our labs, will maintain their fidelity indefinitely. Returned samples fromfuture missions – ices, for example – may have certain properties that have a short “shelf-life”, and hence curation will need todetermine such shelf lives for particular types of analyses through analog studies so that we can prioritize the order in whichscience questions are answered from a particular collection. Another aspect of advanced curation is expanding our ability
to document samples, analyses, and sample histories.
Concluding Remarks: The return of every extraterrestrial sample is a scientific investment, and the curation facilities andpersonnel are the primary managers of that investment. Our primary goals are to maintain the integrity of the samples andensure that the samples are distributed for scientific study in a fair, timely, and responsible manner. It is only through the longterm stability and support of curation facilities, coupled with the infusion of technological advances realized through newadvanced curation initiatives that the maximum returns on that scientific investment are achieved. In the coming decades,
sample return missions will increase in their complexity with respect to sample storage and sample handling requirements. Ouradvanced curation efforts today ensure we will be poised to curate and handle these samples upon return.

Curating NASA’s Past, Present, and Future Extraterrestrial Sample Collections
Ryan A. Zeigler, Judith H. Allton, Cindy A. Evans, Marc D. Fries, Francis M. McCubbin, Keiko Nakamura-Messenger, Lisa
Pace, Kevin Righter, Michael Zolensky
Astromaterials Research and Exploration Division, NASA JSC, Mailcode XI, 2101 NASA Parkway, Houston, TX 77058
Overview: As codified in NASA Policy Directive (NPD) 7100.10F, the Astromaterials Acquisition and Curation Office atNASA Johnson Space Center (hereafter JSC Curation) is charged with curation of all extraterrestrial material under NASA
control, including future NASA missions. The NPD defines Curation as including documentation, preservation, preparation,and distribution of samples for research, education, and public outreach. Here we briefly describe NASA’s astromaterials
collections, the physical infrastructure involved in the curation process, as well as our plans for future facilities to house our
emerging astromaterials collections.
Current Facilities: JSC Curation curates all or part of nine astromaterial collections in seven clean room suites, comprising 22
different rooms: (1) Apollo Samples (1969; ISO 6-7), (2) Luna Samples (from USSR; 1972; ISO 7), (3) Antarctic Meteorites(1976; ISO 7), (4) Cosmic Dust (1981; ISO 5), (5) Microparticle Impact Collection (formerly called Space Exposed Hardware;
1985; ISO 5), (6) Genesis Solar Wind Atoms (2004; ISO 4); (7) Stardust Comet Particles (2006; ISO 5), (8) StardustInterstellar Particles (2006; ISO 5), (9) Hayabusa Asteroid Particles (from JAXA; 2010; ISO 5). We also curate spacecraft
coupons and witness plates for multiple past and current missions (e.g. Stardust, OSIRIS-REx, as well as upcoming missions(e.g., Mars2020). Thus, we currently curate large rock samples (Apollo, Meteorites), bulk regolith and core samples that are
intimate mixtures of particles ranging from submicron to 1 cm (Apollo), micron-scale individual particles (Cosmic Dust,
Hayabusa), micron-scale particles embedded in aerogel (Stardust), atoms of the solar wind implanted in various materials,
physical pieces of spacecraft that have astromaterials embedded in them (Microparticle Impact Collection), and materials that
capture contamination knowledge for returned extraterrestrial samples (Genesis, Stardust, OSIRIS-REx). In addition to the labsthat house the samples, we have installed and maintained a wide variety of facilities and infrastructure required to support theclean-rooms: >10 different HEPA-filtered air-handling systems, ultrapure dry gaseous nitrogen systems, an ultrapure water(UPW) system, and cleaning facilities to provide clean tools and equipment for the labs. We also have sample preparation
facilities for making thin sections, microtome sections, and even focused ion-beam (FIB) sections to meet the researchrequirements of scientists. To ensure that we are keeping the samples as pristine as possible, we routinely monitor thecleanliness of our clean rooms and infrastructure systems. This monitoring includes: daily monitoring of the quality of our
UPW, weekly airborne particle counts in the labs, monthly monitoring of the stable isotope composition of the gaseous N 2
system, and annual measurements of inorganic or organic contamination in processing cabinets. Additionally, each delivery of
liquid N2 is monitored for contaminants (typically <6 ppm Ar, and <1 ppm all others combined). We also track within our
databases the current and ever-changing characteristics (weight, location, destructive analysis spots) of >250,000 individual
samples across our various collections (including the 19,141 samples on loan to 433 Principal Investigators in 24 countries).
Similarly, there are 100s of thousands of images associated with the samples that are stored on our servers. We also have thesample processing and sample handling records (often hand written) for our older collections.
Future Facilities: The next sample return missions are Hayabusa2 and OSIRIS-REx, in 2020 and 2023 respectively. Detailsof the curation plans for each mission can be found in [1,2]. The designs for a new state-of-the-art suite of clean rooms tohouse these samples at JSC have been finalized. This includes separate ISO class 5 clean rooms to house each collection, acommon ISO class 7 area for general use, an ISO class 7 microtome laboratory, and a separate thin section lab. Additionally, a
new cleaning facility is being designed and procedures developed that will allow for enhanced cleaning of cabinets and tools in
an inorganically, organically, and biologically clean manner. We are also designing a large multi-purpose Advanced Curationlaboratory [3] that will allow us to develop the techniques necessary to fully support the Hayabusa2 and OSIRIS-REx
missions, as well as future possible sample return missions (e.g., Lunar Polar Volatiles, Mars, Comet Surface). A micro-CT
laboratory dedicated to the study of astromaterials has come online this summer within JSC Curation, and we plan to add
additional facilities that will enable non-destructive (or minimally-destructive) analyses of astromaterials in the near future(e.g., micro-XRF, confocal imaging Raman Spectroscopy). These facilities will be available to: (1) develop sample handlingand storage techniques for future sample return missions, (2) be utilized by PET for future sample return missions, (3) for
retroactive PET-style analyses of our existing collections, and (4) for periodic assessments of the existing sample collections.
References [1] Righter K. et. al. (2017) This Symposium. [2] Nakamura-Messenger K. et. al. (2017) This Symposium. [2]McCubbin F. M. et. al. (2017) This Symposium.

Sample curation in support of the OSIRIS-REx asteroid sample return mission
Kevin Righter1, Keiko Nakamura-Messenger2 and OSIRIS-REx Curation Working Group1
NASA Johnson Space Center, Mailcode XI2, 2101 NASA Parkway, Houston, TX 77058
2NASA Johnson Space Center, Mailcode XI3, 2101 NASA Parkway, Houston, TX 77058
The OSIRIS-REx asteroid sample return mission launched to asteroid Bennu Sept. 8, 2016. The spacecraft will arrive at
Bennu in late 2019, orbit and map the asteroid, and perform a touch and go (TAG) sampling maneuver in July 2020. After
sample is stowed and confirmed the spacecraft will return to Earth, and the sample return capsule (SRC) will land in Utah in
September 2023. Samples will be recovered from Utah [2] and then transported and stored in a new sample cleanroom at
NASA Johnson Space Center in Houston [3]. The materials curated for the mission are described here.
a) Materials Archive and Witness Plate Collection: The SRC and TAGSAM were built between March 2014 and Summer of2015, and instruments (OTES,OVIRS, OLA, OCAMS, REXIS) were integrated from Summer 2015 until May 2016. A totalof 395 items were received for the materials archive at NASA-JSC, with archiving finishing ~30 days after launch (with thefinal archived items being related to launch operations)[4]. The materials fall into several general categories including metals(stainless steel, aluminum, titanium alloys, brass and BeCu alloy), epoxies, paints, polymers, lubricants, non-volatile-residue
samples (NVR), sapphire, and various miscellaneous materials. All through the ATLO process (from March 2015 until lateAugust 2016) contamination knowledge witness plates (Si wafer and Al foil) were deployed in the various cleanrooms in
Denver and KSC to provide an additional record of particle counts and volatiles that is archived for current and futurescientific studies. These plates were deployed in roughly monthly increments with each unit containing 4 Si wafers and 4 Al
foils. We archived 128 individual witness plates (64 Si wafers and 64 Al foils); one of each witness plate (Si and Al) was
analyzed immediately by the science team after archiving, while the remaining 3 of each are archived indefinitely.
Information about each material archived is stored in an extensive database at NASA-JSC, and key summary information foreach will be presented in an online catalog.
b) Bulk Asteroid sample: The Touch and Go Sampling Mechanism (TAGSAM) head will contain up to 1.5 kg of asteroid
material. Upon return to Earth, the TAGSAM head with the sample canister will be subjected to a nitrogen purge and thenopened in a nitrogen cabinet in Houston. Once the TAGSAM head is removed from the canister, it will be dis-assembled
slowly and carefully under nitrogen until the sample can be removed for processing in a dedicated nitrogen glovebox. Bennu
surface samples are expected to be sub-cm sized, based on thermal infrared and radar polarization ratio measurements [1].
The upper limit on material collected by the TAGSAM head is ~2 cm. Therefore, we will be prepared to handle, subdivide,
and characterize materials of a wide grain size (from ~10 m to 2 cm), and for both organic (UV fluorescence) and inorganic(SEM, FTIR, optical) properties. Representative portions of the bulk sample will be prepared for JAXA (0.5 %; see also [5])and Canadian Space Agency (4%), with the remaining divided between the science team (<25%) and archived for futurestudies (NASA) (>75%).
c) Contact Pad samples: The base of the TAGSAM head contains 24 contact pads that are designed to trap the upper surface
layer of material and thus offer an opportunity to study asteroid samples that have resided at the very top surface of the regolith.
Asteroid material is trapped on the pads in spring steel Velcro hooks, and material will have to be removed from these pads bycuration specialists in the lab.
d) Hardware: Some canister and SRC hardware items will contain information that will be important to understanding thecollected samples, including the canister gas filter, temperature strips, flight witness plates, and the TAGSAM and canisterparts that might have adhering dust grains.
Some challenges remaining for both bulk sample and contact pad samples include: i) working with intermediate size range(200 to 500 m) samples – a size range NASA has not previously worked in such detail; ii) techniques for removal of contact
pad material from the spring steel hooks, iii) static electrical effects of dust sized particles during sample handling and curation
is likely to be significant, and iv) the TAGSAM head and associated canister hardware will undoubtedly be coated with fineadhering dust grains from Bennu. In the case of collection of a large bulk sample mass, the adhering dust grains may be oflower priority. If a small sample mass is returned, the adhering dust may attain a higher priority, so recovery of adhering dust
grains is an additional challenge to consider. In the year leading up to sample return we plan a variety of sample handlingrehearsals that will enables the curation team to be prepared for many new aspects posed by this sample suite.
References: [1] Lauretta, D.S. et al. (2017) Space Science Reviews, in press. [2] Pace, L. et al. (2017) this meeting. [3] Zeigler,
R. et al. (2017) this meeting. [4] Dworkin, J. et al. (2017) Space Science Reviews, in press. [5] Nakamura-Messenger, K. et al.,this meeting.

The European Space Agency Exploration Sample Analogue Collection (ESA2C) and Curation
Facility – progress update
Caroline Smith1, Sarah-Jane Gill1, Chris Jones1, Kamini Manick1, Giles Miller1, Michael Rumsey1 and Ludovic Duvet2
1
Department of Earth Sciences, Natural History Museum, London, SW7 5BD, UK
2
Human Spaceflight and Robotic Exploration Programmes Directorate, European Space Agency ECSAT, Fermi Avenue,
Harwell Campus, Didcot, Oxfordshire, UK, OX11 0FD

Introduction: Since 2014, the Natural History Museum (NHM) has been the prime contractor to the European Space
Agency (ESA) for defining and initiating the development of a Sample Analogue Collection and Curation Facility in supportof the Robotic Exploration mission preparation programme. The ESA Sample Analogue Collection (ESA2C) will support theongoing or future technology development activities that are required for human and robotic exploration of Mars, Phobos,
Deimos, C-Type Asteroids and the Moon. The long-term goal of this work is to produce a useful and useable resource forengineers and scientists developing technologies for ESA missions.
Analogue Sample Collection: The complex mission architectures and diverse target bodies of interest means that avariety of different analogue materials are required to test all systems that come into contact with the target body, whether
these be part of the spacecraft system, such as landing and/or roving systems (e.g. wheels), sample collection systems (e.g.
drills or scoops) or scientific payload. The analogue materials must replicate as far as possible the expected ‘geological’environment of the target body in terms of both physical/mechanical properties and chemical/mineralogical properties. In
addition to ensuring that the samples as accurately as possible represent the physical and chemical properties of the target
bodies of interest, it is important to select materials that can be readily obtained both now and in the future, in enough volume
that will ensure a sustainable collection. As is the case for the existing NASA lunar and martian analogues (JSC-1A and JSCMars-1A) [1] we have selected samples that are available from commercial suppliers to mitigate the risk of materials becoming
unavailable and to ensure large quantities can be sourced if necessary. Additionally, as our chosen suppliers provide materials
to a number of industries we are confident in the quality control procedures in operation during material production, whichshould allow for good reproducibility in sample properties over time.
Samples selected include a variety of aggregates from the olivine-rich basalts from the Upper Lava Formation of the
Paleogene Antrim Lava Group of Northern Ireland and clay samples from Cyprus, Spain and Senegal. During 2016 and 2017
we carried out a detailed characterisation of the analogue samples’ physical and chemical properties [2,3]: Chemical
properties: Whole-rock chemistry – major, minor and trace element analyses by ICP-AES and ICP-MS. Mineralogy –analytical SEM, EPMA and XRD (whole-rock). Physical properties: Grain size and shape – sieving and visual inspection, Xray micro-CT. Bulk density and porosity – mass-volume measurement and helium pycnometry, X-ray micro-CT. Shearstrength (aggregate and powder samples) – shear box apparatus. Compressive and tensile strength – UCS testing and Brazilian
indirect tensile method.
Sample Analogue Curation Facility: This unique venture will build on the Robotic Exploration mission preparation
programme by establishing methodologies and protocols/procedures for curating the ESA2C, as well as defining and validating
the distribution mechanisms and information exchange protocols for the analogue materials. Underpinning the work will be thedevelopment of the ESA2C database that is currently being developed. Samples will be available to suitable qualified PIs andwe welcome requests for information on the samples we have already acquired and characterized and dialogue with colleagues
who are also working on analogue samples as part of mission development e.g. JAXA’s Martian Moons eXploration (MMX)
mission [4].
As part of ongoing work, further samples have been acquired for the ESA2C - anorthosite blocks from a Norwegian
quarry and basaltic sand/gravel and basaltic/hyaloclastite blocks were collected from the Askja Region in Iceland. Additionally,
sample mixtures will be made up using the characterised clays and basalts for varying grain sizes and clay:basalt ratios tobetter replicate the Phobos/Deimos/C-Type Asteroids and Martian regoliths. We will continue to seek sources of new materials
for potential acquisition and subsequent characterization to enhance the initial collection. A critical part of our work is toactively collaborate with our colleagues in the space mission engineering and planetary sciences communities to ensure that
the ESA2C is a relevant and practical resource for technology development.
References: [1] NASA: https://isru.msfc.nasa.gov/simulantdev.html, 2016. [2] K. Manick et al. LPSC XLVIII, #1220(2017). [3] K. Manick et al. LPSC XLVIII, #1222. [4] M. Fujimoto et al. European Planetary Science Congress, vol. 11,
EPSC2017-136

NASA Sample Return Missions: Recovery Operations
Pace, L. F1, Cannon, R. E.2
NASA Johnson Space Center, Houston, TX USA; 2Hill Air Force Base, UT, USA.

1

The Utah Test and Training Range (UTTR), southwest of Salt Lake City, Utah, is the site of all NASA unmanned sample return
missions. To date these missions include the Genesis solar wind samples (2004) and Stardust cometary and interstellar dust
samples (2006). NASA’s OSIRIS-REx Mission will return its first asteroid sample at UTTR in 2023.
The reason for recovery operations at UTTR is many fold, but the simple reason is that it is the largest contiguous block of
restricted airspace in the continental United States. This airspace covers over 9,000 square kilometers of land and is under thejurisdiction of the U.S. Air Force. Hill Air Force Base (AFB) is responsible for the operation of the range and supports thousandsof test and training exercises each year. This valuable test experience coupled with its robust radar tracking assets is anotherattractive feature of NASA’s chosen landing site. Grounding missions due to weather are uncommon, in fact the Hill AFB OnScene Commander reviewed a sub-set of data earlier in 2017 from the last three years of missions and none were grounded due
to weather – just one was delayed by an hour. Temperature lows during their winter months (December, January and February)
are typically below freezing which could be attractive for a future cold sample return. The soft clay on the range is of particularinterest to sample return capsule (SRC) designers because it offers a landing surface that might save precious spacecraft mass if
padding on the SRC is reduced. As a U. S. military base, non-U. S. citizen visitors must be escorted at all times, but this did not
deter international Genesis or Stardust team members from participating in recovery operations. However, it does require moreplanning due to the approval process for foreign visitors.
Two risk items at UTTR are worth noting for future sample return mission managers: (1) the range contains zones where the
SRC cannot be recovered. In comparison to the large landing footprint the range offers, these prohibited zones are small but
should be factored into a mission’s risk posture; and (2) due to the nature of testing conducted on the range, unfired ordnance isa hazard to visitors of the range. For this reason, no one from NASA goes on the range without military escort, and a military
On-Scene Commander led both recovery teams during all training and actual recovery events. It is expected that this protocol
would be followed for any future sample recovery operation.
Once recovered in the field, UTTR has facilities to accommodate sample assessment. Genesis and Stardust (and OSIRIS-REx
in 2023) took advantage of this by setting up a modular ISO Class 7 cleanroom. After initial investigation in Utah, the SRC wasflown from the UTTR’s military airfield directly to Ellington Field, 12 kilometers from NASA’s Johnson Space Center (JSC)
where the Curation facility resides. Upon arrival at JSC, the Genesis and Stardust samples were initially assessed and prepped
for transfer to their dedicated Curation Facility in an ISO 7 hardware cleanroom. Once transferred to the dedicated Curation
Facility (housed within the same building as the hardware cleanroom, these Curation Facilities are ISO Class 4 and 5,
respectively); preliminary examination of the samples by the Science Team began.
The excitement from a sample return is hard to predict. Upon arrival at JSC for Genesis and Stardust, the media, science team,fellow JSC scientists and even the surrounding community’s interest were overwhelming. This excitement can lead the team towork fast. Try to avoid this and stick with the rehearsed plan. Designate a person or two to talk with outsiders so that the mission
team can focus on what’s important – protecting the samples.

Sample return and the Canadian Space Agency:
Ongoing activities and avenues for international collaboration
Tim Haltigin 1
1
Canadian Space Agency, 6767 route de l’Aéroport, St. Hubert, QC, Canada J3Y 8Y9, timothy.haltigin@canada.ca
Canadian Planetary Exploration Overview: Broadly, the Canadian Space Agency’s (CSA) planetary exploration
program consists of participating in ongoing missions and conducting preparatory activities for missions yet to come. CSA’s
science goals are developed in conjunction with the Canadian academic community, and follow two general themes: (i)understanding the origin and evolution of planetary bodies within the solar system, and (ii) habitability and life detection. As
these goals are squarely aligned with a variety of current and future sample return efforts, CSA – in collaboration with its
international partners – has become increasingly involved in sample return mission operations and planning.
OSIRIS-REx: CSA’s first formal participation on a sample
return effort is with the NASA-led Origins Spectral Interpretation
Resource Identification Regolith Explorer (OSIRIS-REx) mission.
OSIRIS-REx aims to return at least 60g of material from asteroid
Bennu, a primitive carbon-rich B-type asteroid believed to containorganic materials [1]. Canada’s hardware contribution to the missionis the OSIRIS-REx Laser Altimeter (OLA) instrument (Fig. 1), built
by MDA Corporation and led by Principal Investigator Dr. Mike Dalyof York University. OLA is a scanning lidar that will provide highresolution 3D topographic information about the asteroid, helping
Figure 1: The OSIRIS-REx Laser Altimeter
provide geologic context for the spacecraft’s spectral instruments and(Image credit: NASA / Goddard / Debora McCallum)
aiding selection of a site where samples can be collected safely [2].
In return for its contribution of OLA and support of a number of mission Science Team members, Canada will receive
4% of the returned sample. A Canadian OSIRIS-REx Sample Advisory Committee is being targeted to assist in evaluating theappropriate curation partner and to review the proposed Curation Plan. This committee would seek input from international
partners who have heritage in astromaterial curation. Upon successful return of the samples, Canada also aims to maximize thescientific use of its sample allocation, and would thus welcome discussions on potential sample access opportunities withinterested parties.
Mars Sample Return – Mission Architecture and Science Management: Mars Sample Return (MSR) remains oneof the highest priorities of the international planetary science community. Because MSR is likely too large an endeavor to betaken on by any individual country or space agency, international cooperation will be paramount to reaching this goal
successfully. Several agencies throughout the world are evaluating possible contributions to this multi-mission endeavor, withcoordination efforts discussed through the International Mars Exploration Working Group (IMEWG).
In 2014, IMEWG tasked the international Mars Architecture for the Return of Samples (iMARS) working group to
define a mission architecture that could successfully achieve MSR and to outline a science management plan for the returned
samples. Canada played a lead role in this effort, co-chairing both the science and engineering sub-teams. Over two years, theworking group developed an extensive set of findings and recommendations, some of which have already been implemented.
A summary presentation was presented at the Mars Exploration Payload Analysis Group (MEPAG) meeting in 2016 [3], withthe full report expected to be published in fall of 2017.
Mars Sample Return – Caching and Retrieval: One of the key findings from the iMARS team was that a minimumof three flight missions would be required to achieve MSR: (i) sample collection and caching; (ii) sample retrieval, and; (iii)
Earth return. A number of open scientific, technical, and operation questions remain open regarding the execution of thesurface elements, (i) and (ii). With international cooperation coordinated via IMEWG, Canada led robotic field deployments
near Hanksville, Utah (USA) to start answering some of these questions (Fig. 2).
Science operations for the sample cache mission were conducted over four weeks spanning 2015 and 2016. The
mission team conducted operations using a combination of rover-integrated sensors and hand-held instruments, successfully
capturing eight scientifically-selected samples and developing an environmental reconstruction of the “landing site”.
Additionally, a two week deployment in 2016 utilized the rover in its sample retrieval configuration, demonstrating
successfully the adaptive caching approach currently preferred by the Mars 2020 mission [4]. These efforts have advanced
international readiness for an eventual MSR campaign and paved the way for future deployments to further reduce risk.

Figure 2: Sample collection and retrieval configurations of CSA’s Mars Exploration Science Rover (MESR) prototype (Image Credit: CSA)

Science Opportunities for the Future: As human presence expands through the solar system, the Canadian planetary science
community is also interested in evaluating new opportunities for science enabled by human exploration of the Moon and Mars.
In addition to developing potential rover concepts, CSA is conducting science definition work in support of a Human Lunar
Exploration Precursor Program lunar sample return mission. With its international partners, terrestrial field demonstrations are
anticipated in the coming years.
Moreover, a number of open competitions are seeking proposals for sample return missions from various destinationsin the solar system. Although Canadian hardware contributions to these campaigns are not currently anticipated, in many cases
Canadian scientists have been sought to provide expertise in a key mission roles. Depending on the outcome of thecompetitions, it is possible that science support will be enabled by CSA through a competitive co-investigator program.
References: [1] Lauretta D.S. et al. 2015. Meteoritics & Planetary Science 50:834. [2] Lauretta D.S. 2015. In Peltonand Allahdadi (eds). Handbook of Cosmic Hazards and Planetary Defense:544. [3] https://mepag.jpl.nasa.gov/meeting/201603/13_iMARS-FinalPresentation_MEPAG_2016-03-02_FINAL.pdf[4] http://www.asc-csa.gc.ca/eng/rovers/analoguemsrad.asp

In the Cold: The Future of Astromaterials Curation?
Christopher D. K. Herd1
Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, Alberta, T6G 2E3, Canada

1

Introduction: Astromaterials, including meteorites, lunar samples, solar wind, cometary dust, asteroidal regolith andinterplanetary dust, provide a unique record of the conditions that prevailed during the formation of our solar system, and thesubsequent processes involved in the evolution of a variety of planetary bodies. However, the majority of astromaterials
formed in environments not found at the Earth’s surface [1]. Therefore, curation is a critical component in the planning ofsample return missions [1] (and can be captured in the question: Why spend billions to bring samples back if they becomecontaminated during sample handling and curation?).
Modern curation facilities have as their primary goal the isolation of astromaterials from the terrestrial environment [1].
Airborne particulate contaminants are mitigated using HEPA filtration systems, as well as recognized clean room practices(e.g., use of gloves, gowns, boots, etc.). Due to the relative abundance of organic compounds at the Earth’s surface, organic
contamination is particularly problematic, and may be mitigated by specialized handling practices to limit the transfer ofterrestrial organics to the samples, and cleaning procedures and methods for identifying and monitoring contaminants [e.g., 2].
However, astromaterials can be compromised in ways other than simple sorption of non-indigenous compounds on exposed
surfaces, or via mixture with airborne dust. Oxidation and hydrolysis are a type of invasive contamination as both processes
permanently chemically alter the intrinsic compounds and minerals in the sample; for this reason, inert atmospheres are
utilized in curation to limit reaction of the indigenous organics and minerals with atmospheric water and molecular oxygen gas.
However, the recognition of volatile and/or reactive organic species in carbonaceous chondrites [e.g., 3] necessitatesconsiderations of curation at low temperature, in order to prevent the loss of intrinsic volatile species.
Insights from Tagish Lake: The Tagish Lake meteorite fell January 18 2000 onto a frozen lake surface in northern British
Columbia, Canada. Samples of the meteorite were recovered within a week of the fall and kept frozen and untouched by hand(the so-called “pristine specimens”). Studies of the Tagish Lake meteorite demonstrate that it is an ungrouped Type 2
carbonaceous chondrite with affinities to CI and CM chondrites [4]. Tagish Lake is among the most enriched in carbon of allchondrites, containing up to ~6 wt% total C, of which approximately half is organic [5]. The soluble organic component, while
relatively small (~2 % of organic C), contains several classes of compounds of prebiotic interest, including some which areparticularly volatile (e.g., formic acid) [6-8]. Systematic study of different lithologies within Tagish Lake demonstratevariation in organic matter characteristics that correlate with mineralogy and petrology [9]; these variations are thought torepresent a record of the effect of parent body alteration on the structure and composition of the organic matter [10]. Further
details on intrinsic and contaminant organic species found in the Tagish Lake meteorite are summarized by [11].
Cold curation in practice: The pristine specimens of Tagish Lake necessitated the development of a facility that would enable
the documentation, processing and storage of astromaterials under cold, inert conditions. The Subzero Curation Facility for
Astromaterials at the University of Alberta is designed with these considerations in mind, within the limitations of funding
available. At the heart of the facility is an Ar gas glove box (MBraun, Inc.), housed within a controlled environment chambercapable of maintaining temperatures between -30 and -10 °C (Fig. 1). The glove box consists of a single user station made ofbrushed 304 stainless steel with radius corners, with a polycarbonate window with chemical and scratch resistant coating (Fig.
1c). Integrated into the window is a binocular microscope (Leica, Inc.), fitted with a camera adapter (Fig. 1c). An adjustablestage sits beneath the microscope, within the glove box. On the right side of the main box is a secondary, storage box made of
the same materials as the main box (Figure 1c); separated from the main box by a sealable door, this box allows for temporarystorage of samples while experiments (e.g., involving solvents) are being carried out in the main box. The atmosphere within
the glove box is maintained using an MB 20 G gas purifier (MBraun, Inc.); once charged with high-purity oxygen-free(99.998%) argon, the system continuously recirculates the argon through a purification system, which removes airborne
contaminants and maintains O2 and H2O to < 1 ppm. HEPA filters on gas inlets also reduce any particulate matter that may beotherwise be circulated into the glove box. An activated carbon filter unit on the gas outlet for the main glove box removes any
volatile organic compounds that might contaminate the materials used within the purifier; this feature also allows for organic
solvents (e.g., chlorinated solvents such as dichloromethane) to be used within the glove box, either for cleaning purposes or tocarry out organic extractions on samples within a purified inert atmosphere at low temperature. A Class 1000 clean room
(Lasco Services, Inc.) serves as a room temperature anteroom to the freezer chamber (Fig. 1a). This anteroom was establishedto provide a source of clean air for the freezer chamber, since HEPA filtering of the freezer chamber air was not practicable.
The anteroom also provides improved storage for the University of Alberta Meteorite Collection. Further details are provided
in [11], including methods and results pertaining to commissioning of the facility.

Figure 1. The Subzero Curation Facility at the University of Alberta, consisting of a Class 1000 room temperature anteroom (A), and a walkin freezer (B) in which an Ar glove box is housed (C).

Insights into cold curation for future sample return: Processing of Tagish Lake specimens now occurs on a routine basis
within the Subzero Curation Facility for Astromaterials. To date, no significant levels of organic contaminants have been
observed in any meteorite samples, although the use of witness plates is planned but not yet implemented. In practicality, thefacility accomplishes the purpose for which it was built, i.e., to enable the processing of Tagish Lake specimens under clean,cold conditions in an inert atmosphere (although Tagish Lake specimens remain in storage in air, [11]). The two main
limitations encountered thus far in the use of the facility include mitigation of a glove box leak and user comfort – the lowtemperature of the freezer chamber compounds the challenges associated with glove box work. As with any cold environment
work, standard operation involves donning insulated clothing (under the clean room smocks), working with a partner, andlimiting exposure to the cold – typically 15-20 minutes at a time. The main advantage of the facility is the reduced risk to
specimens once they are transferred into the glove box, allowing for frequent user breaks (to warm up). However, in the caseof a sudden leak or atmospheric contamination event, rapid mitigation of the problem can be hampered by the cold, especially
if the user has already been working in that environment before the problem is noticed.
Conclusions: In spite of the challenges, cold curation provides significant advantages over room-temperature curation,
including: the retention of intrinsic volatiles; the suspension or inhibition of microbial activity; the minimization of outgassingof glovebox components; and the reduction in reaction rates of oxidation and hydrolysis of intrinsic organic compounds andminerals. Therefore cold curation is recommended for future sample return from any parent body in which volatile components
are anticipated (e.g., organic-rich asteroids, cometary nuclei, Mars). The optimal design of a cold curation facility will need tobalance the parent-body-specific conditions required to preserve the sample with those which maintain user comfort. In
practice, this will most likely require the ultra-cold (~ -80°C) storage of specimens and the handling and processing ofspecimens under cold (~ -15°C) conditions. Notably, micromanipulation of small samples under cold conditions has yet to betested, and is an important consideration for future sample return mission planning.
References[1] Allen C. et al. 2011. Chemie der Erde - Geochemistry 71:1-20. [2] Calaway M.J. et al. 2014. Organic Contamination
Baseline Study in NASA Johnson Space Center Astromaterials Curation Laboratories, Report S-1159. [3] Botta O. and J.L.
Bada 2002. Surveys in Geophysics 23:411-467. [4] Zolensky M.E. et al. 2002. Meteoritics & Planetary Science 37:737-761.
[5] Grady M.M. et al. 2002. Meteoritics & Planetary Science 37:713-735. [6] Pizzarello S. et al. 2001. Science 293:2236-2239.
[7] Hilts R.W. et al. 2014. Meteoritics & Planetary Science 49:526-549. [8] Glavin D.P. et al. 2012. Meteoritics & Planetary
Science 47:1347-1364. [9] Blinova A.I. et al. 2014. Meteoritics & Planetary Science 49:473-502. [10] Herd C.D.K. et al. 2011.
Science 332: 1304-1307. [11] Herd C.D.K. et al. 2016. Meteoritics & Planetary Science 51:499-519.

Amino Acids in Returned Samples and other Solar System Materials
Jamie E. Elsila
NASA Goddard Space Flight Center, Greenbelt, MD USA

1Introduction:
The organic contents of asteroids and comets reflect early solar system chemistry, as well as the physical and chemical
processes that have occurred in the past 4.5 billion years. Both returned samples and meteorites present an opportunity tounderstand these organic contents. Meteorites provide samples from a diverse selection of solar system bodies, while returned
samples have the advantage of context, known parent bodies, and minimal contamination.
Among the most well-studied of the organic compounds present in these extraterrestrial materials are amino acids. Aminoacids are of particular interest to astrobiology and astrochemistry research for several reasons: (1) they are essential to life on
Earth; (2) they are a structurally diverse group of compounds; and (3) some of them possess large enantiomeric excesses ofextraterrestrial origin. Amino acids have been detected in a variety of meteorites, as well as in materials collected fromNASA’s Stardust mission to Comet Wild-2 and in lunar samples returned by NASA’s Apollo missions. Observations by the
ROSINA mass spectrometer also identified glycine in the coma of 67P/Churyumov-Gerasimenko. The abundances, relative
distributions, enantiomeric ratios, and stable isotopic composition of amino acids in extraterrestrial materials can be used tounderstand formation histories and contamination of these materials.
Amino acids in meteorites:
We have examined the abundances, structural distributions, stable isotopic ratios, and enantiomeric compositions of aminoacids in meteorites from all eight carbonaceous chondrite groups (CI, CM, CR, CO, CV, CK, CH, and CB), as well as
representatives of other meteorite classes[1]. Analytical techniques include liquid chromatography coupled with fluorescence
detection and time-of-flight mass spectrometry (LC-FD/ToF-MS) to sensitively measure abundances, and gas chromatography
coupled with mass spectrometry and isotope-ratio mass spectrometry (GC-MS/IRMS) to measure compound-specific isotopic
ratios. These studies show a wide diversity in the amino acids present across these samples. This diversity highlights thepotential roles of parent body processes and composition on the organic content of these bodies, as well as the potential for avariety of formation mechanisms and organic reservoirs in the solar system. In addition, the observed large L-enantiomeric
excesses of some proteinogenic amino acids in certain meteorites (up to ~60%) may be relevant to understanding the origin ofhomochirality in life on Earth, although the potential mechanisms leading to these enantiomeric excesses are currently poorly
understood.
Amino acids in returned samples:
Analysis of bulk comet-exposed materials from the Stardust collector by LC-FD/ToF-MS revealed several amines and aminoacids, including glycine, methylamine and ethylamine [2]. The origin of these compounds could not be firmly established by
LC-FD/ToF-MS data alone, although the distinctive 1:1 ratio of methylamine to ethylamine suggested a cometary origin for
those compounds. Subsequent GC-MS/IRMS analyses measured the stable carbon isotopic ratios of glycine and determined
its likely extraterrestrial origin for glycine, representing the first detection of a cometary amino acid [3]. The in-situ
measurements of glycine in the coma of 67P/Churyumov-Gerasimenko supported the presence of cometary amino acids [4].
Lunar regolith samples returned by NASA’s Apollo missions were investigated almost immediately after their return, but thesestudies yielded inconclusive identifications about the origins of detected amino acids (e.g. [5,6]), in part due to analyticallimitations. It was not possible to determine if the detected amino acids were indigenous to the lunar samples or the result of
terrestrial contamination. More recently, we applied modern analytical techniques to determine the abundances, distributions,and carbon isotopic ratios of amino acids in lunar regolith from the Apollo 16 and 17 missions. We observed amino acids inlow concentrations in all samples. Isotopic and abundance data suggested that terrestrial biological contamination was a
primary source of the observed amino acids, but that some contribution from meteoritic infall was also present [7].
The material returned by JAXA’s Hayabusa mission from asteroid Itokawa was examined for organic materials, including
amino acids. Five individual particles were extracted with organic solvents, but analyses of these extracts showed amino acids

present only at levels below those seen in a procedural blank [8]. Future studies with hot-water extraction may be possible, but
the small sample sizes available from this returned material may preclude any compound-specific amino acid identification.
Future plans for amino acid studies of returned samples:
Both the samples to be returned by NASA’s OSIRIS-REx mission to asteroid Bennu and JAXA’s Hayabusa2 mission toasteroid Ryugu are expected to be analyzed for amino acids and other organic materials. Asteroid Bennu is a B-type
carbonaceous asteroid whose spectra most closely match those of CI and CM chondrites. A comparison of the amino acidcontent of the Bennu regolith with previous carbonaceous chondrite studies will help in understanding the potential
relationship of these meteorites to asteroid parent bodies. Asteroid Ryugu is a Cg-type asteroid that may preserve some of themost pristine material in the solar system and studies of its organic content and amino acid inventory will add to ourknowledge of extraterrestrial organic formation, distribution, and preservation.
References[1] Elsila J. E. et al. (2016) ACS Central Science, 2, 370-379. [2] Glavin D. P. et al. (2008) Meteorit Planet Sci, 43, 399-413.
[3] Elsila J. E. et al. (2009) Meteorit. Planet. Sci., 44, 1323-1330. [4] Altwegg K. et al. (2016) Science Advances, 2. [5] Harada
K. et al. (1971) Science, 173, 433-435. [6] Hare P. E. et al. (1970) Proc. Apollo 11 Lunar Sci. Conf.; Geochim. Cosmochim.
Acta, Suppl. 4, Vol. 2, 1799-1803. [7] Elsila J. E. et al. (2016) Geochim. Cosmochim. Acta, 172, 357-369. [8] Naraoka H. et al.
(2012) Geochem J, 46, 61-72.

The origin and evolution of organic matter in the solar system: the amino acid content ofinterstellar ices and the primitive carbonaceous chondrite Paris
Z. Martins1, P. Modica2,3, C. Meinert4, B. Zanda5, L.L.S. d’Hendecourt2,6
1
ESE, Imperial College London, SW7 2AZ, UK; 2CNRS, Université Paris XI, Institut d’Astrophysique Spatiale, ‘‘Astrochimieet Origines’’, 91405 Orsay Cedex, France; 3Laboratoire de Physique et Chimie de l’Environnement et de l’Espace (LPC2E),
CNRS/Université d’Orléans, 45071 Orléans, France; 4Université Côte d’Azur, Institut de Chimie de Nice, UMR 7272 CNRS,
06108 Nice, France ; 5Muséum d’Histoire Naturelle, CNRS, 75005, Paris, France; 6Equipe ASTRO, Laboratoire de Physiquedes Interactions Ioniques et Moléculaires, UMR CNRS 7345, Centre de Saint Jérôme - case 252, Université d'Aix-Marseille,
13397 Marseille, France.
The organic matter present in carbonaceous chondrites reflects the physical and chemical reactions that occurred in theinterstellar medium, solar nebula, and/or on their parent bodies [1, 2]. It is possible that organic matter synthetized in the initialmolecular cloud survived the protosolar disk phase, was incorporated into planetesimals that would later form comets andasteroids, and finally experienced (aqueous or thermal) alteration on the parent body of carbonaceous meteorites [3]. Therefore,
laboratory produced interstellar ice analogues, as well as primitive carbonaceous meteorites are precious samples that allow
studying key steps into the origin and evolution of organic matter in the solar system. Amino acids, as well as many othercomplex organic molecules may be formed from ultraviolet irradiation and thermo-processing of interstellar icy grains,accreted into the parent bodies of meteorites [4-6], and finally witness aqueous alteration, which seems to influence theirdistribution and relative abundance [7-11].
In this study, we have analysed the amino acid content of laboratory organic residues produced by simulated photo- andthermo-processing of icy mixtures [12]. These have been considered as analogues for the organic material synthetized ininterstellar or circumstellar icy grains [13-17]. We have also analysed the amino acid content of one of the most primitive CM
chondrites, the Paris meteorite [6]. This meteorite is one of the least aqueously altered CM chondrites analysed to date [18-23].
Our results show that Paris has the lowest relative abundance of β-alanine/glycine (0.15 ± 0.02), which is the smallest βalanine/glycine ratio observed in CM chondrites [6]. The relative abundance of β-alanine/glycine increases with increasing
aqueous alteration, from the CM2.7/2.8 Paris to the CM2.0 MET01070. The isovaline detected in the Paris meteorite is
racemic (corrected D/L = 1.03). This is a good indication that aqueous alteration may be responsible for extending an initial Lenantiomeric excess (Lee) of isovaline [6], but not responsible for creating an isovaline asymmetry [24-31]. Furthermore, ourdata shows that the laboratory organic residues have relative distributions of 4-carbon amino acids in agreement with that of
the Paris meteorite, and that the relative β-alanine/glycine ratio is similar to that of Paris [12]. The analysis of the solubleorganic content of carbonaceous meteorites and laboratory organic residues analogue to interstellar ices helps to increase ourknowledge on the origin and evolution of organic matter in the solar system. It also shows that interstellar ice evolution may be
an important source for organic matter in the solar system. This helps to build links between the different contributions for theformation of complex molecules, i.e. interstellar precursors, solar nebula, the incorporation in asteroids, and finally meteorite
parent body alteration.
References[1] Martins Z and Sephton MA (2009), In “Amino acids, peptides and proteins in organic chemistry”, Wiley-VCH, pp. 3-42.
[2] Martins Z (2011) Elements 7, 35. [3] Messenger S (2000) Nature 404, 968. [4] d'Hendecourt LB et al. (1982) A&A 109, 2,
L12. [5] d'Hendecourt LB et al. (1986) A&A 158, 1-2, 119. [6] Elsila JE et al. (2007) ApJ 660, 911. [7] Glavin D et al. (2006)
Meteorit. Planet. Sci. 41, 889. [8] Glavin D et al. (2011) Meteorit. Planet. Sci. 45, 1948. [9] Martins Z et al. (2007) Meteorit.
Planet. Sci. 42, 2125. [10] Martins Z et al. (2015) Meteorit. Planet. Sci. 50, 926. [11] Elsila JE et al. (2016) 47th LPSC,
Abstract 1533. [12] Modica et al. ApJ, submitted. [13] Muñoz Caro GM et al. (2002) Nature 416, 403. [14] Meinert C &Meierhenrich UJ (2012) Angew. Chem. Int. Ed. 51, 10460. [15] Myrgorodska I et al. (2015) Angew. Chem. Int. Ed. 54, 1402.
[16] de Marcellus P et al. (2011), ApJL 727, 1, L27. [17] Modica P et al. (2014) ApJ 788, 79. [18] Bourot-Denise M et al.
(2010) 41st LPSC, Abstract #1533. [19] Caillet Komorowski C et al. (2011) 74th Annual Meeting of the Meteoritical Society,
Abstract #5289. [20] Caillet Komorowski C et al. (2013) 76th Annual Meeting of the Meteoritical Society, Abstract #5199.
[21] Cournède C et al. (2011) 74th Annual Meeting of the Meteoritical Society, Abstract #5252. [22] Blanchard I et al. (2011)
74th Annual Meeting of the Meteoritical Society, Abstract #5322. [23] Zanda B et al. (2010) 73rd Annual Meeting of the
Meteoritical Society, Abstract #5312. [24] Bonner and Rubenstein (1987) Biosystems 20, 99. [25] Bailey et al. (1998) Science
281, 672. [26] Lucas et al. (2005) OLEB 35, 29. [27] Meinert et al. (2012) ChemPlusChem 77, 186. [28] Meinert et al. (2014)

Angew. Chem. Int. Ed. 53, 210. [29] Modica et al. (2014) ApJ 788, 79. [30] Klussmann M et al. (2006) Nature 441, 621. [31]Glavin D et al. (2012) Meteorit. Planet. Sci. 47, 1347.

Sugars and its related compounds in space and on the early Earth
Yoshihiro Furukawa1, Yoshito Chikaraishi2, Chiaki Abe1, Naohiko Ohkouchi3, and Tomoki Nakamura1
1
Department of Earth Science, Tohoku University
2
Institute of Low Temperature Science, Hokkaido University
3
Japan Agency for Marine-Earth Science and Technology
Sugars are essential components of life, employing as substrates in nucleic acid formation and working as energy resourcein numerous biological reactions. The distribution of sugars, particularly bio-important pentoses and hexose, in space including
the Earth would be important for the origin of life.
Carbonaceous chondrites contain many bio-important molecules suchABC
as amino acids and nucleobases [e.g., 1,2]. Thus, they were a source ofbuilding blocks of life on the prebiotic Earth. The detection of glucose,mannose, arabinose, and xylose by paper chromatography incarbonaceous and enstatite chondrites was originally reported in 1960’s[3,4]. However, the paper chromatography has not sufficient resolution to
identify any sugar isomers, and these reports were not clear proof on their
extraterrestrial origin. Thus, a review concluded that the origin of thesereported sugars were terrestrial contamination [5]. More recently,
Fig. 1: Structures of sugar, sugar acids and sugar
Cooper’s group have intensively investigated sugars and their related
alcohols detected in meteorites. A) dihydroxyace
tone,B) ribonic acid, and C) 2-Deoxypentantonic
compounds in Murchison and Mary carbonaceous chondrites. They foundacid. Cooper et al., 2001.
3-carbon sugar, dihydroxyacetone, several sugar acids, and several sugar
alcohols by gas chromatography/mass spectrometry (GC/MS) (Fig. 1)[6,7]. Some of the detected compounds were confirmed on those extraterrestrial origins by compound-specific carbon isotope
analysis. However, the presence of meteoritic bio-important sugars remained unclear.
The formose-like reaction is a plausible process to form sugars in meteorite parent bodies, on interstellar dusts, and on theprebiotic Earth. In the Formose reaction, the condensation of formaldehyde forms numerous sugars, simultaneously. Ribose isan intermediate product of this reaction. However, characterization of the product “formose” remained insufficient so far,which causes ambiguity in the potential availability of sugars in space.
We developed a protocol to effectively extract sugars from mineral assemblages. Then, we found multiple sugars incarbonaceous chondrites with GC/MS. The carbon isotopic composition of individual sugars in meteorite extracts wasdetermined by gas chromatography/isotope ratio mass spectrometry (GC/IRMS). For comparison, we analyzed the products oftypical Formose reaction simulating meteorite parent bodies. Insoluble organic matter (IOM) was extracted from the samechondrites by demineralization with inorganic acids, and the carbon and nitrogen isotopic compositions of bulk chondrite and
IOM were determined. These carbonaceous chondrites were also investigated by scanning electron microscopy (SEM) toevaluate the aqueous alteration levels. In this talk, we will present our preliminary results of these analyses for sugars incarbonaceous chondrites as well as in several experimental Formose reaction products, and will discuss the availability ofsugars in space including Earth.

References[1] Glavine. D. et al. 2011. Meteoritics & Planetary Science 45: 1948-1972. [2] Callahan M. et al. 2011. Proceedings of the
National Academy of Sciences USA 108: 13995-13998. [3] Degens E.T., Bajor M. 1962. Naturwiss. 49: 605-606. [4] Kaplan
I.R., Degens E.T., Reuter J.H., Geochim. Cosmochim. Acta 27: 805-834. [5] Hayes J.M., 1967. Geochimica et Cosmochimica
Acta 31: 1395-1440. [6] Cooper G. et al. 2001. Nature 414: 879–883. [7] Cooper G. and Rioss A.C. 2016. Proceedings of the
National Academy of Sciences USA. 113: E3322-31.

Constraining Mineralogical Composition of Asteroid Ryugu with Ground-Based Observations
Lucille Le Corre1, Vishnu Reddy2, Juan A. Sanchez1, Driss Takir3, Ed A. Cloutis4, Audrey Thirouin5, Jian-Yang Li1, Seiji
Sugita6, Eri Tatsumi6.
1Planetary Science Institute, Tucson, Arizona, USA
2
Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA
3
SETI Institute, Mountain View, CA, USA
4
Department of Geography, University of Winnipeg, Winnipeg, Manitoba, Canada
5
Lowell Observatory, Flagstaff, AZ, USA
6
Dept. of Earth and Planetary Science, University of Tokyo, Tokyo, Japan
In preparation for the arrival of the Japanese Space Agency’s (JAXA) Hayabusa2 sample return mission to near-Earth asteroid(NEA) (162173) Ryugu, we took the opportunity to characterize the target with a ground-based telescope. We observed Ryugu
using the SpeX instrument in Prism mode on NASA Infrared Telescope Facility (IRTF) on Mauna Kea, Hawaii, on July, 122016 when the asteroid was 18.87 visual magnitude, at a phase angle of 13.3°. The NIR spectra were used to constrain
Ryugu’s surface composition, determine meteorite analogs and study spectral affinity to other asteroids. We also modeled its
photometric properties using archival data. Using the Lommel-Seeliger model we computed the predicted flux for Ryugu at awide range of viewing geometries as well as albedo quantities such as geometric albedo, phase integral, and spherical Bond
albedo. Our computed albedo quantities are consistent with results from Ishiguro et al. (2014). In previous work, Ryugu’s
visible spectrum revealed that it can be classified as a C-type object. In addition, not all previous ground-based observations of
Ryugu detected the 0.7 µm absorption feature due to the presence of phyllosilicates. Our spectrum of Ryugu has a broad
absorption band at 1 µm, a slope change at 1.6 µm, and a second broad absorption band near 2.2 µm, but no well-definedabsorption features over the 0.8-2.5 µm range. The two broad absorption features, if confirmed, are consistent with CO and CV
chondrites. We computed the Reflectance Factor (REFF) of Ryugu at 550 nm, which is consistent with the reflectancemeasured for the CM and CI carbonaceous chondrite groups. Samples of CO and CV chondrites are usually brighter and lessred sloped than Ryugu. It is interesting to note that recent work suggested space weathering could darken and redden the
spectra of carbonaceous chondrites. Our spectrum of Ryugu is different from previously published spectra showing a moreneutral spectral slope, however, this is not the only object with this kind of spectral shape. The shape matches very well thoseof NEA (85275) 1994 LY and Mars-crossing asteroid (316720) 1998 BE7, suggesting that their surface regolith have similar
composition. With a semi-major axis of ~ 1.9 AU, and NEA 1994 LY may come from the inner part of the main asteroid belt.
Asteroid 1998 BE7, with a semi-major axis of ~ 3 AU, probably formed far in the outer part of the main belt. The differences
observed between the spectra of these asteroids could be explained by differences in composition, grain size, space weathering,and phase angle. We also compared the spectrum of Ryugu with that of main belt asteroid (302) Clarissa, the largest asteroid in
the Clarissa asteroid family, suggested as a possible source of Ryugu by Campins et al. (2013). We found that the spectrum ofClarissa shows significant differences with our NIR spectrum of Ryugu. Our analysis shows Ryugu’s spectrum best matches
two CM2 carbonaceous chondrites, Mighei and ALH83100. Previous work suggested CM and CI carbonaceous chondrites are
the most consistent with Ryugu’s spectra. We expect the surface regolith of Ryugu to be altered by a range of factors including
temperature, contamination by exogenic material, and space weathering, posing challenges to link spacecraft and ground-based
data, and sample site selection.
References[1] Campins et al. (2013), The Astronomical Journal, 146:26. [2] Ishiguro et al. (2014), The Astrophysical Journal, 792, 74.

3-μm SPECTROSCOPY OF WATER-RICH METEORITES AND ASTEROIDS:NEW RESULTS AND IMPLICATIONS
D. Takir1, J. P. Emery2, C.A., Hibbitts3, 1SETI Institute, Mountain View, CA 94043, USA;
2
University of Tennessee, Knoxville, TN 37996, USA; 3JHU Applied Physics Laboratory,
Laurel, MD 20723-6005, USA.
Introduction: Ground-based observations of water-rich asteroids are important toconstrain many questions related to the abundance and distribution of volatiles in the earlySolar System, and to the evolution of many diverse Solar System bodies. Recent studies
have revealed that several airless bodies, including the Moon and asteroid Psyche ([1], [2],[3], [4]), show spectral indications of hydration on their surfaces. Absorption features at∼3.0 µm are particularly indicative of aqueous alteration. These absorptions are likely due
to hydroxyl and/or water- bearing materials (OH/H2O) (e.g., [5], [6]), but could also be due
to surficial OH implanted from solar wind or exogenic sources like those seen on Vesta[7]. We are observing and studying 60 new water-rich asteroids in the 3-µm region using
NASA Infrared Telescope Facility (IRTF) and Gemini North telescopes, in addition to the
50 water-rich asteroids previously observed by [6] and [8]. We are also studying additional
carbonaceous chondrite meteroites (e.g., CI, CM, CO, CV, CR, CH, and CB) by measuring
their 3-µm spectra under asteroid-like conditions to determine their mineralogical andspectral indicators. Applying these spectral analyses of carbonaceous chondrites to waterrich asteroids in the 3-µm region has been challenging because chondrite spectra havegenerally been acquired in ambient terrestrial environments, and hence are contaminatedby atmospheric water. In this work, however, chondrite IR reflectance spectra are measured
under asteroid-like conditions (i.e., vacuum and elevated temperatures) to eliminate theadsorbed water that affected previous analyses. This investigation is important for
matching the observed water-rich asteroids to specific chondritic groups for better
understanding of the origin and evolution of our Solar System. Results from this work will
also help analyze and characterize the returned carbonaceous samples from asteroids Bennu (OSIRIS-REx’s target) and Ryugu (Hayabusa2’s target), putting these returned samples
into a wider perspective and broader Solar System context.
Methodology: Ground-based spectra of water-rich asteroids were measured using the longwavelength cross- dispersed (LXD: 1.9-4.2 µm) mode of the SpeX spectrograph/imager at
the NASA IRTF and the cross-dispersed mode of the Near InfraRed Spectrograph (GNIRS)
spectrometer at Gemini North, following the methodology of [6]. New 3-µm bi-directionalreflectance spectra (incidence = 15o, emission = 45o, phase angle = 60o) of carbonaceouschondrites (CVs, COs, and CIs) have been collected at the Johns Hopkins University
Applied Physics Laboratory (JHU APL) under vacuum-desiccated conditions, following
the methodology used in [9].
Results: [8] found that CM (and CI) chondrites are possibly the meteorite analogs forwater-rich asteroids with the sharp 3-µm band, attributed to phyllosilicates. The sharpspectral group contains asteroids that are located in the 2.5 < a < 3.3 AU region. No
meteorite match was found by [8] either for the rounded group, Ceres-like group, or
asteroid Europa-like group. These three spectral groups are located farther from the Sun(3.0 < a < 4.0 AU). Here we present new 3-µm spectra of water-rich asteroids, including
212 Medea, 690 Wratislavia, 372 Palma, 259 Aletheia, 114 Kassandra, 701 Oriola, 360
Carlova, 747 Winchester, 386 Siegena, 356 Liguria 233 Asterope, 135 Hertha, 87 Sylvia,
and 142 Polana. Asteroid Polana, which is the main asteroid in the New Polana Family[10], is thought to be the probable source of primitive near-Earth asteroids including Bennu
and Ryugu [11]. The new 3-µm spectra are grouped according to the classification schemeof [6]. We will also present new 3-µm spectra of carbonaceous chondrites, which will be
used to interpret ground-based, and eventually space-based, spectra of water-rich asteroids.
We will then compare the new spectra of meteorites and asteroids to determine new
possible matches on the basis of the 3-µm band.
References: [1] Clark (2009) Science 5952:552. [2] Pieters et al. (2009) Science 5952:568.
[3] Sunshine et al. (2009) 5952:565. [4] Takir et al. (2017) ApJ 153:1. [5] Rivkin et al.
(2002) In Univ. Of Arizona Asteroids III 235- 253. [6] Takir and Emery (2012) Icarus
219:641-654. [7] Reddy et al. (2012) Icarus 221:544-559. [8] Takir et al. (2015) 257:185193. [9] Takir et al. (2013) 48:1618-1637. [10] Walsh et al. (2013) Icarus 225:283-297.
[11] Bottke et al. (2015) Icarus 247:191-217.

Hayabusa2 landing site selection (LSS) training: Summary report of scientific evaluation
Hikaru Yabuta1, Naru Hirata2, Rie Honda3, Yoshiaki Ishihara4, Kohei Kitazato2, Mutsumi Komatsu5, Akira Miura4, Koji
Matsumoto6, Tomokatsu Morota7, Tomoki Nakamura8, Aiko Nakato9, Takaaki Noguchi10, Tatsuaki Okada4, Naoya Sakatani11,
Seiji Sugita12, Shogo Tachibana12, Satoshi Tanaka4, Eri Tatsumi12, Sei-ichiro Watanabe7, Tomohiro Yamaguchi4, Yukio
Yamamoto4, LSS, AA Team (Hayabusa2 Project)
1
2
Hiroshima University, University of Aizu, 3Kochi University, 4ISAS/JAXA, 5Sokendai, 6NAOJ, 7Nagoya University, 8Tohoku
University, 9Kyoto University, 10Kyushu University, 11Meiji University, 12Tokyo University
The Japanese C-type asteroid sample return mission, Hayabusa2, was launched on December 3, 2014. The spacecraft
is scheduled to arrive at the near Earth asteroid Ryugu on July 2018. During its 18-month stay, remote-sensing observations
will be carried out by the on-board instruments, Optical Navigation Camera (ONC), Near Infrared Spectrometer (NIRS3),
Thermal Infrared Imager (TIR), and Light Detection and Ranging (LIDAR). Based on the observation data, the collection of
the asteroid samples from three sites at maximum will be performed. We will carry out the landing site selection (LSS) withina month after the arrival to Ryugu, for the first touch down and for the release of MASCOT, a small hopping rover developed
by DLR and CNES on October 2018.
It is therefore very important that scientists from remote sensing, MASCOT, and sample analyses are mingled to workout a landing site selection strategy by sharing the common picture of the multi-scale asteroid science. During this June-August
2017, we carried out the LSS training by using the asteroid Ryugu analog model “Ryugoid”. Beginning of shape modeling, thedata products such as surface temperature, thermal inertia, grain sizes, visible and near infrared spectra, and spectral
parameters (albedo, UV slope) were obtained from the Box A (at 20 km in altitude), Box C and mid-a
ltitude (at 5 km in altitude) observations by TIR, ONC, NIRS3, and LIDAR teams. Then, six potential landing sites (zones A,
B, C, D, D2, and E, in figure) were indicated by the system side. Based on the products, scientific evaluations (e.g.,
compositions and distributions of hydrate minerals, relative abundance of organic carbon, thermal metamorphism degree,
space weathering degree, and number density of boulders) of these zones were conducted in order to prioritize the first landingsite. This training has made us prepare for the actual LSS next year, to determine the most scientifically valuable site, that is,water-rich region.
(a) 

4.#Highlights#of#data#products:#NIR3#NIRS#reﬂectance#spectra#
(d) 

(e) 

Zone B 
Zone D, D2, E
Zone A 
Zone C
↓

(b) 

A
Zone B -> Zone C 

4.#Highlights#of#data#products:#NIRS3#map#data#(c) (c)#NIR#slope

Figure. (a) The overview image of the Ryugoid, (b) a global map of
thermal inertia acquired through mid-altitude observation by TIR, (c) a
global map of 3 μm absorption depth acquired by NIRS3, (d) Nearinfrared reflectance spectra (normalized) of the potential landing sites
acquired by NIRS3, and (e) reflectance spectra of zones A-C throughthe mid-altitude observation by ONC. (d)#NIR#albedo

References: [1] Tachibana. S. et al. 2014. Geochemical Journal 48, 571-587.

Measuring Shock Stage of Itokawa Regolith Grains by Electron Back-Scattered Diffraction and Synchrotron X-ray
Diffraction
Michael Zolensky1, Takashi Mikouchi2, Kenji Hagiya3, Kazumasa Ohsumi4, James Martinez1, Kenji Hagiya3, Scott Sitzman5,
Yasuko Terada4, Naoto Yagi4, Mutsumi Komatsu6, Hikaru Ozawa3, Yuta Taki3, Yuta Yamatsuta3, Atsushi Takenouchi2, Hikari
Hasegawa2, Haruka Ono2, Kotaro Higashi2, Masaki Takata4, Arashi Hirata3, Ayaka Kurokawa3, Shoki Yamaguchi3.
1
ARES, NASA JSC, Houston, TX (USA); 2School of Science, Univ. of Tokyo (Japan); 3Graduate School of Life Science, Univ. of
Hyogo (Japan); 4Japan Synchrotron Radiation Research Institute (Japan); 5Aerospace Corporation, El Segundo, CA, (USA);
6
SOKENDAI (Japan).
We have been analyzing Itokawa samples in order to definitively establish the degree of shock experienced by theregolith of asteroid Itokawa, and to devise a bridge between shock determinations by standard light optical petrography, crystal
structures as determined by electron and X-ray diffraction techniques [1,2,3,4]. We are making measurements of olivine crystal
structures and using these to elucidate critical regolith impact processes. We use electron back-scattered diffraction (EBSD)
and synchrotron X-ray diffraction (SXRD). We are comparing the Itokawa samples to L and LL chondrite meteorites chosen to
span the shock scale experienced by Itokawa, specifically Chainpur (LL3.4, Shock Stage 1), Semarkona (LL3.00, S2), Kilabo(LL6, S3), NWA100 (L6, S4) and Chelyabinsk (LL5, S4). In SXRD we measure the line broadening of olivine reflections as ameasure of shock stage. In this presentation we concentrate on the EBSD work. We employed JSC’s Supra 55 variable
pressure FEG-SEM and Bruker EBSD system. We are not seeking actual strain values, but rather indirect strain-related
measurements such as extent of intra-grain lattice rotation, and determining whether shock state “standards” (meteorite
samples of accepted shock state, and appropriate small grain size) show strain measurements that may be statisticallydifferentiated, using a sampling of particles (number and size range) typical of asteroid regoliths.
Using our system we determined that a column pressure of 9 Pa and no C-coating on the sample was optimal. We varied
camera exposure time and gain to optimize mapping performance, concluding that 320x240 pattern pixilation, frame averaging
of 3, 15 kV, and low extractor voltage yielded an acceptable balance of hit rate (>90%), speed (11 fps) and map quality using
an exposure time of 30 ms (gain 650). We found that there was no strong effect of step size on Grain Orientation Spread(GOS) and Grain Reference Orientation Deviation angle (GROD-a) distribution; there was some effect on grain average
Kernel Average Misorientation (KAM) (reduced with smaller step size for the same grain), as expected. We monitored GOS,
Maximum Orientation Spread (MOS) and GROD-a differences between whole olivine grains and sub-sampled areas, andfound that there were significant differences between the whole grain dataset and subsets, as well as between subsets, likely
due to sampling-related “noise”. Also, in general (and logically) whole grains exhibit greater degrees of cumulative lattice
rotation. Sampling size affects the apparent strain character of the grain, at least as measured by GOS, MOS and GROD-a.
There were differences in the distribution frequencies of GOS and MOS between shock stages, and in plots of MOS and GOS
vs. grain diameter. These results are generally consistent with those reported this year [5]. However, it is unknown whether thedifferences between samples of different shock states exceeds the clustering of these values to the extent that shock stage
determinations can still be made with confidence. We are investigating this by examination of meteorites with higher shockstage 4 to 5.
Our research will improve our understanding of how small, primitive solar system bodies formed and evolved, andimprove understanding of the processes that determine the history and future of habitability of environments on other solar
system bodies. The results will directly enrich the ongoing asteroid and comet exploration missions by NASA and JAXA, andbroaden our understanding of the origin and evolution of small bodies in the early solar system, and elucidate the nature ofasteroid and comet regolith.
References: [1] Zolensky et al. (2012) Lunar and Planetary Science, XLIII, #1477, Lunar Planet. Inst., Houston (CD-ROM);[2] Zolensky et al. (2014) Hayabusa 2014: 2nd Symposium of Solar System Materials. Abstracts.; [3] Zolensky et al. (2016)
Hayabusa 2016 Abstracts; [4] Hagiya et al. (2016) Abstracts, 79th Annual Meeting of the Meteoritical Society; Ruzicka andHugo (2017) 80th Annual Meeting of the Meteoritical Society, 6368.

Transmission Electron Microscopy of Plagioclase-Rich Itokawa Grains: Space Weathering Effects
and Solar Flare Track Exposure Ages.
Lindsay P. Keller1 and Eve L. Berger2
1
ARES, Code XI3, NASA/JSC, Houston, TX 77058
2
GCS – Jacobs JETS – NASA/JSC, Houston, TX 77058.
Introduction
Limited samples are available for the study of space weathering effects on airless bodies. The grains returned by the Hayabusa
mission to asteroid 25143 Itokawa provide the only samples currently available to study space weathering of ordinarychondrite regolith. We have previously studied olivine-rich Itokawa grains and documented their surface alteration andexposure ages based on the observed density of solar flare particle tracks. Here we focus on the rarer Itokawa plagioclase
grains, in order to allow comparisons between Itokawa and lunar soil plagioclase grains for which an extensive data set exists[1].
Samples and Methods
Four plagioclase-bearing grains from the JAXA collection were allocated for this study: RB-QD04-0058, RB-QD04-0074, RBQD04-0090, and RA-QD02-0157. We embedded the particles in low viscosity epoxy and used an ultramicrotome to partly
section three of the particles, placing the sections on TEM grids with continuous amorphous carbon support films. Sectioningof the fourth particle is underway. For two of the particles, the epoxy surrounding the particle was trimmed away on three sides
to enable further sectioning utilizing a focused ion beam (FIB) instrument [2] (FEI Quanta 3D). The microtome and FIB
sections were analyzed in a JEOL 2500SE scanning and transmission electron microscope (STEM) equipped with an energydispersive x-ray (EDX) spectrometer optimized for nanometer-scale quantitative x-ray mapping. Brightfield and darkfield
images were acquired using both conventional TEM and STEM imaging. Solar flare particle tracks were imaged in STEM
mode, and observed track densities were converted to apparent surface exposure ages using our recent calibration [3].
Results and Discussion
RB-QD04-0090 is an angular ~40 m grain of twinned albitic plagioclase. No shock features are observed. EDX analyses givea composition of Ab85Or5An12. Solar flare particle tracks occur with a density of ~5x109 cm-2 which indicates a surface
exposure of ~110,000 y (Figure 2). The particle is surrounded by a thin continuous amorphous rim ~50 nm wide.
Quantitative EDX mapping shows that the rim consists of two layers, an inner amorphous layer ~20 nm thick with the same
composition as the underlying crystal-line host, and an outer amorphous layer ~30 nm thick that is Fe-rich and compositionallydistinct from the underlying layer and host grain (Figure 1). We interpret the inner layer as a solar wind amorphized layer, andthe outer layer as a vapor deposit. Vapor deposits of this thickness are unusual for Itokawa grains, because most grains are
typically dominated by solar wind damage [1, 3, 4]. Nanophase Fe grains are present as a thin outermost layer. A few adhering
grains (also plagioclase) are attached to the grain surface. In addition, there are numerous ~0.1-0.3 μm crystals of NaCl on thegrain surface. We also observed a thin continuous rim of NaCl surrounding the grain.
RB-QD04-0074 is an ~32 m irregularly-shaped polymineralic grain. The grain contains major olivine (Fo65), twinned albite(Ab85Or2An12), and minor orthopyroxene (En65Fs33Wo2). The olivine and orthopyroxene are more Fe-rich than typical
Itokawa grains [5] but consistent with literature data for LL chondrites [6]. The orthopyroxene contains a high density ofstacking faults and the olivine contains numerous planar dislocations along (100). The planar dislocations in the olivine grain
are consistent with those that develop due to moderate shock. The observed track density 6x107 cm-2 (corresponding tocounting 6 tracks in 10 m2) is very low and is approaching the limit that can be reliably counted in a grain this large by TEM
methods. The track density implies a short surface exposure of ~2000 y. The plagioclase shows a solar wind amorphized outerlayer ~10 nm wide. The olivine grain appears undamaged and does not show a nanocrystalline solar wind damaged rim likethose on olivine-rich Itokawa grains [7]. RB-QD04-0074 is over an order of magnitude younger than the other olivine andplagioclase grains we have analyzed and was either freshly excavated from greater depth in the Itokawa regolith, or possibly
had an origin as a relatively fresh fragment of a larger grain due to regolith gardening. This grain also shows surface adhering
NaCl particles. We had not previously detected NaCl particles on previous Hayabusa samples analyzed in our lab. Noguchi etal. [8] detected NaCl and KCl particles on Itokawa grains but were unable to determine whether they were indigenous or
possible contaminants.

RA-QD02-0157 is an angular ~38 m grain dominated by albitic plagioclase and minor FeS and olivine. FIB sectioning isunderway and here we report preliminary observations from ultramicrotome thin sections. The plagioclase shows twinning andis compositionally similar to the other albite grains in this study. We have not observed solar flare tracks in this particle to date,although there appears to be a thin amorphous layer (<10 nm) that likely represents solar wind damage. Analysis of a FIB
section will provide a better constraint on exposure age of this grain. A small FeS grain adhering to the surface shows adamaged, outer layer consistent with our previous work on solar wind damaged sulfide grains in Itokawa samples.
Comparison to Lunar Plagioclase
We have previously established a relationship between the width of solar wind damaged rims on lunar plagioclase and olivine,
and their surface exposure age based on solar flare particle track densities [1]. Although large compositional differences exist
between the albitic Itokawa plagioclase grains and the dominantly Ca-rich plagioclase in lunar soils, the solar wind damaged
rim widths in Itokawa grains follows the trend for lunar plagioclase. The Itokawa grains show space weathering features
typical of immature lunar soil grains.
Conclusions
We analyzed the space weathering features on three Itokawa plagioclase-bearing grains. Particles RA-QD04-0074 and RAQD02-0157 are relatively fresh with little surface modification from solar wind damage. The low track density for -0074
suggests a surface exposure age of ~2000y. Particle RA-QD04-0090 has a much longer surface exposure (~110,000 y) andcorresponding surface alteration including a 30 nm thick vapor deposit overlying a solar wind damaged layer.
References[1] Keller, L. P. et al. (2016) LPSC 47, #2525. [2] Berger, E. L. & Keller, L. P. (2015) Microscopy Today 23, 18-23. [3]Berger, E. L. & Keller, L. P. (2015) LPSC 46, #2351. [4] Noguchi, T. et al. (2014) MAPS 49, 188. [5] Nakamura, T., et al.
Science 333, 1113-1116. [6] Nakamura, T., et al. LPSC XXXXII, 1766. [7] Keller, L. P. & Berger, E. L. Earth, Planets andSpace 66, 71-77. [8] Noguchi, T., et al. (2014) MAPS 49, 1305-1314.
Acknowledgement
We thank JAXA for allocating the particles analyzed in this study. This work was supported by a NASA LARS grant (LPK).

Figure 1. A brightfield STEM image from a FIB section of particle RA-QD04-0090 showing
twinning in the host grain, solar flare particle tracks (red arrows), and a space-weathered rim
consisting of two distinct layers, a vapor-deposited layer (1) and a solar wind damaged layer(2).

Microstructures of iron sulfide of Itokawa particles
1

T. Matsumoto1, A. Miyake3, S. Nakao2, A. Tsuchiyama3, M. Sakai2
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), 2Institute of Molecular Science,
3
Kyoto University(E-mail: tmatsumoto@planeta.sci.isas.jaxa.jp).

Introduction:
Space weathering has been referred to describe the collective processes that modify the optical properties, chemicalcompositions, and structures of materials on the surfaces of airless Solar System bodies [1]. Hayabusa spacecraft touched down
to a S-type near-Earth asteroid 25143 Itokawa and recovered surface regolith particles, which are consistent with minerals
contained in LL5-6 ordinary chondrite [2]. Analysis of Itokawa particles revealed nanoparticle-bearing rim, which are probably
the major cause of alteration of reflectance spectra of Itokawa [3]. Prior to Hayabusa mission, the Near-Earth Asteroid
Rendezvous (NEAR) mission’s orbital study of S-type asteroid Eros revealed that change of reflectance spectra has beendeveloping on Eros’s surface similar to Itokawa’s surface [4]. NEAR also discovered that Eros’s surface appears to be strongly
depleted in sulfur compared to ordinary chondrite [4]. However, sulfur depletion has not been obvious on Itokawa from remotesensing observation and sample analysis so far. Sulfur in Itokawa samples is primarily bound in the form of iron sulfide [1], we
investigated microstructures of iron sulfide of Itokawa particles in order to understand behavior of sulfur on airless bodies.
Experiments:
The four Itokawa particles were fixed with a 5 µm-diameter carbon fiber using glycol phthalate. The surface morphologiesof the Itokawa particles were observed using a field-emission scanning electron microscope (Hitachi, SU6600) equipped withan energy-dispersive X-ray (EDX) spectroscopic detector (Bluker XFlash FladQUAD 5060FQ) at the Institute of Molecular
Science, Japan. Regions of interest (ROI) were selected based on the FE-SEM observation, and electron-transparent sections
including particle surface were prepared from the ROI using a focused ion beam (FEI, Helios G3 CX) at Kyoto University, Japan.
The sections were observed using a field-emission transmission electron microscope (JEOL, JEM-2100F) equipped with an EDX
system (JED-2300T) at Kyoto University.
Results:
Iron sulfides are visible as inclusions of olivine grains, adhered particles, and melt-splashes on the Itokawa particles. Fromsurface observation using FE-SEM, we found needle-like structures protruding from the iron sulfide surfaces (Fig.1ab). The
lengths of the needles range from several tenth nm to 1 µm. The needles often develop on porous iron sulfide surfaces (Fig.1ab).
SEM-EDX analysis shows that the needles are composed of iron and they are deficient in sulfur (Fig.1c). The needles often
contain minor nickel. So far, we lifted out FIB sections from a melt-splash of iron sulfide where needle-like structures develop
on its surface. The melt-splash is an immiscible mixture of silicate and iron sulfide, covering an olivine grain. Fig. 1 shows across section of the melt splash of 50 nm in thickness including the needles. Elemental maps by TEM-EDX analysis clearlyshows that the needle consists of iron and lacks in sulfur (Fig.1d). A TEM-selected area electron diffraction (SAED) pattern ofthe needle (Fig. 1f) indicates that the needle has a structure of body-centered cubic iron (α-iron). The iron sulfide layer iscomposed of amorphous structures, expect for regions nearby the iron needle. Crystalline pyrrhotite structure is developed in thevicinity of the iron needle. Beneath the iron sulfide layer, vesicular damage rims are developed on olivine surface, which might
have been formed due to the implantation of solar wind hydrogen and helium [3]. The existence of vesicular rim indicates that
olivine surface has been exposed to the sun over a period of time, before the melt splash attached to the olivine surface.
Discussions:Remarkable surface morphology of iron sulfide such as iron needles have not been reported in previous analysis of Itokawa
particles. On the other hand, prior observation of pyrrhotite grain of Itokawa particles reported that the outer 10-nm-wide zone
is sulfur-depleted, including metallic iron grains (<5 nm) [5]. Mineral surfaces exposed to the space environment can be modified
through space weathering by solar wind irradiation and impacts of micrometeorites. In previous studies, the feasibility ofalteration of iron sulfide by space weathering effects have been examined experimentally [6, 7]. Laboratory studies on thechemical alteration of troilite by 4keV He ions simulating exposure to the solar wind and by nanosecond laser pulses simulating
evaporation by micrometeorite impact showed that sulfur is depleted from troilite by these both effects [6] and iron layer of 2-3
nm in thick is identified after He ion implantation [7]. However, these experiments have not produced metallic iron needles as
observed in this study. Prior experiments of heating troilite at near its eutectic temperature under H2 gas flow showed that sulfur
evaporates from troilite and iron residue is formed through incongruent evaporation [8]. This experiment showed that iron exists
as irregular rods or sheet of micron meter in size. This could suggest that heating events such as meteoroid impacts together withimplantation of solar wind hydrogen cause metallic iron needles on iron sulfide of Itokawa particles.
These heating events and ion implantation may lead to preferential loss of sulfur from Itokawa. X-ray fluorescenceobservations of Itokawa by the Hayabusa spacecraft did not find evidence for a large sulfur depletion on this S-class asteroid, as
seen on Eros, though errors are large due to low solar activity during the orbital phases of the Hayabusa mission [9]. The
microstructures of iron sulfide observed in this study could suggest that sulfur depletion processes are ongoing on Itokawa.
References:[1] Pieters. et al. 2000. MAPS, 35, 1101-1107 [2] Nakamura et al. (2011) Science, 333, 1113-1116. [3] Noguchi et al. (2014)
MAPS, 49, 188–214. [4] Trombka et al. 2000. Science, 289, 2101-2105. [5] Keller and Berger. 2014. EPS, 66:71. [6] Loeffer etal. 2008. Icarus, 195, 622-629. [7] Keller et al. 2010. LPSC Abstract#1172. [8] Tachibana and Tsuchiyama. 1998. GCA, 62,
2005-2022. [9] Arai et al. 2008. EPS 60:21-31.
Figure 1 (a) (b) Secondary electron images of iron sulfide.
Needle-like structures are indicated by arrows. (c) A SEMEDX image of iron sulfide grains on olivine surfaces. (d)STEM-EDX images of a cross section of splash melt on
olivine particle. A needle-like structure is indicated byarrows. (e) A TEM image and A SAED pattern of a needlelike structure.

FTIR Micro-tomography of five Itokawa Particles
Dionnet Z.1, Aléon-Toppani A.1, Borondics F.2, Brunetto R.1, Buellet A.C.1, Djouadi Z.1 , King A.3 and Rubino S.1
1
Institut d’Astrophysique Spatiale, CNRS, Université Paris-Saclay, CNRS
2SMIS beamline, Synchrotron SOLEIL, France
3
PSICHE beamline, Synchrotron SOLEIL, France

Primitive extra-terrestrial materials (asteroidal and cometary particles, meteorites, IDPs) are characterized by a large
mineralogical and compositional heterogeneity at different scales (from nm to mm) [1], which witnesses the complexity of the
pre-accretional (solar nebula) and post-accretional (parent bodies) processes undergone by the small bodies of our solar system[2]. This heterogeneity has been observed by different techniques such as infrared (IR) micro spectroscopy mapping which is a
powerful tool as it is (a) non-destructive and allows (b) comparison with astronomical observations of primitive Solar Systemsmall bodies (asteroids, comets, TNOs) [3] and (c) access both to the mineral and carbonaceous phases.
Thanks to Focal Plane Array (FPA) detector, 3D hyperspectral micro-tomography, can be performed to accessstructural information on intact samples [4, 5]. So far, this technique has never been applied to Hayabusa-1. Here, we will
present the first 3D infrared reconstruction of five particles of Itokawa (RA-QD02-0214, RA-QD02-0223, RA-QD02-0232,
RA-QD02-0156 and RB-QD04-0046). The FTIR micro analyses are performed at the SMIS beamline of the Synchrotron
SOLEIL using a FPA detector with its Globar intern source. It is complementary to the X-ray micro-tomography previously
performed on Hayabusa-1 particles [6]. Novel numerical methods have been developed to deal with a huge quantity ofhyperspectral infrared data and we were able to obtain the 3D spatial distribution of chemical/mineralogical components(low/high calcium pyroxene, olivine, and plagioclase).
Another analysis was performed on grains of the Paris meteorite, one of the most primitive carbonaceous chondrite[7], to study the spatial correlation between the organic and mineral phases at scales down to ~3 μm. X-rays tomography was
also performed on the same Paris particles, at the PSICHE beamline of the synchrotron SOLEIL, to obtain complementary
information about the physical properties of the grains (shape, fractures, porosity …). By combining X-ray and FTIR data we
could obtain a physico-chemical description of precious grains in a non-destructive way and thus gives information about theformation and evolution of asteroids.
Performing FTIR micro-tomography on extraterrestrial samples rich in organic matter, is an important step in view ofthe sample return of dust particles from carbonaceous asteroid Ryugu by the Hayabusa-2 mission. In the sequence of analyses,
micro-FTIR 3D spectral imaging coupled with X-rays tomography can provide a first, powerful non-destructive
characterization of whole grains, in order to identify areas of interest and provide useful information before subsequent
destructive analyses.

Acknowledgments
We are grateful to T.Yada and T.Nakamura for help and useful discussion. The micro-spectroscopy activities are supported by
grants from Région Ile-de-France (DIM-ACAV) and SOLEIL.

References[1] Rietmeijer, F.J.M. 1998. Reviews in Mineralogy, 36, 95pp. (Chapter 2). [2] Alexander, C.M.O’D. 2007. Geochimica et
Cosmochimica Acta, 71, Issue 17, p. 4380-4403. [3] Brunetto et al. 2011. Icarus 212, 896–910. [4] M.J. Nasse et al. 2011.
Nature method 8, 1585. [5] M.C. Martin et al. 2013. Nature Methods, 10, 861–864. [6] Tsuchiyama A. et al. 2011. Science
333, 1125. [7] R. Hewins et al. 2014. Geochimica et Cosmochimica acta 124, 190-222.

Asteroid 25143 Itokawa Dust Particles:
Mineralogy and Chondrite Affinities
Suporn Boonsue and John G. Spray
Planetary and Space Science Centre, University of New Brunswick, NB, E3B 5A3, Canada
In the third international announcement of opportunity (AO3) for Hayabusa mission sample investigation, we received three dust
particle samples. Two specimens are polished sections of post-analyzed particles embedded in resin: RA-QD02-0011-02 (~30 μm)
and RA-QD02-0048 (~20 μm) with Au- and C-coatings, respectively (Figure 1). The third sample is a pristine particle, RB-CV-0083(~95 μm). Particle RA-QD02-0011-02 was originally described to be mainly composed of olivine, low-Ca pyroxene, high-Ca
pyroxene, and plagioclase [1-4]. In this study, the morphology and composition of the particles were inspected by means of (1) fieldemission scanning electron microscopy (FESEM), and associated energy-dispersive X-ray microanalysis (EDS) and electron backscattered diffraction (EBSD) using an Hitachi SU-70 with Schottky type field emission gun, and (2) micro-Raman spectrometry at
the Planetary and Space Science Centre (PASSC), University of New Brunswick, Canada.

Figure 1. The three assigned Itokawa dust particles RA-QD02-0011-02 (~30 μm), RA-QD02-0048 (~20 μm), and RB-CV-0083 (~94 μm) provided
by the Japan Aerospace Exploration Agency (JAXA) Hayabusa asteroidal sample return mission for this study.

The particles were collected from the surface of the S-type asteroid 25143 Itokawa. The particles comprise olivine, pyroxene andplagioclase. Fe-Ni metal, troilite (FeS), and chromite are also present. Energy dispersive spectrometry reveals that the olivine is Fo70,
and the plagioclase is (Ab81An13Or6). The plagioclase is interstitial to the olivine. The EBSD pattern of the (Mg,Fe)SiO4 phase in
RA-QD02-0011-02 matches well with the pattern of the orthorhombic crystal structure of forsterite with space group Pbmn. The unit
cell dimensions are a = 4.76 Å, b = 10.21 Å, c = 5.98 Å, α = 90.0o, β = 90.0o,  = 90.0o (Figure 2a). Raman analysis of the olivine
reveals high intensity Raman bands at 819 and 851 cm-1, with a Raman band calculated Fo number of 70 (Figure 3a). In addition, the(Na,K,Ca)(AlSi)4O8 phase next to olivine yields a typical EBSD pattern of amorphous material (Figure 2b). Raman analysis of theplagioclase reveals a broad band of amorphous material with an intense Raman band of crystalline phase albite/oligoclase. Both
EBSD and the Raman results suggest that plagioclase was partially transformed to maskelynite (feldspathic glass). Intense Raman
bands at 678, 659, 334 and 1006 cm-1 of orthopyroxene were obtained from RB-CV-0083. A cluster of forsterite (Fo68.7), augite andplagioclase (Na0.81Ca0.12K0.06(Al,Si)4O8) present at the rim of the particle. A microcrystal (~5 um diameter) of rounded, unzoned
forsterite (Fo69.5) with a nano-lath of albite/oligoclase (~1.0 m x 500 nm) occurs in dust particle RB-CV-0083. The Mg/(Mg+Fe+Ca)
ratio in pyroxene based on Raman band recalculation (678 and 334 cm-1) is 0.7 (En70) (Figure 3b), which is in good agreement with
the EDS results (Wo3En73Fs24). The olivine and orthopyroxene compositions are consistent with those of an LL4-6 chondrite. The
presence of maskelynite suggests that the particles experienced shock metamorphism. The compositional homogeneity of olivine
and the development of plagioclase indicate that the petrologic type of Itokawa dust particles is derived from a highly equilibratedchondrite. Our study confirms that the analyzed Itokawa dust particles are from a shocked equilibrated LL4-6 chondrite that now
forms part of the asteroid’s regolith. The source of the dust particles remains conjectural in that they could be from fragmented
projectiles that impacted Itokawa, or from excavated material from within Itokawa, which itself is probably an assemblage of multiple
asteroid components. The presence of maskelynite strongly suggests that the asteroid experienced shock impact during its evolution.

(a)

(b)
Figure 2. (a) The EBSD pattern of the (Mg,Fe)SiO4 phase in RA-QD02-0011-02 matches well with the pattern of the orthorhombic crystal structureof forsterite (Pbmn) with unit cell dimensions a = 4.76 Å, b = 10.21 Å, c = 5.98 Å, α = 90.0o, β = 90.0o,  = 90.0o. (b) Electron backscattered diffraction
patterns (EBSD) of (Na,K, Ca)AlSi3O8 phases shows an amorphous EBSD diffraction pattern in the absence of Kikuchi bands.

(a)

(b)

Figure 3. (a) The Raman peak positions at 851 and 819-820 cm-1 of olivine in Itokawa sample RA-QD02-0011-02 (red dots) are plotted on a diagramof peak positions of its charcteristic Raman modes of olivine [5]. The data points fall along the calibration line suggesting the Mg/(Mg+Fe) value
for the Itokawa olivine ~0.7 (Fo65-70). (b) The data for a pair of peak positions of characteristic Raman modes (678 and 334 cm-1) for orthopyroxenefrom RB-CV-0083 are plotted on the curve (pink dots), which corresponds to Mg/(Mg+Fe+Ca) molar fraction in pyroxene values of 0.7 (En70) [6].

References[1] Yurimoto et al. 2011. Science. 333, 1116-1119. [2] Nakamura et al. 2011. Science 333, 1113-1116. [3] Tsuchiyama et al. 2011.
Science. 333, 1125-1128. [4] Yada et al. 2012. Japan Aerospace Exploration Agency, Japan, unpublished document. [5] Wang et al.,2004. J. Raman Spectrosc. 35, 504-514 [6] Huang et al., 2000. Am. Mineralogist 85, 473-479.

Electrical properties of Itokawa grains returned by Hayabusa
F. Cipriani1, N. Drozdovski1, D. Koschny1, L. Colangeli1, M. Ferrari2,3, V. Della Corte2, M. Accolla2,3, B. Butler1,
A. Rotundi2,3, B.Shortt1,S. Sanders1, D. C.v.d. Luijt1, D. Breeveld, 1 ESA/ESTEC, Keplerlaan 1, 2200AG,
Noordwijk, The Netherlands E-mail : fabrice.cipriani@esa.int 2 INAF-Istituto di Astrofisica e Planetologia
Spaziali, Via Fosso del Cavaliere 100, 00133 Roma, Italy 3 Dip. Scienze e Tecnologie, Universita degli Studi diNapoli “Parthenope”, Centro Direzionale I C4, 80143 Napoli, Italy
Although a wealth of data exists on the properties of lunar regolith samples returned by Apollo missions e.g. [1,2] aswell as investigations on terrestrial minerals, no such experimental data have yet been collected on asteroids material. In thisstudy we present the measured secondary electron emission characteristics from areas of samples RA-QD02-0126-02 and RAQD02-0136-14 [3] under electronic irradiation whithin the range 200eV to 5keV. Such measurements are related to surface
structure, orientation and mineralogy, and compared to reference measurements including single grains and powders of reference materials of high purity, as well as terrestrial minerals and planetary analogs (see exemple Figure 1). In addition we observe the build-up of local electric field patterns arising from surface electrostatic charging in relation with grains morpholgoy.
Consequences on our understanding of regolith properties and electrostatic effects on planetary regolith will be discussed.

Figure 1: Secondary emission yields measured from Fosterite grains

References:[1] B. Feuerbacher et al , Proceedings of the Third Lunar Science Conference, 1972: Vol. 3, pp. 2655-2663[2] D.W. Strangway et al, Earth and Planetary Science Letters, 1972, Volume 16, Issue 2, pages 275-281,[3] Nakamura et al. , 2014, Meteorit Planet Sci, 49: 215–227. 10.1111/maps.12247

Particle track densities in olivine of the heated Jbilet Winselwan CM2 chondrite: Constraints onregolith heating?
Dennis Harries1 and Philip Wild1
Institute of Geosciences, Friedrich Schiller University Jena, Carl-Zeiss-Promenade 10, 07745 Jena, Germany (Email:dennis.harries@uni-jena.de).

1

Sample-return missions underway to the near-Earth objects 101955 Bennu (OSIRIS-REx) and 162173 Ryugu (Hayabusa 2) are
expected to return surface regolith from two primitive C-group asteroids for laboratory study. Spectroscopically the C-group
asteroids share similarities with CI and CM chondrites and are likely parent bodies of these meteorite groups. Material returned
from the Moon and S-type asteroid 25143 Itokawa has shown that phenomena related to space weathering are well-recorded on
the surface of silicate grains [1]. The degree (or maturity) of space weathering can potentially provide insights into theevolution of regoliths and, therefore, shed light on the dynamical evolution of near-Earth asteroids and their orbits [2,3,4].
Olivine is a good candidate for comparative taxonomy of space weathering due to its wide-spread occurrence in lunar andasteroidal samples and its experimentally extensively studied properties. If C-group asteroids are indeed related to CI and CM
chondrites, olivine is expected to be a significant mineral in their regoliths. However, aqueous and thermal alteration processes
recorded in CI and CM chondrites potentially leave morphological and chemical signatures on mineral surfaces, onto whichspace weathering would be superposed. This motivated us to investigate olivine grains of the Jbilet Winselwan (JW) meteorite,a moderately heated (tentatively <500 °C) CM2 chondrite [5]. In particular, we try to understand how olivine grains and thephyllosilicate mineralogy of JW can be used to constrain the heating event, which may have taken place in a number ofdifferent settings, e.g., deep in the CM2 parent body, in the regolith of a rubble-pile asteroid, or during the meteoroid stage of
JW’s travel towards the Earth.
Material and Methods: A 37.6 gram fragment of JW was sliced using a diamond wire saw and interior slices were used to
produce two polished petrographic sections (~20×30 mm2) and cuboidal subsamples (~10×7×7 mm3). The cuboids were
subjected to 100 to 150 cycles of freeze-thaw disaggregation in high-purity water. After drying, olivine crystals were separated
by hand-picking and mounted onto SEM stubs or epoxy-embedded and polished. The grain mounts and polished petrographic
sections were studied by field-emission SEM. The polished grain mounts were etched in WN solution in order to reveal
damage tracks produced by ionizing, high-energy particles [6].
Results and Discussion: SEM imaging of the JW petrographic sections indicates subtle textural heterogeneities, most evident
by variations in the abundance of serpentine/tochilinite-like aggregates. There is no obvious brecciation as seen in other CM2
chondrites [7] and specimens of JW [8]. Many components (dominantly chondrules) are surrounded by fine-grained rims, andthe general texture resembles a primary accretionary rock [7]. The freeze-thaw disaggregated material is a black, non-cohesive
powder (~80% <100 µm, ~50% <50 µm).
Euhedral to subhedral olivine crystals are optically prominent objects in the powder. The hand-picked olivine grains havemedian sizes of ~240 µm and a size range of 100 to 600 µm. Comparison with the petrographic sections suggests that thelarger grains often occur as single grains within the meteorite. The smaller ones are most probably derived from porphyritic
chondrules. The surface morphologies show a large diversity and can be subdivided into ‘as-grown’ crystal surfaces andfractured surfaces. Pristine surfaces are smooth and featureless, fresh fracture surfaces are typically characterized by step-likehackle marks. Altered surfaces have developed significant roughness through dissolution and the formation of secondary
mineral scales. Such features superposed on surfaces with hackle marks suggest that fracturing had occasionally occurred
before aqueous alteration.
We have studied a total of 81 olivine grains from three interior cuboids of JW for particle tracks, and etching has revealed
tracks in 65 of them. In all cases the track densities are <5×104 tracks/cm2 (Fig. 1), and the median is ~9400 tracks/cm2 (~6500
tracks/cm2, if upper limit track densities for track-free grains are considered). The maximum track densities found in two
grains are approximately consistent with the background track densities due to galactic cosmic rays (GCR) in typical CM2chondrites [7]. However, the median values are much lower than typical GCR background track densities. The absence of
brecciation and track-rich grains (>106 tracks/cm2, from irradiation by solar flare ions) indicates that the material of our JW
specimen was never exposed in the upper few millimeters of a regolith. This is corroborated by the absence of solar wind noble
gases in other samples of JW [9]. However, JW’s unusually long Neon exposure age of 6.6±1.7 Ma [9] and the very low GCR
track count suggests that GCR tracks may have been partially annealed by the, so far unidentified, heating event.

Figure 1. Cumulative plot of the particle track densities in Jbilet Winselwan olivines.

If JW was heated deep within its parent body, then GCR tracks and GCR-produced neon should have been acquiredconsistently during the meteoroid stage, unless the meteoroid that delivered JW to Earth was very large, and our specimen was
deeply shielded within. The freshness of most JW specimens and the total known mass of JW meteorites of less than 10 kg(e.g., compared to >100 kg of Murchison) rule this possibility somewhat unlikely. Alternatively, JW may have been heatedduring a regolith residence or its meteoroid stage, e.g., by solar irradiation at low perihelion distances. If indeed solar heating
can be made responsible for the mineralogical changes observed in JW (and possibly other heated CM and CM-like chondrites[10]), the implications for our understanding of space weathering phenomena in returned samples would be large, as heating
and annealing may alter the exposure record of space-weathered grains (e.g., [3]).
References[1] Noguchi T. et al. (2011) Science 333:1121–1125. [2] Conolly H. C. et al. (2015) Earth, Planets and Space 67:12. [3]Harries D. and Langenhorst F. (2014) Earth, Planets and Space 66:163. [4] Harries D. et al. (2016) Earth and Planetary Science
Letters 450:337-345. [5] Nakamura T. et al. (2014) Antarctic Meteorites XXXVII, 54. [6] Krishnaswami S. et al. (1971)
Science 174:287–291. [7] Metzler K. (2004) Meteoritics & Planetary Science, 39:1307–1319. [8] Zolensky M. E. et al. (2016)
47th Lunar and Planetary Science Conference, abstract #2148. [9] Meier M. M. M. et al. (2016) Meteoritics & Planetary
Science 51:A455. [10] Harries D. and Langenhorst F. (2013) Meteoritics & Planetary Science 48:879-903.
Acknowledgements
We acknowledge funding from Friedrich Schiller University Jena (DRM/2016-01). The SEM facility at U Jena is supported by
the DFG (grant LA 830/14-1 to F. Langenhorst).

Carbon isotopic ratios of calcite grains in the LAP 031166 CM chondrite: Implications for possible
link between CM and cometary ices.
Wataru Fujiya1, Kohei Fukuda2, Paula Lindgren3, Martin R. Lee4, Mizuho Koike5, and Yuji Sano5
1
Ibaraki University, 2-1-1 Mito, Bunkyo, Ibaraki 310-8512, JAPAN. (wateru.fujiya.sci@vc.ibaraki.ac.jp),
2
University of Tokyo, 3Lund University, 4University of Glasgow, 5Atmosphere and Ocean Research Institute,
University of Tokyo.
Introduction: Carbonate minerals are ubiquitous in CM chondrites, which formed by aqueous alteration in the CM chondrite
parent body. Previous studies have shown that C isotopic ratios of CM carbonates are highly variable at whole-rock scales aswell as among individual grains in single meteorites [e.g., 1-3]. Despite extensive studies on C isotopic ratios of CM carbonates,
the reason for variability in 13C variation and the origin of the carbonate C remain poorly understood.
Here we report C isotopic ratios of calcite (CaCO3) in the LAP 031166 CM chondrite (CM 2.1), and discuss the origin of the
carbonate C and a possible link between ices in CMs and in comets. The O isotopic ratios of calcite in this meteorite werereported by Lindgren et al. [4].
Experimental: Carbon-isotope analysis was performed with the NanoSIMS 50 installed at Atmosphere and Ocean ResearchInstitute, the University of Tokyo, on the calcite grains whose O isotopic ratios were measured previously. Negative secondary
ions of 12C-, 13C-, 18O-, 12C14N-, and 28Si- produced by rastering a Cs+ primary ion beam (20-30 pA, ~1 m in diameter) over 6 x
6 m2 sized areas were detected simultaneously with five electron multipliers.
Results and discussion: The 13CPDB and 18OSMOW values of the calcite grains in LAP 031166 are shown in Fig. 1, together
with literature data of Ca-carbonate (calcite and aragonite) in the Murchison, Nogoya, and Paris CM chondrites [3,5,6]. The 13C
and 18O values of the CM carbonates are highly variable, ranging from ~20 to 80‰ and from ~15 to 40‰, respectively, andthey do not correlate with each other.
Alexander et al. [1] have suggested that the range in 13C can be explained by variable formation temperatures (0-130 oC) of CM
carbonates which are isotopically equilibrated with gaseous C species dominated by CO (or CH4). However, this model implies
that the 13C and 18O values of the CM carbonates would correlate, which is clearly not the case as demonstrated by this work
(Fig. 1). Instead, the observed 13C range must be produced under nearly constant temperatures.
Here we propose a modified version of the model outlined by Alexander et al. [1], where we consider mixing of CO2 and CO
gases with higher and lower 13C values, respectively. Because the equilibrium CO/CO2 ratios are <<1 for fO2 higher than theiron-magnetite buffer, CO should be converted to CO2 and the CO/CO2 ratios of gas phases would have decreased with time. As
the CO/CO2 ratios decreased, CO2 as well as carbonates acquired lower 13C values. Given 1000ln(calcite-CO2) of ~10-14 at
0-30 oC [7], where  is a C isotopic fractionation factor, the CM carbonates with the highest 13C values of ~80‰ were
equilibrated with CO2 with 13C ~ 70‰. The 13C value of the trapped CO in Murchison is ~-30‰ [8]. The lowest 13C valuesof the CM carbonates are ~20-30‰, which is common for all the CM chondrites analyzed (Fig. 1). Therefore, the gaseous C
species which coexisted with the CM carbonates with the lowest 13C values of ~20-30‰ would have been dominated by CO2,
i.e., most of CO was converted to CO2. If correct, the 13C value of the bulk gaseous C species (CO2 + CO) would be ~10‰.
Using the above numbers, mass balance calculation suggests that a CO/CO2 mole ratio of the gaseous C species which coexistedwith the CM carbonates with the highest 13C value of ~80‰ would be ~1.5, which may reflect the CO/CO2 ratio of ice accreted
onto the CM parent body. The carbonate C/H2O mole ratios of most CMs range from ~0.01 to 0.1 [1]. These carbonate C/H2O
ratios may set lower limits on the CO2/H2O ratio of the CM ices because of possible CO2 loss. Thus, CO2 accounts for at least
1 % of the CM ices.
The inferred CO/CO2 and CO2/H2O mole ratios of the CM ices are shown in Fig. 2, together with those of cometary ices [9].
Unfortunately, only upper limits on the CO/CO2 ratios are obtained for most of the observed comets. Nevertheless, the CO/CO2
ratios of these comets seem lower than unity, and thus, lower than those of the CM ices. Although the possible similarity between
ices in CMs and in some comets cannot be ruled out, these observations suggest that ices in the two classes of bodies had adifferent origin, which is consistent with contrasts in the D/H ratios of water between CMs and comets [10].
References: [1] Alexander C. M. O’D. et al. 2015. Meteorit. Planet. Sci. 50:810. [2] Tyra M. A. et al. 2012. Geochim.
Cosmochim. Acta 77:383. [3] Fujiya W. et al. 2015. Geochim. Cosmochim. Acta 161:101. [4] Lindgren P. et al. 2017. Geochim.
Cosmochim. Acta 204:240. [5] Fujiya W. et al. 2016. Abstract #1712. 47th LPSC. [6] Vacher L. G. et al. 2017. Geochim.
Cosmochim. Acta 213:271. [7] Chacko T. et al. 2001. Rev. Mineral. Geochem. 43.1. [8] Yuen G. et al. 1984. Nature 307:252.
[9] Ootsubo T. et al. 2012. Astrophys. J. 752:15. [10] Alexander C. M. O’D. et al. 2012. Science 337:721

Fig. 1. 13C and 18O values of Ca-carbonates in CM
chondrites. Errors are 2.

Fig. 2. CO/CO2 and CO2/H2O mole ratios of theinferred CM ices and comets. Data with arrows
represent upper limits. JFCs: Jupiter-family comets,
OCs: Oort cloud comets. Only comets which wereobserved within 2.5 AU from the Sun are shown,
where H2O effectively sublimes from the nucleus of
the comet.

Volatile Contents in Vesicles in IDP Grains Analyzed with Scanning Transmission Electron
Microscopy
Katherine D. Burgess1, Rhonda M. Stroud1, David Joswiack2 and Donald Brownlee2
1
U.S. Naval Research Laboratory, Washington, DC
2
University of Washington, Seattle, WA
Chondritic porous interplanetary dust particles (IDPs) are believed to come from comets and incorporate a wide variety ofprimitive early solar system and interstellar materials. Alteration is thought to be from nebular processes, such as solar windexposure, and atmospheric entry heating. The compositional and structural changes associated with these processes can beanalyzed using (scanning) transmission electron microscopy (S/TEM) with energy dispersive X-ray spectroscopy (EDS) andelectron energy loss spectroscopy (EELS). Vesicles formed in the space weathered rims of grains are thought to be filled withhydrogen or helium from the solar wind, although heating may be required for the formation of the vesicles. Solar wind hydrogenhas been identified in vesicles in the space weathered rim of a pyroxene grain [1], while helium was suggested as the likely
source of bubbles formed in a pyrrhotite grain [2].
Stratospheric IDPs from collection plate U2012, flown on NASA Ames Research Center U2 aircraft in March 1993, were washedand embedded in epoxy, then microtomed and placed on grids for STEM analysis. The samples were baked at 140°C for six
hours to drive off adsorbed water before insertion in the UHV system. Electron energy loss spectroscopy (EELS) and energy
dispersive x-ray spectroscopy (EDS) data were collected with the NION UltraSTEM200-X at the U.S. Naval ResearchLaboratory, equipped with a Gatan Enfinium ER EEL spectrometer and a Bruker SSD-EDS detector. The STEM was operated
at 60 kV or 200 kV, with a ~0.1 nm probe. Spectra were collected as spectrum images (SI), with a spectrum collected for eachpixel, allowing for mapping of variations in thickness and composition.
Sample U2012A-2J contains a pyrrhotite grain with a nominally continuous space weathered rim full of subhedral to euhedral
vesicles. The voids range in size from a few nanometers to ~30 nm. Brownlee et al. [2] suggested that these voids formed due tohelium implantation, but were unable to confirm the presence of helium in specific voids. High resolution EELS mapping ofseveral of the voids reveals a small peak at ~22 eV associated with individual voids, indicating they are filled with helium fromthe solar wind (Figure 1).
A vesicular grain observed in sample U2012A-3C is much more enigmatic (Figure 2). The core of the grain is iron sulfide andit is surrounded by a highly vesicular oxygen-rich shell. EDS data show the rim material contains significant O, Fe and S, alongwith several at% Mg and trace (~0.5 at%) Si. EELS data from the vesicles show small peaks at 8.5 eV and ~13 eV, both associatedwith hydrogen [1]. Additionally, the carbon K-edge in spectra from the same vesicles shows a distinct peak at 287.4 eV due tothe presence of C-H bonds. Attribution of this peak to a specific compound is ambiguous due to the ubiquity of these types ofbonds in natural materials as well as laboratory sources. The peak is associated only with this particle and clearly tied to theindividual vesicles, suggesting it is indigenous. A sharp peak at the same energy is seen in hexamethyl disiloxane [3], a compound
related to the silicone oil in which the IDPs were collected, and hexane [4], used to wash the IDPs, both possible sources ofcontamination. However, the vesicles are not correlated with significant Si, as expected for silicone oil, and evidence ofcontamination is not seen elsewhere on the sample. Isotope measurements of the grain are planned in order to clarify the possible
sources of the rim material and hydrocarbons.
The helium- and hydrogen-filled bubbles have very different morphologies, and it is unlikely the hydrogen filled vesicles formed
solely due to the influence of the solar wind. The cores of both grains are predominantly iron sulfide. However, while the helium
vesicles are euhedral and in material that otherwise very closely resembles vesicle-free portions of the grain, the hydrogenvesicles are in a highly porous rim that is rich in oxygen relative to the core of the grain and also has other minor and traceelements (e.g., Mg, Si) not present in the core. Solar wind helium-filled vesicles in lunar ilmenite are not euhedral [5], indicatingthat both host mineral composition and heating could play a role in vesicle formation and shape.
With the ability to identify and map the volatile contents of very small vesicles in IDPs and other extraterrestrial materials, we
can better understand the timing of alteration and source of volatiles, whether from atmospheric heating and decomposition ofpyllosilicates, implantation by the solar wind, or contamination during collection and laboratory preparation procedures. This
technique is applicable to samples collected from many airless bodies including Itokawa, Bennu, and Ryugu.

cbaFigure 1. (a) HAADF image of pyrrhotite from U2012A-2J showing vesicle-rich rim around particle. (b) Higher magnification image ofseveral euhedral vesicles. (c) EELS data from two vesicles indicated in (b) showing small peaks at ~22 eV indicating helium is present in
the vesicles. A spectrum from a portion of the pyrrhotite not in a vesicle is shown for comparison (black).

a

b

c

d
H-K

C-K

Figure 2. (a) HAADF image of particle in U2012A-3C with a vesicular rim. (b) Window map of 8.5 eV peak from region outlined bygreen box in (a). (c) Low loss spectra from the bright vesicle highlighted in (b) (blue) and surrounding material (gray) showing peaks at~8.5 eV and ~13 eV, indicating the presence of hydrogen in the vesicles. (d) Carbon K-edge spectrum showing a large peak at 287.4 eV
spatially associated with H-filled vesicles. The peak is indicative of C-H bonds. Amorphous carbon spectrum from the grid substrate(gray) is shown for comparison.

References[1] Bradley, J.P., et al. (2014) PNAS, 111, 1732. [2] Brownlee, D., et al. (1998) LPSC, 29, Abstract #1869. [3] Urquhart, S.G.,
et al. (1997) Organometallics, 16, 2080. [4] Hitchcock, A.P., and I. Ishii (1987) Journal of Electron Spectroscopy and Related
Phenomena, 42, 11. [5] Burgess, K. and R. Stroud (2017) LPSC, 48, Abstract # 1076.

Simulating Space Weathering of a Carbonaceous Chondrite via Pulsed Laser Irradiation
Michelle Thompson1, L. P. Keller1, R. Christoffersen2, M. J. Loeffler3,4, R. V. Morris1, T. G. Graff2, and Z. Rahman2
1
ARES, NASA JSC, Houston, TX 77058
2
Jacobs, NASA Johnson Space Center, Mail Code XI3, Houston, TX, 77058
3NASA GSFC, Greenbelt, MD 20771
4Northern Arizona University, Department of Physics and Astronomy, Flagstaff, AZ 86011
Introduction: Grains on the surfaces of airless bodies are continually exposed to irradiation from solar wind ions andmicrometeorite impact events. These processes, collectively known as space weathering, alter the microstructure, chemicalcomposition, and spectral properties of surface soils [1-2]. While much work has been done to understand space weathering of
lunar and ordinary-chondritic materials e.g., [3-5], the effects of these processes on hydrated carbonaceous chondrites is not
yet well-understood. Analysis of the space weathering of carbonaceous materials will be critical for interpreting remotesensing reflectance data and for understanding the nature of samples returned by missions targeting primitive, organic-richairless bodies, e.g., Hayabusa2 and OSIRIS-REx.
Prior to sample return, we can simulate space weathering processes in the laboratory. Micrometeorite impacts can be
simulated through pulsed-laser irradiation, and recent experiments have shown the spectral properties of carbonaceous
materials are altered by such simulated weathering events e.g., [6-8]. However, the resulting type of alteration i.e., reddening
vs. bluing of the reflectance spectrum, is not consistent across all experiments. Further, the microstructural and crystal
chemical effects of many of these experiments have not been well characterized, making it difficult to attribute spectralchanges to specific mineralogical or chemical changes in the samples. Here we report results of pulsed laser irradiation
experiments on chips of the Murchison CM2 carbonaceous chondrite to simulate micrometeorite impact processing.
Samples and Methods: We performed three separate pulsed laser experiments by scanning a Nd-YAG laser (wavelength of1064 nm, average energy per pulse of 48 mJ, similar to [9]) (1) once, (2) twice, and (3) five times over the surface of thesample, in order to simulate various degrees of surface exposure. Glass slides were placed above the samples enabling thecollection of the recondensed vapor plume produced by the irradiation, similar to [10]. We obtained reflectance spectra (0.32.5 µm) from unirradiated and 1x-irradiated samples, as well as of thevapor deposit of the 1x-irradiated sample. We have analyzed themorphological and chemical effects of the 1x-irradiated samples using
the JEOL 7600F field emission scanning electron microscope (SEM)with x-ray detector system at JSC. From this sample, we have preparedelectron transparent thin sections from the vapor deposit, the meteorite
matrix, and several individual mineral phases using the FEI Quanta 3D
focused ion beam (FIB) instrument. These sections were analyzed using
the JEOL 2500SE scanning transmission electron microscope (STEM)
equipped with a Thermo thin window energy-dispersive X-ray (EDX)
spectrometer. We expect to make similar spectral measurements andprepare sections for STEM analysis for the 2x and 5x-irradiated sections.
Reflectance Measurements: The 1x-irradiated sample is darker (1-2%)
than the unirradiated material (Fig. 1a) and the vapor deposit on the glass
slide shows strong reddening through the VIS-NIR wavelengths (Fig. 1b).
Figure 1: Reflectance spectra of the A) Surface of the

Chemical and Structural Analysis: Vapor Deposit: The vapor deposit irradiated Murchison meteorite (red) compared to theis microstructurally and chemically complex, composed of several raw sample (blue), and B) The glass slide with theindividual layers ranging between 30-350 nm in thickness. The first layer deposit on it (red) compared to the plain glass slide(blue).
is a uniform (~50 nm) amorphous layer containing embedded
nanoparticles. Quantitative EDX maps indicate the composition of this layer is enriched in Fe, and includes S, Si, and O.
Overlying this initial deposit in several locations are thicker (up to 250 nm) deposits composed of Mg, Si, Fe, and Ca (inlocalized regions). There are vesicles and nanoparticles distributed throughout this layer. The outermost layer is thin (30-50nm) and EDX maps indicate it is enriched in volatile species including Fe and S, and includes embedded nanoparticles. The

nanoparticles distributed throughout the individual layers range in size from 2–30 nm in diameter and selected area electron
diffraction (SAED) indicates at least three individual phases are present in the nanoparticle-bearing deposits including troilite(FeS), pentlandite ((FeNi)9S8), and magnetite (Fe3O4).
Matrix: The SEM images show the irradiated fine-grained
matrix material has a distinctive ‘frothy’ texture, exhibiting
sub-µm voids uniformly distributed across the surface. TEM
analyses of the surface of the irradiated matrix provide
evidence of melting including amorphous spherules anddroplets. These melt products are up to 500 nm in thickness,
are often vesiculated, and contain embedded nanoparticles.
Quantitative EDX maps indicate the elemental composition of
the melt layers includes Fe, Mg, Si, and S, although volatile
species such as Fe and S are depleted in the melt layer relative
to the underlying matrix. The matrix phases maintaincrystallinity up to the boundary with the melt layer, with only
localized regions of amorphization. The nanoparticles range
in size from 5-50 nm and EDX maps indicate they are
dominated by Fe-Ni-Sulfides.
Olivine: Bright-field STEM images of an olivine grain
indicates there is an amorphous melt layer of uniform
thickness (~15 nm) on the surface of the grain. EDX maps
indicate this layer has an elemental composition that includes
Ca, Al, Mg, Si, and Fe, with more refractory species like Ca
and Al in higher concentrations than in the underlying grain.
Superimposed on this refractory deposit is a thicker, irregular Figure 2: Analysis of the irradiated sulfide grain reveals A) melt
features and vesicles in BF STEM, and B) areas of recrystallization(up to 70 nm) amorphous layer with high concentrations of in DF STEM, outlined by the dashed green lines. HRTEM images inC) and D) show zones of amorphization and short range order,
embedded nanoparticles ranging in size from 2-30 nm.
highlighted by FFTs of regions bounded by the red dashed boxed.
Fe-Ni-Sulfide: The surface of the Fe-Ni-Sulfide grain exhibits Measurements of the lattice fringes indicate spacings are consistent
melt textures including droplet-like features. Dark-field STEM with pentlandite. Round vesicles are shown in E). The region
and correlated HRTEM images of the melted region indicate outlined by the blue box in E) is shown in F). The chemicalcomposition of this region is shown by EDX maps of G) Ni, H) S,
localized areas near the surface of have recrystallized. Vesicles and I) Fe, indicating the composition is consistent between theare present within 500 nm of the surface and range in size irradiated area and the underlying material.
from 5-100 nm. Quantitative EDX maps indicate there is no significant difference in the composition of the sulfide grain at themelted and recrystallized surface when compared to the interior region of the sample (Fig. 2).
Implications for Space Weathering of Primitive Bodies: The observed elemental fractionation between melt and vapor
deposits influences the mineralogy of the nanoparticle population produced during space weathering events. The diversity ofnanoparticle phases identified here indicates that the space weathering of carbonaceous materials is more complex than their
lunar and ordinary chondrite-style counterparts. In addition, volatile species (including water) may play a significant role in theformation of space weathering features in carbonaceous surface materials. The prevalence of Fe-Ni-Sulfide and presence of
Fe-Oxide nanoparticles may contribute to the unpredictable spectral behavior of some experimentally-produced samples. As
such, an improved understanding of the optical characteristics of nanophase Fe-Ni-Sulfides is necessary to predict their effecton the spectral properties of airless body surfaces.
References: [1] Hapke B. 2001. Journal of Geophysical Research-Planets 106: 10,039-10,073. [2] Pieters C. M. and Noble S.
K. 2016. Journal of Geophysical Research-Planets 121: 1865-1884. [3] Keller L. P. and McKay D. S. 1997. Geochimica et
Cosmochimica Acta 61: 2331-2341. [4] Noguchi T. et al. 2014. Meteoritics and Planetary Science 49: 188-214. [5] Thompson
M. S. et al. 2014. Earth, Planets, and Space 66: 1-10. [6] Sasaki S. et al. 2001. Nature 410: 555-557. [7] Loeffler M. J. et al.
2008. Icarus 196: 285-292. [8] Gillis-Davis J. J. et al. 2017. Icarus 286: 1-14. [9] Matsuoka M. et al. 2015. Icarus 254: 135-143.
[10] Keller L. P. et al. 2013. Abstract 2404, 44th LPSC.

Development on non-destructive muonic X-ray analysis:
Appication to Earth and Planetary Science
K. TERADA1, A. SATO1, K. NINOMIYA1, Y. KAWASHIMA1, K. SHIMOMURA1, 2,
D. Tomono1, G. YOSHIDA1, Y. KAWAI1, T. OSAWA3 and S. TACHIBANA4
1

Osaka University, 2High Energy Accelerator Research Organization.
3
Japan Atomic Energy Agency and 4Hokkaido University

The muon is a lepton with a mass of 105.7 MeV/c2, approximately 200 times heavier than the electron. So far,electron-induced characteristic X-ray analysis has been widely used to determine chemical compositions of materials in Earthand Planetary Science. In recent years, analysis of characteristic X-rays from muonic atoms, in which a muon is captured, has
attracted attention because both a muon beam and a muon-induced characteristic X-ray have high transmission abilities, ofwhich energies are about 200 times higher (e.g., muonic carbon-Kα is 75keV, whereas electron-induced carbon-Kα is 0.3
keV). It is known that muonic X-ray analysis has great advantages in several ways; (1) non-destructive elemental analysis fromlight to heavy elements, (2) depth profile analysis, (3) isotopic measurement for heavy elements and (4) investigation ofchemical condition (redox-state). Such a non-destructive muonic X-ray analysis has a great potential to characterize precious
extraterrestrial samples returned by spacecrafts such as Hayabusa2 and OSIRIS-REx in 2020’s.
Following our successful detection of muonic X-ray spectra from carbonaceous chondrites, Murchison and Allendewith intense pulsed Muon beam at J-PARC [1], we have developed on muonic X-ray analysis at the MuSIC (MuSIC; MUon
Science Innovative Channel at Osaka University, [2, 3]), and obtained the fundamental data for quantitative analysis ofplanetary materials [4]. Using one of the world-leading intense direct current muon beam source, we successfully detectedcharacteristic muonic X-rays of Mg, Si, Fe, O, S and C from Jbilet Winselwan CM chondrite, of which carbon content is about
2 wt%, and the obtained elemental abundance pattern was consistent with that of CM chondrites. We also checked Muon
irradiation damage of pellets of mixed organic chemical reagents (alanine, glucose, paraformaldehyde, phenanthrene, andstearic acid) after 3–12 hour exposure to check the irradiation damage, and confirmed that they do not show any systematicchanges with either the exposure time or the depth, and are not different from those of non-exposed samples within thevariation of initial reagent mixtures. We also performed the muonic X-ray analysis of terrestrial PbS (Galena) for Pb isotopes
measurement and iron meteorite to check the feasibility of chemical condition (redox-state) measurement. At the symposium,
we will report on our recent progress of muonic X-ray analysis and discuss on a future prospect for applications for earth andplanetary science.

Figure 1: Direct-current Muon beam line at MuSIC, Osaka University.

Figure 2: Muonic X-ray spectra of Jbilet Winselwan CM2 chondrite.

References[1] Terada, K. et al. 2014. Sci. Rep. 4, 5072; DOI:10.1038/srep05072 [2] Hino, Y. et al. 2014. Nuclear Physics B (Proc.
Suppl.) 253-255, 206-207. [3] Cook, S. et al. 2017. Physical Review Accelerators and Beams 20, 030101.

Using X-ray Microfocus Spectroscopy to determine
Cometary and Asteroidal Parent-Body Processes
L. J. Hicks1, J. C. Bridges1, T. Noguchi2, M. C. Price3, J. E. Wickham-Eade3,
M. J. Burchell3, J. L. MacArthur1, G M. Hansford1, A. L. Butterworth4
1
Leicester Institute for Space and Earth Observation, Space Research Centre, University of Leicester, UK. (ljh47@le.ac.uk)
2Faculty of Arts and Science, Kyushu University, Japan. 3School of Physical Sciences, University of Kent, UK.
4Space Sciences Laboratory, University of California at Berkeley, USA.
Since the Stardust and Hayabusa missions, we have investigated a selection of these returned cometary and asteroidal samples
using Beamline I-18 at the Diamond Light Source synchrotron in UK, measuring Fe-K X-ray Absorption Spectroscopy (XAS)
and transmission X-ray Diffraction (XRD). Such techniques are essential to determine the origin and evolution of fine grainedplanetary materials, and in particular we have identified evidence for water-rock reaction on the Wild2 parent body.
I-18 X-ray microfocus spectroscopy
Beamline I-18 has an energy range 2.0-20.7 keV and a spot size reduced to ~2.5 μm. X-ray Fluorescence (XRF) can provide
chemical compositions, with XRF maps providing the opportunity to accurately locate features of interest at the micron-scale.
Fe-K XAS measurements typically range 6900-7500 eV at variable energy resolutions 1.0-10 eV, with higher resolution stepsof 0.1 eV focused over the XAS near-edge (XANES) region 7090-7150 eV necessary to accurately determine minor shifts andvariations in the 1s→3d transition pre-edge peak structure and absorption edge. The 1s→3d centroid position is estimated fromthe intensity-weighted average energy position over the pre-edge peaks, and the absorption edge position is the energy at which
intensity is 0.5 of the normalized spectra. Comparisons are made to reference materials, in particular the ferric content of silicatesare estimated by comparing pre-edge centroids with the ferrous-ferric energy shift in standards [1]. Combined with XRF mapping,producing XANES maps can reveal any variations in the ferric content. Additionally, in-situ measurements of transmissionXRD are acquired at 13 keV, with observable 2θ ranging 5.5°-38.4°, corresponding to d-spacings 9-1.5 Å.
Identifying magnetite in Comet Wild 2 samples
Initial investigations of Comet Wild 2 samples returned by Stardust
identified mostly high temperature ferromagnesian silicates [2], but
additional constituents have included CAI’s and chondrule-likefragments, suggesting links between carbonaceous chondrites and theWild 2 material [3].
Hicks et al. (2017) [4] investigated the terminal grains of eight
Stardust aerogel tracks, which include terminal grains identified asnear pure magnetite Fe3O4. Stardust track C2045,4,178,0,0 (#178)
featured a magnetite terminal grain measuring 10 µm in diameter, anda 5 µm magnetite terminal grain in track C2065,4,187,0,0 (#187),
both visibly identified via XAS structure (Figure 1). In particular,
absorption edge positions at 7121.5 and 7121.0 eV, and 1s→3d Figure 1. The Fe-K XAS and pre-edge centroid (inset) ofcentroid positions estimated at 7113.1 and 7113.5 eV, closely terminal grains in tracks #178 (Tg1a), #187 (Tg1), and #189
resemble that of a magnetite powder standard with edge and centroid (Tg1), and an analogue CR2 terminal grain (Tg) shot into
positions at 7120.8 eV and 7113.2 eV respectively. A small positive aerogel, compared to powdered magnetite and hematite
shift of up to ~0.5 eV in the Wild 2 grains, compared to the magnetite standard reference material.
standard, could be due to a minor Ni2+ content identified with XRF,
which replaces some Fe2+, resulting in a higher Fe3+/ΣFe content, thus a positive shift in the energy of the Fe-K XAS spectra.
In-situ transmission XRD analyses also identified magnetite with 2θ peaks at d-spacings 1.48 Å, 1.61 Å, 1.71 Å, 2.10 Å, 2.42 Å,
2.53 Å, and 2.96 Å for the cometary #178 (Tg1a and Tg2) and #187 (Tg1), closely matching the 2θ peaks a magnetite referencematerial. However, with unit cell dimensions ranging 8.355-8.370 Å for the cometary grains being slightly lower than that of apure magnetite at 8.387 Å, this shift also suggests a Ni-bearing magnetite. Raman analyses performed at University of Kent also
confirmed a Ni-bearing magnetite. Material in other Stardust tracks, identified via XAS analyses on I-18 at Diamond, include
olivine (#177, #178, #187), pyroxene (#189, #190), Fe,Ni-metal (#170, #176), and Fe,Ni-sulfide (#187, #188) [4].

Magnetite grains are prominent in carbonaceous chondrites, if they have been oxidised and aqueously altered [5], thus thepresence of magnetite in the Wild 2 mineral assemblage suggests further affinities to carbonaceous chondrites, probably resulting
from hydrothermal alteration of the co-existing FeNi and ferromagnesian silicates in the cometary parent-body. Exploring thishypothesis further, powdered NWA 10256 CR2 chondrite material was shot into aerogel at 6.1 kms -1, using a light gas gun [6],simulating the conditions of the Stardust collection. Fe-K XAS identified CR2 magnetite terminal grains (Figure 1) establishing
the likelihood of preserving magnetite during capture in silica aerogel.
Itokawa ferromagnesian silicates and LL5 chondrite
Initial analyses of the Itokawa asteroid particles returned by
Hayabusa had already found mineralogical, petrological, and oxygenisotopic affinities to LL5-6 chondrites [7,8,9]. We used Fe-K XAS toinvestigate the relative abundance of Fe3+ and Fe2+ ions in the
ferromagnesian silicates of the Itokawa grains, comparing them to the
Tuxtuac LL5 chondrite meteorite.
Noguchi et al. (2014) [10] investigated four samples from the first
Hayabusa touch-down location: RB-QD04-0008; RB-QD04-0011;
RB-QD04-0015; and RBQD04-0024. These samples, each embedded
in epoxy resin, featured olivine with trace amounts of opaque Figure 2. The Fe-K XAS for olivine in three Itokawa particles,
minerals (0011 and 0015), olivine and high-Ca pyroxene (0008), and the Tuxtuac LL5 chondrite, and a terrestrial olivine (Sanlow-Ca pyroxene with plagioclase and small (<2 μm) opaque Carlos).
minerals (0024).
Fe-K XAS for the olivines (Figure 2) estimated absorption edges and 1s→3d centroids at 7119.5-7119.8 eV and 7112.5-7112.6
eV respectively, indistinguishable from those estimated for the Tuxtuac olivine and in terrestrial olivine. Edges and centroids forthe low-Ca Itokawa pyroxene (7119.7 eV and 7112.6 eV), and the high-Ca Itokawa pyroxene (7119.4 eV and 7112.6 eV), arealso indistinguishable from Tuxtuac and from Fe2+ in terrestrial augite. EXAFS analyses of the high-Ca Itokawa pyroxene
suggested a disordered structure which may be partial equilibration or shock. A Ni-bearing phase associated with that high-Ca
Itokawa pyroxene (0008) was also measured for Ni-K XAS, finding similarities to taenite in the LL5 Tuxtuac.
The Fe-K XAS analyses suggested a negligible abundance of Fe3+ ions in Itokawa and the LL5 ferromagnesian silicates,consistent with the initial analyses [7,8,9]. However, the EPMA analyses of the four Itokawa grains, that followed the Fe-K
XAS analysis, suggested a wide range of thermal metamorphism corresponding to petrologic chondrite types LL4 to LL6.
Future XAS investigations of Planetary Sample Returns
As we continue to investigate planetary materials further, and as missions such as Hayabusa 2 and OSIRIS-REx return samples
to Earth, more advanced techniques will be essential to analyse micron-sized material, furthering our understanding of planetary
formation. Offering similar techniques to I-18, but with higher spatial resolution down to ~50 nm, the new I-14 hard X-ray
nanoprobe beamline at Diamond offers nanoscale microscopy with an energy range 5-23 keV, capable of XAS, XANES mapping,and XRD. Additionally, the I-08 Scanning X-ray Microscope (SXM) beamline performs XRF and XANES, but in the soft Xray energy range 0.25-4.4 keV, including Si-K XANES, with a spatial resolution down to ~200 nm.
References[1] Berry, A.J. et al., XANES calibration for the oxidation state of iron in silicate glass. Am. Mineral., 88, 967-977, 2003. [2Zolensky, M. et al., Mineralogy and petrology of Comet 81P/Wild 2 nucleus samples. Science, 314, 1735-1739, 2006. [3]Westphal, A.J. et al., The future of Stardust science. Meteorit. Planet. Sci., in press, 2017. [4] Hicks, L.J. et al., Magnetite in
Comet Wild 2: Evidence for parent body aqueous alteration, Meteorit. Planet. Sci., in press, 2017. [5] Hutchison, R., Meteorites:
A petrologic, chemical and isotopic synthesis. Cambridge Press, 2004. [6] Burchell, M.J., et al., Hypervelocity impact studies
using the 2 MV Van de graff accelerator and two-stage light-gas gun of the University of Kent at Canterbury. Meas. Sci. Technol.,10, 41-50, 1999. [7] Nakamura T. et al., Itokawa Dust Particles: A Direct Link Between S-Type Asteroids and Ordinary
Chondrites. Science, 333, 1113-1116, 2011. [8] Yurimoto H. et al., Oxygen Isotopic Compositions of Asteroidal Materials
Returned from Itokawa by the Hayabusa Mission. Science, 333, 1116-1119 2011. [9] Nakamura E. et al., Space environment ofan asteroid preserved on micrograms returned by the Hayabusa spacecraft. Proc. Nat. Acad. Sci., 109, 4031-4032, 2012. [10]Noguchi, T. et al., Mineralogy of four Itokawa particles collected from the first touchdown site, Earth Planets Space, 66: 124,
2014.

The Astromaterials X-Ray Computed Tomography Laboratory at Johnson Space Center
Ryan A. Zeigler, Poorna Srinivasan, Lindsay P. Keller, Francis McCubbin, and Daniel M. Coleff
Astromaterials Research and Exploration Division, NASA JSC, Mailcode XI, 2101 NASA Parkway, Houston, TX 77058
Overview: The Astromaterials Acquisition and Curation Office at NASA’s Johnson Space Center (hereafter JSC curation)is the past, present, and future home of all of NASA’s astromaterials sample collections. JSC curation currently houses all orpart of nine different sample collections. Our primary goals are to maintain the long-term integrity of the samples and ensurethat the samples are distributed for scientific study in a fair, timely, and responsible manner, thus maximizing the return oneach sample. Part of the curation process is planning for the future, thus we also perform fundamental research in advanced
curation initiatives. Advanced Curation is tasked with developing procedures, technology, and data sets necessary for curating
new types of sample collections, or getting new results from existing sample collections [1]. As part of these advanced curation
efforts we are augmenting our analytical facilities. A micro X-ray computed tomography (micro-XCT) laboratory dedicated tothe study of astromaterials came online within the JSC Curation office this summer, and we plan to add additional facilities
that will enable non-destructive (or minimally-destructive) analysesof astromaterials in the near future (micro-XRF, confocal imaging
Raman Spectroscopy). These facilities will be available to: (1)develop sample handling and storage techniques for future sample
return missions, (2) be utilized by PET for future sample return
missions, (3) be used for retroactive PET-style analyses of ourexisting collections, and (4) for periodic assessments of the existing
sample collections. Here we describe the new micro-XCT system, as
well as some of the ongoing or anticipated applications of the
instrument.
Instrument: We have installed a Nikon XTH 320 micro-XCTsystem in JSC curation. It has four interchangeable X-ray sources:
180 kV nano focus transmission source, 225 kV reflection sourcewith multi-metal target (Mo, W, Ag, Cu), a 225 kV rotating target(W) reflection source, and a 320 kV reflection source. The system
also has a 16-bit, 400 mm2 (2000 x 2000 pixel) CCD detector, as
well as a heavy-duty stage that will accommodate large (up to 30cm) and heavy (up to 100 kg) samples. The multiple sources, highresolution detector, and large stage allow us the flexibility toanalyze a wide range of sample sizes. The 180 kV transmission
source will allow for high resolution (submicron) scans on small
samples (less than ~5 mm), whereas the 225 kV and 320 kV sources
will allow scans of larger samples at resolutions on the order of 10s
or 100s of microns per voxel depending on the sample size. The
maximum size high-density rock sample that can be scanned has yet
to be determined, but test scans on basalt samples >15 cm indiameter have been successful.
Discussion: High-intensity XCT scanners have been used to
study astromaterials (and other geologic samples) for over 15 years[2-3], and the practice is becoming ever more prevalent. They havea wide range of scientific uses, including (but certainly not limitedto) measuring porosity, determining the modal abundance and 3D
distribution of phases inside samples, and identification of fabrics
or strain patterns in samples. In addition to their use for research,
Figure 1: Slices of the micro-CT scan of sample 14321,1404.
Brightness of the phases are proportional to x-ray attenuation (aXCT scans have increasingly been utilized as a part of themeasure of composition and density of the phase). Yellow arrows
astromaterials curation process, beginning with meteorites [4-5],
highlight interesting feldspathic (top) and mafic (bottom) clasts.
Sample is ~ 6 cm in diameter.
and more recently with the Apollo samples [6]. Their utility inFigure 2: Single 2D slice of the micro-CT scan of ungrouped achondrite NWA 11119 showing the igneous textures and major mineralogical phases
within the sample. Sample is ~ 3 cm long.

curation lies in their ability to non-destructively map out the phases and voids within a sample. As an example, we havescanned several large Apollo polymict breccias, and we were able to identify and tentatively classify the lithologies in theseclasts. The samples can then be subdivided, either through sawing or careful chipping, and those “new” clasts made available
to scientists. In addition to the myriad curatorial uses, we have begun to use the XCT system as an integral part of coordinatedanalyses of astromaterials. Two examples of this are the mapping of textures within ungrouped achondrite NWA 11119(Figure 2), as well as a newly acquired unclassified carbonaceous chondrite from Morocco (Figure 3). In each case, the XCTscans were able to characterize the major phases with the meteorites, and identify areas of interest for additional higher
resolution study (e.g., by TEM). The penetrative nature of the XCT scans allows for astromaterials samples to be analyzed
within sealed low-density containers, preserving the pristinity of the samples. The XCT technique is not completely nondestructive, however. A recent study by [7] has shownthat XCT scans of meteorites can alter the naturalradiation dose of the sample. The number of techniques
where this is applicable (e.g., thermo-luminescence) islimited, however. Never-theless, XCT scans could
cause damage for other types of studies (e.g., organics),
and we plan to undertake extensive studies to fully
characterize the impact XCT scans have on the samples.
In the meantime, the percentage of any one sample thatis studied by XCT will be limited to ensure that no
irreparable damage is done to an entire sample.
References [1] McCubbin et. al. (2017) This
Symposium, [2] McCoy et al. (2002) EPSL 246, 102108. [3] Zolensky et al. (2014) MAPS 49, 1997-2016.
[4] Almeida et al. (2014), MAPS 77 abstract #5033. [5]Smith C. L. (2013) MAPS 76, abstract #5323. [6]Zeigler (2014) 45th LPSC, abstract #2665. [7] Sears, etal. (2016) MAPS 51.4, 833-838.

Figure 3: Single slice of the micro-CT scan of an unclassified Moroccan
carbonaceous chondrite. Large dark grey areas are large zoned CAIs. Sample is~4 cm in diameter.

Reproduction of GEMS-like materials in the induction thermal plasma system

1

Tae-Hee Kim1, Akira Tsuchiyama1, Junya Matsuno1, Aki Takigawa1,2
Mineralogical Laboratory, Division of Earth and Planetary Sciences, Kyoto University, Kyoto, Japan
2
The Hakubi Center for Advanced Research, Kyoto University, Kyoto, Japan

Amorphous silicates are considered to be one of the most primitive materials of the solar system and some of them camefrom pre-solar environments. Chondritic porous interplanetary dust particles (CP IDPs) contain abundant amorphous silicate
grains of ~100 nm in size with Fe-Ni and FeS nanoparticles known as GEMS (glass with embedded metal and sulfides) [1,2].
Solar and interstellar origins of GEMS have been proposed [1, 2]. Experimental study on non-equilibrium condensation of
GEMS-like materials is crucial for determination of the GEMS origin.
The ITP system (induction thermal plasma) offers rapid vaporization condition by a discharged high temperature flame(~10,000 K) and rapid cooling rate (104~105 K/s). Amorphous silicates with metallic iron nanoparticles inside, which aresimilar to the characteristics of GEMS, were experimentally reproduced using an ITP system [3]. In order to constrain theformation condition of GEMS, we systematically changed ITP operation conditions and performed evaporation andcondensation experiments with a new ITP system [4].
The ITP system used in the present study was JEOL TP-40020NPS with 6 kW RF plasma torch. We carried out thevaporization and condensation experiments with a mixed Ar-He plasma flame in the system of Si-Mg-Fe-Na-Al-Ca-Ni-O withthe averaged chemical composition of GEMS [1] without sulfur. The plasma generating condition was controlled by selectionof a plasma forming gas injecting direction (tangential and radial flame patterns) and reactor pressure (30 and 70 kPa). The
tangential flame of the thermal plasma provides more higher cooling rate than the radial flame, and higher reactor pressure
enhances the vaporization degree of the starting material [4].
All run products show presence of amorphous silicate, metallic iron, and FeNi in X-ray diffraction spectra and peaks ofamorphous silicate at ~10 µm in the FTIR spectra. TEM observation shows that the run products have a variety of textures;
amorphous silicate grains from <a few nm to >100 nm with or without aggregation and with or without embedded metallic
iron or iron nickel nanoparticles. Among them, the most similar nanomaterial with GEMS was reproduced in a tangential
flame condition at 70 kPa (Fig. 1). Although the condensation condition was not quantitatively investigated yet, the present
result shows that GEMS-like nanomaterial can form in a limited parameter range of the ITP system, which indicates that theformation conditions and environments of actual GEMS might also be limited.

Figure 1. (a) TEM image and (b) STEM-HADDF image of metal embedded amorphous silicate grains produced in tangential plasma flame
condition at 70 kPa.

References[1] Keller L. P. et al. 2011. Geochimica et Cosmochimica Acta, 75:5336[2] Bradley J. P. et al. 2004. Astrophysical Journal, 17:650[3] Matsuno J. 2015. Ph.D. thesis, Kyoto University.
[4] Kim T. H. et al. 2017. Proceeding #P2-33-7. ISPC 23 (International Symposium on Plasma Chemistry)GRAVITATIONAL INSTABILITY ON PROPAGATION OF MHD WAVES INASTROPHYSICAL PLASMA
Alemayehu Mengesha Cherkos1,2 AND S. B. Tessema 1,2
1. Entoto Astronomical Observatory and Space Science Research Center, P.O. Box 8412, Addis

Ababa, Ethiopia
2. Department of Physics, Kotebe College, P.O. Box 31248, Addis Ababa, Ethiopia(alexye9@yahoo.com)
Abstract
We determine the general dispersion relation for the propagation of magnetohydrodynamic (MHD)
waves in astrophysical plasma by considering the effect of gravitational instability and viscositywith anisotropic pressure tensor and heat-conducting plasma. Basic MHD equations have been
derived and linearized by the method of perturbation to develop the general form of dispersion
relation equation. Our result indicates that the transverse propagation of waves in such a plasma isaffected by the inclusion of heat conduction. For wave propagation, parallel to the magnetic field
direction, we find that the fairhose mode is unaffected, whereas the mode corresponding to thegravitational instability is modified in astrophysical plasma with anisotropic pressure tensor being
stable in the presence of viscosity and strong magnetic field at considerable wavelength.

Study of solar cycle variation and its impact on critical frequency of F2 layer
P. K. Purohit1and Roshni Atulkar1
National Institute of Technical Teachers' Training and Research, Bhopal – 462002, MP, India.

1

The period of approximately 11 year cycle of solar activity is characterized by the rise and fall in the numbers
and surface area of sunspots. We observed a number of other solar activity indices, including the 10.7 cm radio
flux, solar Mg II core to wing ratio, relative sunspot number Rz and solar flare index geomagnetic activity thatvary in association with the sunspots for solar cycles 23 (1996–2008). This paper presents an analysis of the Fregion variability of the ionospheric F2 layer critical frequency (foF2) at Australian mid latitude ionosonde
station, Hobart (42.88° S and 147.32° E) during the period 1996 – 2008 of solar cycle 23. The diurnal, monthly,and yearly. characteristics of ionospheric F-region parameter foF2 have been studied in detail. We also
compared the dependence of foF2 on solar activity indices by using a correlation analysis, and showed asignificant linear relationship between the foF2 values and Solar indices. The foF2 variation is strongly
influenced by solar activity with about an 11-year solar cycle from the solar maximum to solar minimum.

Table 1. Correlation of foF2 with solar indices during different phases of solar cycle 23.
Geomagnetic Indices Vs Fof2.

Correlation

Flare Index-foF2

0.85

Rz-foF2

0.92

F10.7-foF2

0.93

Mg II c/w-foF2

0.88

Figure – 1: Monthly variation of solar indices with criticalfrequency foF2 during Solar Cycle 23.

Figure-3: Behavior of critical frequency foF2 and solar
indices during the solar cycle 23.

Figure–2: Annual variation of solar indices with criticalfrequency foF2 during Solar Cycle 23.

Figure – 4: Scatter and Correlation of foF2 with Flare index,
sunspot number (Rz), Radio flux (F10.7) and Mg II core to
wing ratio during the solar cycle 23.

References[1] Adler N O et al 1997., Solar cycle length variation: its relation with ionospheric parameters, Journal of
Atmospheric and Solar-Terrestrral Physics, Vol. 59, No. 2, pp. 159 162.[2] Bruevich E.A.et al 2011., Changed
Relation Between Radio Flux F10;7 And Some Solar Activity Indices During Cycles 21 – 23, Solar and Stellar
Astrophysics (astro-ph.SR.[3] Bilitza D. 2000The importance of EUV indices for the international reference
ionosphere. Phys Chem Earth (C), 25: 515–521[4] Sethi N. K., Goel et al 2002Solar cycle variations of foF2
from IGY to 1990, Ann. Geophys., 20, 1677 – 1685.

Study of magnetic storm effects on the variation of TEC over low, mid and high latitude station
1

Roshni Atulkar1 and P. K. Purohit1
National Institute of Technical Teachers' Training and Research, Bhopal – 462002, MP, India.

The ionosphere is very important because of its influence on the passage of radio waves. Total electron content (TEC) is a key
ionospheric parameter that describes the major impact of the ionosphere on the propagate on of radio waves which are crucial
for terrestrial and space communication. The present investigation is dedicated to study the latitudinal variation of ionosphere.
The study is carried out by taking three stations one each in low, mid and high latitude regions namely IISC, Bangalore, India(13.020 N, 77.570E), GUAO, Urumqi, China (43.820N, 87.600E) and NYAL, NY-Alesund, Norway (78.920N, 11.860E)
respectively. To study the changes in the ionosphere at three selected station we have considered the GPS observations. The
GPS derived TEC values have been collected from the SOPAC (Scripps Orbits and Permanent Array Center) data archive of
the IGS (International GPS service). We studied the behaviour of ionospheric Total Electron Content (TEC) during thegeomagnetic storms. We have selected 5 intense geomagnetic storms (Dst ≤ -100nT) that were observed during the year 2012.
From our analysis we observed that the effect of geomagnetic storms on VTEC is highest at low latitude, moderate at midlatitude and low at high latitude.
Table 1. Catalogue of all the five selected intense geomagnetic storm events along with Peak Dst.

Event Date

Peak Dst(Min.)

9 March 2012

-143nT

24 April 2012

-104nT

15 July 2012

-133nT

1October 2012

-133nT

14 November 2012

-109nTFigure 1:

Figure 2

Figure 3

Figure 4

Figure 5
Figure 1. 2,3,4 and 5. Plot of temporal evolution of ionospheric VTEC along with Dst, IMF Bz and AE during the geomagnetic storm of
9 March, 24 April,15 July,1 October, and 14 November 2012.

References[1] Akasofu S -I.(1981) Relationships between the AE and Dst indices during geomagnetic storms. J. Geophys. Res.86:4820–
4822.[2] Mendillo M, et al. 1970, Ionospheric storms at midlatitudes. Radio Sci.;5:895–898. and,doi: 10.1029/RS005i006p00895.[3] Titheridge J E et al.1988. A comparison of Northern and Southern Hemisphere TEC storm
behaviour. J. Atmos. Terr. Phys.;50:763–780.

Moon-Earth: global basaltic effusions, their different ages, common chemical trends(alkalinity, iron content)
Gennady G. Kochemasov
IGEM of the Russian Academy of Sciences, 35 Staromonetny, 119017 Moscow,kochem.36@mail.ru

Global basaltic covers are very characteristic phenomena in the inner solar system. Basaltic
effusions of different ages and compositions originated in asthenospheric layers of theplanetary mantles. To heat and melt some parts of the mantle, a part of enormous mechanicalenergy of orbiting cosmic bodies was transferred to the heat energy.
“Orbits make structures” – a main point of the new wave planetology based on one
important property of the Keplerian elliptical planetary orbits [2, 3] . The ellipticity implies
periodical changes of accelerations and, thus, orbital forces structuring cosmic bodies. The
Earth and the Moon sharing the same circumsolar orbit have similar main structural features.
Among them there are terrestrial Oceans and lunar Basins. The most obvious are two tectonic
triads: Pacific Ocean – Malay Archipelago – Indian Ocean on Earth and Procellarum Basin –Mare Orientale – SPA Basin on the Moon. The planetary depressions of both bodies arecovered with basalts, but basaltic effusions are drastically different in age: the AR on Moon
and Mz-Cz on Earth. These ages well correlate with the bodies masses. The more massive andinert Earth has heated and melted mantle much later (The Newton’s law of inertia). Energy of
movement transfers to the heat energy.
The both cosmic bodies, as well as the rest of them, are tectonically dichotomous. Theirsubsided hemispheres, for keeping angular momentum of hemispheres equal, are filled with
dense basaltic material. But times of the fillings are significantly different.
The Earth-Moon system expands with time, that is increases its angular momentum. A
natural response to it is in slowing down rotation of both bodies diminishing their angularmomentum (action - opposite action). Diminishing momenta are compensated by melting anduplifting to surfaces dense basaltic material. But on the Moon it happened much earlier(4.5-3 billion years ago) because of diminished inertia of the small mass satellite. At muchlarger and massive with large inertia Earth this process was significantly “delayed” intime.(Mz-Cz). Earth is 81 times more massive than Moon. (3-4.5 billions) : 81 = 37-55
million years. According to this calculation, a “peak” of the basaltic reaction of Earth, fillingin by basalts the oceanic depressions is in the boundary of Mesozoic and Cenozoic [3]].
Despite of enormous age differences between lunar and terrestrial basaltic covers (billionsof years!) some common chemical shift of their compositions is notable and significant. Let
us compare Procellarum Basin and Pacific Ocean basalts. The oldest parts of their covers
occur mainly in the West of Procellarum (KREEP) and SW of the Pacific (Ontong Java
Plateau – the largest LIP of Earth). Potassium, phosphorus, rare earths, thorium enrich theolder lunar KREEP basalts. The older terrestrial oceanic Ontong Java basalts (Cretaceous ageabout 122 mln. y) also show “KREEP trend”. They belong to E-MORBs and have elevatedvalues of potassium, lithium, chlorine, REE, thorium. Elevated Fe/Mg (and siderofile
platinum group elements) also is in Ontong Java basalts [1]. All these chemical peculiarities
distinguish them from the younger N-MORBs of other parts of the Pacific Ocean (EPR, forexample). As all considered basalt melts of both bodies originate in asthenopheres, the older
parts of these melts derive from relatively earlier “cool” asthenosphere. It means that only
easily melted alkali and iron rich parts were involved in the process. Later on, significantly
heated asthenospheres produced enormous volumes of chemically different (less alkaline andmore magnesian) basalts. In this sense, rather impressive is a comparison of the lunar iron andthorium geochemical maps stressing coincidence of their anomalies in the Procellarum
KREEP terrain area (Fig. 1, 2).
The considered time development of basaltic magmatism could be paralleled with thedevelopment of alkaline terrestrial magmatism. Its earlier older parts often are more alkaline
than later Cenozoic parts. Famous large agpaitic massifs are mainly Proterozoic-Paleozoic inage. Again, early “cold” asthenosphere produces more easily melted relatively small alkalineparts than the later “hot” asthenosphere making large volumes of deeply melted moremagnesian less alkaline ones.
References:[1] Ely J.C. and Neal C.R. (2003) Using platinum-group elements to investigate the origin of
the Ontong Java Plateau, SW Pacific // Chemical Geology, v. 196, 235-25[2] Kochemasov G.G. (2016) The Moon and Phobos: specific responses of two satellites
moving off and nearer their respective planets // DPS 48/EPSC 11, Pasadena, Oct. 16-21,
2016, Bulletin of the American Astronomical Society, 2016, vol. 48, # 7, p. 175, Abstract
318.08, Session 318: Formation and Evolution of Planets and Satellites Posters.
[3] Kochemasov G.G. (2017) New planetology and geology: tectonic identity and principal
difference of terrestrial oceans and lunar basins // New Concepts in Global Tectonics (NCGT)
Journal, 2017, V. 5, # 1, p 131-133.

1

2

On the bulk silicate composition of carbonaceous chondrites
P. Futó1, A. Gucsik2
University of Debrecen, Department of Mineralogy and Geology, Debrecen, Egyetem tér 1. H-4032, Hungary(dvision@citromail.hu)
2
Wigner Research Center for Physics, Hungarian Academy of Sciences, Konkoly Thege Miklós 29-33., Budapest, Hungary
1Introduction:
The bulk compositions of the stony meteorites have been dominated by silicates and oxides. The one part of meteoritic
minerals came through different grade of the chemical and/or physical transformations during the formation of the SolarSystem. There are ancient mineral constituents, which survived the early stage of the evolution of the Solar-System and they
appears original form: presolar dust grains. Primitive meteorites contain presolar dust grains: silicates, oxides, nanodiamonds,
silicon carbide graphite, silicon nitride. The dominant sources of dust grains are the AGB stars and supernovae. The presolar
silicate abundance is greater than the abundances of other presolar minerals [1].
Carbonaceous chondrites (CC, c-chondrites) are primitive meteorites with significant silicate and oxide amounts, some of them
contain a relatively larger amount of elemental carbon (diamonds, graphite) and carbon-based compounds (silicon-carbide,
different organic compounds). They are composed mostly of chondrules, inclusions and the fine-grained matrix. C-chondrites
can be classified according to that their parent bodies formed in different regions of the early Solar-system. Accordingly,
different CC-groups may distinguished as CI, CM, CV, CO, CR, CK, and CH type chondrites [2]. The groups are further
divided into different subgroups.
Similarities and significant differences also appears in the abundances of given compounds in the different chondrites
depending on the formation conditions of their parent bodies. For instance, the bulk composition of Allende matrix is Fe-richobtained by Inoue et al. [3], the CM2 Murchison meteorite is an organic rich carbonaceous chondrite [4]. Chemical similarities
appear between CM and CO chondrite chondrules [5], while considerable differences show the Murchison (CM2) and the
Allende (CV3) chondrites in carbon content of the matrix.
In carbonaceous chondrites, highly forsteritic (Mg 2SiO4) olivine can be found for example in the chondrules, in the (Amoebid
Olivine Aggregates (AOA) and in the grains and aggregates embedded in the matrix. Fayalitic olivine (Fe 2SiO4) is also
identified in the mineral structures, but its amount is smaller than that of the forsterite. Enstatite (MgSiO 3) and ferrosillite(FeSiO3) are also known in the mineral textures of chondrites.
Bulk silicate composition of c-chondrites The investigation for characteristics of silicates based on in detail the Kaba primitiveCV3 c-chondrite [6], otherwise we studied the pure matrix material of the Allende CV3 c-chondrite with the concerning datautilized from the results of Inoue N. et al. 2004 [3]. We determined the Mg/Fe ratio in the silicates and the results have beensummarized in the Table 1.
Kaba (CV3)mineralstructure

Mineral sample

FeO(wt%)MgO(wt%)Mg/FePorphyritic Forsteritechondrule

Fo1-1

0.30

55

Mg0.993Fe0.007

Granularol-px
chondrule

Forsterite

Fo3-1

0.89

54.99

Mg0.98 Fe0.02

Forsterite

Fo3-2

1.02

54.70

Mg0.976Fe0.024

Isolatedolivinegrain

Forsterite

Fo8-2

0.21

56.91

Mg0.995Fe0.005

Comlicated Fayalite
aggregate

Fa9-2

68.05

0.26

Mg0.003Fe0.997

36.60

19.19

Mg0.407Fe0.593

Allende(CV3)Pure matrix

A1

Table 1. The FeO and the MgO abundances in different mineral structures of the Kaba meteorite (CV3) and in the bulk chemical compositionof the matrix of the Allende (CV3) chondrite. The Mg/Fe ratio is calculated from the basic data that are taken from Gucsik A. et al. (2013)
and from Inoue M. et al. (2004).

As seen in the Table 1, the mineral components of the Kaba meteorite is rich in highly forsteritic (Fo>0.99) olivines, while thebulk silicate composition of the Allende matrix enriched in iron. In fact, the mineral composition of chondritic meteorites has
been dominated by silicates. The elemental abundances of chondrites approximately consistent with the cosmic abundances of
elements and minerals. The high ratio of Mg, Si, and O in meteorites refers to the dominance of magnesium silicates for thecase of chemical characteristics of the Galaxy as opposed to the abundances of Fe-, Ca-, Al-silicates.
Summary: The carbonaceous chondrites are known to have been dominated by silicates but they may contain carbonaceous
mineral constituents in small amounts. The bulk composition of the planet-building materials in the most circumstellar
enviroments is assumed to be chondritic-like.

References[1] Nguyen A. N. et al., Characterization of presolar silicate and oxide grains in primitive carbonaceous chondrites, The
Astrophysical Journal 656, 1223-124, 2007. [2] Kallemeyn G.W. and J.T. Wasson, The compositional classification ofchondrites—I. The carbonaceous chondrite groups, Geochimica et Cosmochimica Acta , 45(7), 1217-1230, 1981. [3] Inoue N.
et al. EE abundances in the matrix of the Allende (CV) meteorite: Implications for matrix origin, Meteoritics & Planetary
Science 39,599-608, 2004. [4] Kebukawa Y. et al., Kinetics of organic matter degradation in the Murchison meteorite for theevaluation of parent-body temperature history, Meteoritics & Planetary Science 45, 99-113, 2010. [5] Schrader D. L. and J.
Davidson, CM and CO chondrites: A common parent body or asteroidal neighbors? Insights from chondrule silicates,
Geochimica et Cosmochimica Acta , 214, 157-171, 2017. [6] Gucsik A. et al., Cathodoluminescence microscopy andspectroscopy of forsterite from Kaba meteorite: An application to the study of hydrothermal alteration of parent body,
Meteoritics & Planetary Science 48, 2577-2596, 2013.

NASA Curation Preparation for Ryugu Sample Returned by JAXA’s Hayabusa2 Mission
Keiko Nakamura-Messenger1, Kevin Righter1, Christopher J. Snead2, Francis M. McCubbin1, Lisa F. Pace1, Ryan A. Zeigler1,& Cindy Evans1
1
NASA Johnson Space Center, Houston, TX USA, 2JETS at NASA Johnson Space Center, Houston, TX, USA
The NASA OSIRIS-REx and JAXA Hayabusa2 missions to near-Earth asteroids Bennu and Ryugu share similar
mission goals of understanding the origins of primitive, organic-rich asteroids. Under an agreement between JAXA and NASA,
there is an on-going and productive collaboration between science teams of Hayabusa2 [1] and OSIRIS-REx missions [2].
Under this agreement, a portion of each of the returned sample masses will be exchanged between the agencies and thescientific results of their study will be shared. NASA’s portion of the returned Hayabusa2 sample, consisting of 10% of the
returned mass, will be jointly separated by NASA and JAXA. The sample will be legally and physically transferred to NASA’s
dedicated Hayabusa2 curation facility at Johnson Space Center (JSC) no later than one year after the return of the Hayabusa2
sample to Earth (December 2020). The JSC Hayabusa2 curation cleanroom facility design has now been completed. In thesame manner, JAXA will receive 0.5% of the total returned OSIRIS-REx sample (minimum required sample to return 60 g,
maximum sample return capacity of 2 kg) from the rest of the specimen [2]. No later than one year after the return of the
OSIRIS-REx sample to Earth (September 2023), legal, physical, and permanent custody of this sample subset will betransferred to JAXA, and the sample subset will be brought to JAXA’s Extraterrestrial Sample Curation Center (ESCuC) at
Institute of Space and Astronautical Science, Sagamihara City Japan.
Both the Hayabusa2 sample to be sent to NASA and the OSIRIS-REx sample to be sent to JAXA will be unprocessed
and representative of the returned bulk sample. “Unprocessed” means that the sample will be handled in a way that minimizes
chemical and physical changes to the sample, including avoidance of harsh radiation and heating environments such as
electron beams and Raman microscopy. The exchange samples will also be protected from organic and other forms ofcontamination to the greatest extent possible. “Representative” means that the separated sample has, as well as can be
determined on the unprocessed sample, very similar characteristics to the bulk returned sample, including grain size, color, andother physical properties readily determined by optical observation.
The overarching objectives of NASA’s Hayabusa2 curation are to preserve and protect the returned Ryugu subset
samples to maximize the science return. Curation scientists at JSC together with ESCuC members and the OSIRIS-REx
science team have been working to identify requirements on contamination and sample environmental controls. The
Hayabusa2 curation requirements can be categorized into the following nine major responsibilities: 1) Contamination control,
2) Curation procedures for solid and gas samples from Ryugu surfaces, 3) Clean laboratory design and construction, 4).
Sample characterization for catalog (non-destructive organic-nonorganic lithology identification in a glovebox), 5) Sample
distribution, and 6) long term curation activity. Many of the aspects of NASA Hayabusa2 curation for the Ryugu samples are
already well developed and have strong heritage at JSC. Examples of existing knowledge and application in this area include
ppb level organic residue monitoring of the gaseous curation grade nitrogen, precision cleaning of ultrapure water circulatingin the clean labs, particle count monitoring, and metal material control for terrestrial trace element contamination control(Apollo, Genesis samples), and sample handling of small particles (cosmic dust, Stardust cometary particles, Hayabusa1
asteroid samples), to mm-cm sized rocks (Antarctic meteorites). The Hayabusa2 sample storage and handling facility at JSC
have been co-designed with the OSIRIS-REx sample curation clean facility to protect the samples from contamination, crosscontamination, temperature excursions, and moisture that could alter the sample. The construction of the facility will start in2018 [3].
As with every new extraterrestrial collection, returned primitive Ryugu samples bring special new requirements forpotentially organic rich samples. Hayabusa2 mission will attempt to collect three samples from the surface of the asteroid inorder to return a minimum of 100 mg of material. Prior to its third touchdown, Hayabusa2 will release an impactor to theasteroid that will create a small crater, possibly exposing more pristine materials from beneath the surface from which sample
collection may be attempted. Each of the three samples may have different characteristics and they should be properly handled
to preserve them. Hayabusa2 Science Team will attempt to extract the gas sample before opening the pneumatically sealed
sample container. JSC will develop the gas sample curation and handling technique under our advanced curation activity [4].
References: [1] Watanabe S. et al. (2017) Space Science Reviews, 208, 3-16. [2] Lauretta D.S. et al. (2017) Space Science
Reviews, in press. [3] Righter et al. (2017) this volume. [4] McCubbin F.M et al. (2017) this volume.

Current status of developments by the collaboration team with ESCuC/JAXA for curation works
and analysis of Hayabusa2 returned samples
M. Uesugi1, M. Ito2, N. Tomioka2, K. Uesugi1, A. Yamaguchi3, N. Imae3, T. Ohigashi4, Y. Karouji5, T. Yada6, and M. Abe6,
Japan Synchrotron Radiation Research Institute (JASRI/SPring-8) (uesugi@spring8.or.jp), 2Japan Agency for Marine-Earth
Science and Technology (JAMSTEC), 3National Institute of Polar Research (NIPR), 4Institute for Molecular Science (IMS),
5
Tokyo Metropolitan University, 6Japan Aerospace Exploration Agency (JAXA).

1Extraterrestrial sample curation center (ESCuC) of Japan aerospace exploration agency (JAXA) organized a special team forthe development of techniques and devices for the handling, transfer and analysis of samples returned by Hayabusa2 spacecraft,from 2015 under the agreements of collaboration. The special team constitutes of members of institutes those having state-ofthe-art analytical instruments and experiences of curatorial works of precious natural samples, but beyond the specialists of theextraterrestrial materials. Through the collaboration, we can introduce latest specialties and knowledges from diverse scientificand technological fields into the processes of analysis of Hayabusa2 returned samples [1,2].
So far, we finished the development sample transfer container for the inter-institute transfer, even international transfer ofsamples, without contamination of terrestrial materials and sample damages such as breaking and sample lost. We also
evaluated the sealing performance of the container and confirmed that it has enough sealing performance against even positive
pressure inside the container. The container, named as Facility to Facility Transfer Container (FFTC), is already available
commercially.
Currently, the team members are working for (1) development of sample holders for the sample transfer in high cleanness
environment, (2) development of devices for the atmosphere shielding environment for the sample handling, (3) developmentof sample holders applicable for multiple analytical methods, and (4) development of techniques for the evaluation ofcleanness of those developed materials and environments. Although those devices and techniques are still under development,
we already applied them for the analysis of samples in each institute, and evaluated its applicability and problem for the
analysis of Hayabusa2 returned samples.
We also started development of new analytical protocols of extraterrestrial materials, which includes method of sample
transfer, sample separation and data sharing, through the rehearsals of the curation works for the initial description of
Hayabusa2-returned samples using extraterrestrial materials. Currently, 5 Antarctic micrometeorites provided by national
institute of polar research (NIPR) were imaged by synchrotron radiation computed tomography (SR-CT) and x-ray diffraction(XRD) at SPring-8, and investigated by high resolution field emission scanning electron microscopy and energy dispersive
spectroscopy (FE-SEM-EDS) system at institute for molecular sciences (IMS). Through the series of non-destructive analysis,
we selected Antarctic micrometeorites those having similar characteristics of carbonaceous chondrites, and formed thinsections by focused ion beam (FIB) for the characterization of organic materials by scanning transmitted x-ray microscopy andnear edge x-ray absorption fine structure analysis (STXM-NEXAFS) at IMS, high resolution analysis by transmission electron
microscopy (TEM), and isotopic analysis of light elements such as hydrogen, carbon, nitrogen and oxygen by secondary ion
mass spectrometry (SIMS) at Japan agency for marine-earth science and technology (JAMSTEC).
In order to make possible such large scale collaboration for the series of sample analysis between institutes, we need toevaluate sample damages and contaminations through the analysis, and develop the methods for cleaning of sample holder andprotocols for suppressing sample damages, as well as sample transfer system. Sample holders are already under theexamination. So we can start the evaluation of cleanness and development of method for the cleaning of them by ultrasoniccleaning and acid-alkali cleaning [3,4]. We will start the development in this year, and will report the result near future.
Thus progress of our development is going along quite smoothly. We can share the result of our development withpreliminary examination team of Hayabusa2 sample analysis organized by Hayabusa2 project, and can make their start process
faster.
In future work, we will develop the cutting method of samples with low-contamination processes, including sample
mounting devices and handling method after the cutting. In order to include rare and trace element analysis using laser ablationinductively coupled plasma mass spectrometry (LA-ICP-MS) in our protocol, we will also start the development of sample
holders and examination of it, in parallel with the rehearsals of the initial description of Hayabusa2 returned samples.
References[1] Web page: https://hayabusaao.isas.jaxa.jp/curation/release/index.html (Japanese) [2] Uesugi M. et al. 2016. Abstract#1129-1100. Haybusa symp. 2016. [3] Karouji et al., 2014. Chikyu kagaku 48:211-220 (Japanese) [4] Ishibashi Y., Karouji Y.,
Fujimura A., Yada T., Uesugi M., Yakame S., Okada T., and Abe M. 2012. Asteroids, Comets, Meteors, abstract #6492

Systematic detection of carbonaceous phases in chondrites –request for sophisticated techniques for Hayabusa 2 particle analyses
V.H. Hoffmann1,2, T. Mikouchi3, M. Kaliwoda4, R. Hochleitner4Fac. Geosciences, Dep. Geo- and Environmental Sciences, Univ. Munich, 2Dep. Geosciences, Univ. Tübingen, Germany;3
Dep. Earth Planet. Science, Univ. Tokyo, Japan; 4Mineralogical State Collection, Munich, Germany.

1

The Asteroid Explorer “Hayabusa 2” is the successor of “Hayabusa” (MUSES-C), which for the first time ever returned
pristine samples from an asteroid [1]. 25143 “Itokawa” is a small Near-Earth S-type asteroid consisting mainly of ordinarychondrite type material [2, and refs herein]. The mission was a major step towards further elucidating the origin and formationof our solar system. The “Hayabusa 2” mission, launched in 2014, will target another Near-Earth asteroid, namely 162173“Ryugu” (1999 JU3) which is a C-type asteroid. To learn more about the formation and evolution of our solar system,
investigating different types of asteroids, namely S-, C-, and D-type, is mandatory. C-type asteroids such as “Ryugu” areinterpreted as more primordial bodies than for example “Itokawa” and are considered to contain more carbonaceous, organic or
hydrated mineral phases. Spectroscopical data show that this asteroid type might be closely related to primitive carbonaceouschondrites or comets in terms of material composition [3].
Very sophisticated techniques are required for the investigation of pristine “Ryugu” particles in our laboratories (return planedend of 2020). LASER Micro Raman Spectroscopy is perfectly suited for identifying and discriminating (extra-) terrestrial
mineralogy: (a) fully non-destructive (repeated experiments possible on one and the same spot under variable conditions), (b)investigations with high sensitivity and in parallel high resolution, optionally in 3 dimensions, (c) as a major advantage
experiments on pristine material without any preparation or coating, and (d) mineral polytypes (eg diamonds) can be welldiscriminated. Variable LASER frequencies allow to optimize and fine-tune the Raman system to specific sample andexperiment requirements. High resolution scanning can produce very detailed distribution maps of selected mineral phases.
Micron- or even nano-sized particles such as various diamond polytypes can be detected in this way. Within our Hayabusa
sample analyses project we have successfully applied LASER Micro Raman Spectroscopy on several individual Itokawa
particles [2].
Generally, the carbon-phase mineralogy has not really been investigated systematically in most meteorite types [4,5]. The main
focus was on ureilites and certain carbonaceous chondrites [4-7], and priority was set on graphitic components and diamonds.
The presence of very rare carbonaceous phases such as graphenes, fullerenes or nanotubes which can be exspected in a numberof meteorite types has not been investigated to our best knowledge. Therefore we have started detailed and systematicinvestigations on the carbon-phase mineralogy of a larger set of various stony meteorite types. Priority is presently set on thefollowing selected recent falls and finds [8-13]: (a) Ordinary chondrites Machtenstein H5 (find around 1956, classified 2014),
Braunschweig L6 (fall 2013), Stubenberg LL6 (fall 2016), and for comparison the HED meteorite Saricicek (howardite fall2015) as well as a large series of Almahata Sitta individuals [polymict ureilite, 12,13 and refs]. In our poster we will present
first detailed results concerning the carbon phase mineralogy in these meteorites and will also focus on hypotheses concerning
the possible formation processes of the meteoritic micro-nano diamonds [6,7,14,15]: (a) Chemical Vapor Deposition (CVD)and (b) shock metamorphism as optional in situ diamond producing processes, and (c) presolar diamonds of extrasolar origin(eg from supernovae explosions).
References[1] http://global.jaxa.jp/projects/sat/hayabusa2/: last visit 9/2017.
[2] Mikouchi T. et al., 2014. Earth, Planets, Space, 66, pp82.
[3] Norton R.O., 2002. The Cambridge Encyclopedia of Meteorites. Cambridge Univ. Press.
[4] Ramdohr P., 1973. The opaque phases in stony meteorites. Elsevier, New York.
[5] Makjanic et al., 1993. Meteor. 28, 63-70.
[6] Szurgot M. et al., 2006. Nanodiam, PWN, Warszawa, pp259.
[7] Karczemska A.T., 2010. J. Achievm. Mater. Man. Engineer. 43/1, 94-107.
[8] https://www.lpi.usra.edu/meteor/metbull.php: last visit 9/2017.
[9] Hochleitner R. et al., 2015. LPSC #2453.
[10] Hochleitner R. et al., 2015. LPSC #1471.
[11] Bischoff A. et al., 2017. Meteor. Planet. Sci. 1-21, doi: 10.1111/maps.12883.
[12] Hoffmann et al., 2017. LPSC #2365.
[13] Hoffmann et al., 2017. Metsoc #6290.
[14] Gucsik et al., 2008. LPSC #1201.
[15] Hus G.R., 2005. Elements 1, pp97-100.

Preliminary results of Sulfur speciation by µ-XANES and STXM in Extraterrestrial Organics
Motoo Ito1, Ryoichi Nakada1, Hiroki Suga2, Takuji Ohigashi3, Yu Kodama4 and Hiroshi Naraoka5
1
Kochi Institute for Core Sample Research, JAMSTEC, 2Hiroshima University
3
UVSOR Synchrotron, Inst. Mol. Sci., 4Marine Works Japan, 5Kyushu University
Sulfur is one of the major elements in terrestiral and extraterrestrial organics. The elemental compositions of theMurchison IOM (insolble organic matter) are proposed to be C100H70O22N3S7 [1] or C100H48N1.8O12S2 [2]. Because sulfur
shows a wide range in oxidation state (-2 to +6) with both electropositive and electronegative elements, both reduced andoxidized sulfur species have been found in various carbonaceous chondrites [3, 4]. Therefore, understanding of speciation of
sulfur and its distribution within organics in a carbonaceous chondrite is crucial to provide the secondary alteration processesof thermal metamorphism and aqueous alteration in the parent body.
X-ray absorption near edge spectroscopy (XANES) is a powerful analytical tool to characterize and quantify chemical
speciation, functional group and bonding environment of the sample. In the field of cosmochemistry, many researches werecarried out to identify functional groups of C, N and O in extraterrestrial organics (i.e., IOM in carbonaceous chondrites [5],cometary returned sample [6], organics found in Hayabusa Category-3 grains [7], organics in IDPs [8]). However, sulfur
study with XANES in the extraterrestrial organics is very rare [3, 9].
In this study, we report preliminary results of sulfur speciation measurements by K- and L3-edge XANES of the IOM
extracted from Asuka 881458 CM2 carbonaceous chondrite. We carried out X-ray fluorescence (XRF) mapping for S and Nwith a spatial resolution of 20 µm in the IOM (0.8 x 1 mm2) at BL27SU of SPring-8. We, then, conducted µ-XAFS (sulfur
K-edge) measurements to acquire point spectra (#1-#6 in Fig. 1). In addition, we have measured carbon K-edge and sulfur
L3-edge XANES spectra in the FIB section of the AA881459 IOM (8 x 20 µm2) using scanning transmission X-ray microscope(STXM) at Inst. Mole Sci. UVSOR
42 8   45 2
18 .
82 4. 18 5 Figure 2. Possible sulfur components in the extractedorganics from A881458 obtained by K?edge spectrum.
  
.
84
BL4U.
Spot1#• 0.8"x"1"mm
Low
High
Spot2#
Figure 1 shows S and N• 37"x"51"pixels"(20"µm/pixel)
Spot3#
Spot4#
S&XRF"image
N&XRF"image
S
Spot5#XRF images together with optical
Optical"microscope"Image
Spot6##6#6
microscope image of the sample on#1#1
the Si wafer. The distributions of#5#5
S and N are similar but slightly#2 #3 #4
#2 #3 #4
different abundances. We used
these images to determine XANES
1"mm
analysis spots in the sample (about
20 µm in size, #1 to #6 in Figure 1).
Measured S K-edge XANES spectra (#1 to #6) have deconvoluted with a least- Figure'3.'Sulfur'L.edge'STXM'image'and'SIM'image'square linear combination best fits to reference spectra of S contained organic and Low&High&
FIB section image
inorganic compounds. Figure 2 shows a radar diagram of possible S components
and their abundances in each spot (#1-#6). Each spot has different sulfur containedorganics and inorganics and their abundances. This suggested that extraterrestrialorganics is a complex mixture of several types of sulfur species. Our result is
consistent with previous works [3, 9]. S L3-edge XANES spectra of several Scontained organics with different species (lauryl sulfate, sodium methanesulfonate,
9 µm
L-cysteic acid and DL-methionine sulfone) were obtained as references. Figure 3 S"STXM&
image&
shows high-resolution (50 nm) S L3-edge STXM image of the FIB section of theAA881459 IOM. It is noted that S is homogeneously distribute and tiny S hot spots were observed within the sample.
However, it is difficult to deconvolute the L3-edge spectra of the sample based on fitting by a linear combination of standard
materials spectra because of lack of the S L3-edge spectra for reference materials at this moment.
2

4!aminothiophenol#
Trimethylsulfonium# 15#
4!nitrobenzen#
Thianthrene#
Anthraquinone#

Sulfoxide#

Sulfonate#

13#
11#

Aroma9c!SH1#

CysAlaAla#9#

pyrrho9te#

Cys9ne#7#5#pyrite#Dibenzothiophene#

3#

Polyphenylenesulﬁde#Dibenzyl#disulﬁde#

1#

!1#

PhCH2SPh#

Dibenzyl#sulﬁde#Octoclothepin#

Dihydrodibenzothiopin#

Na9ve!S#Na2SO4#

Na2SO3#DL!Methionine#
Methylsulfonium#
Methionine#
Methanesulfonic#acid#

DL!methionine#sulfone#

Dothiepin#

gypsum#

HOPhSPhOH#
Lauryl#sulfate#
L!cysteic#acid#

References: [1] Remusat, 2011. EPJ Web of Conferences 18:05002. [2] Gilmour, 2005. In Meteorites, comets and planets,
Treatise on Geochemistry, p.269. [3] Orthous-Daunay et al. 2010. EPSL, 300, 321−328. [4] Cooper et al. 1997. Science, 277,
1072−1074. [5] Cody et al. 2011. Meteor Planet Sci 43:353–365. [6] Sanford et al. 2006. Science, 314:1720–1724. [7] Yabuta
et al. 2014. EPS, 66, 156. [8] Flynn et al. 2003. Geochim Cosmochim Acta, 67, 4791–4806. [9] Bose et al. (2017) Meteor
Planet Sci, 52, 546−559.

The evolution of water-rich asteroids: Linking the mineralogy and spectroscopy of fully hydrated
CM carbonaceous chondrites
Helena Bates1,2, Ashley King1, Kerri Donaldson Hanna2, Neil Bowles2 and Sara Russell1
1
Mineral and Planetary Sciences Division, Natural History Museum, London, SW7 5BD, UK
2
Atmospheric, Oceanic and Planetary Physics, University of Oxford, Oxford, OX1 3PU, UK
Introduction: The C-complex asteroids (which include B, C, F and G-types [1]) are of interest because they arethought to be volatile-rich, and may be able to tell us about the evolution of water and organic compounds in the early Solar
System. Additionally, C-complex asteroids likely made a significant contribution to the volatile budget of the terrestrial planets[2,3]. Carbonaceous chondrite meteorites are physical samples of C-complex asteroids; linking laboratory spectra ofcarbonaceous chondrites to remote sensing observations of asteroids can therefore give insight into the processes, which occur
on primitive bodies in the Solar System.
Spectrally, many C-complex asteroids show evidence for aqueous alteration and links with CM and CI carbonaceouschondrites on their surfaces [4–7]. Most spectral links have been between the C-complex asteroids and moderately altered
CM2 chondrites. Although there have been limited studies on the association of these asteroids with fully hydrated (“type 1”)chondrites, Clark et al. [8] suggested a possible relationship between more aqueously altered CM and/or CI chondrites and thesurface mineralogy of the B-type, OSIRIS-REx target asteroid, Bennu.
The CM1 chondrites are among the most hydrated extra-terrestrial materials available to study; their precursor
mineral assemblages have been almost entirely transformed into secondary, hydrated phases. King et al. [9] investigated
CM1 and CM1/2 chondrites with the aim of establishing modal mineralogy and examining variations in the extent of aqueousalteration. In this study we collected reflectance spectra from the same powders used by King et al. [9] so that any spectral
trends could be put into context of the mineralogy and degree of aqueous alteration for each meteorite sample.
Experimental: The suite of meteorites investigated included six CM1/2 chondrites and four CM1 chondrites.
Approximately 100 mg of each sample was ground into a fine powder using an agate mortar and pestle to a particle size of <35µm. Infrared reflectance spectra of the powders were obtained using a Bruker VERTEX 70v Fourier Transform Infrared(FTIR) spectrometer at the University of Oxford, using a wide range MIR-FIR beam splitter and a room temperature
deuterated L-alanine doped tryglycine sulfate (RT-DLaTGS) detector to measure the reflectance between 6000 - 200 cm-1 (1.750 µm). All observations were obtained under vacuum (~5 hPa), at a resolution of 4 cm-1. In order to remove instrumental
effects, spectra were calibrated by dividing each meteorite spectrum with a spectrum of a gold calibration target,
Results & Discussion: Initial observations of the mid-infrared spectra show samples, which are mostly composed ofhydrated minerals, particularly serpentine-group phyllosilicates. Upon further investigation of individual spectral regions - the
3 µm band, 6 µm band, Christiansen features (CF: 7.5-9.5 µm), and the transparency features (TF: 10.5-14 µm) - different
phyllosilicate compositions and abundances resulted in different, distinguishable spectral features.
The 3 µm band centres are affected by the Fe-cronstedtite abundances in the samples, with higher abundances shifting
the feature to longer wavelengths. The 6 µm band features appear to reflect the anhydrous silicate content, with greater band
depths for higher olivine contents. The CFs are identified at similar wavelength positions for all samples (8.8 - 8.9 µm)
suggesting the meteorites have similar bulk mineralogy. The TFs were affected by the total phyllosilicate abundance, withhigher abundances shifting the peaks to shorter wavelengths.
The above conclusions resulted in splitting the meteorites into two groups. Group A samples had larger 6 µm bandfeatures, a 3 µm band centre, and TF peak at longer wavelengths (~2.8 µm and ~12.5 µm respectively). Group B samples had
smaller 6 µm band features, a 3 µm band centre, and TF peak at shorter wavelengths (~2.7 µm and ~11.6 µm respectively).
Group A samples represent the least altered CM1/2s, which have significant Fe-cronstedtite abundances of 30.8 –
36.9% and anhydrous olivine abundances of 18.2 – 19.6%. Group B samples represent the most altered CM1s, which havesignificant Mg-serpentine (52.4 – 71.6%) and low olivine abundances (3.6 – 8.0%). This study shows that slight variations inaqueous alteration might be discernible in current and future telescopic and space mission observations of C-complex asteroids.
References: [1] Tholen, D.J., 1984. [2] Alexander, D. et al., 2012 Science, 721. [3] Alexander, C.M.O., 2017
Philosophical Transactions of the Royal Society, 375. [4] Fornasier, S. et al., 1999 Astron. Astrophys. Suppl. Ser, 135:65. [5]Ziffer, J. et al., 2011 Icarus, 213: 538. [6] Cloutis, E.A. et al., 2011 Icarus, 216:309. [7] Takir, D. et al., 2015 Icarus, 257:185.
[8] Clark, B.E. et al., 2011 Icarus, 216:, 462. [9] King, A.J., P.F. Schofield, S.S. Russell, 2017 Meteoritics & Planetary
Science, 52:1197.

Current status of consortium study of silica-containing Hayabusa-returned particle.
M. Hashiguchi1, A. Miyake2, A. Tsuchiyama2, T. Nakamura3, M. Uesugi4, J. Matsuno2, A. Nakato2, T. Yada5, M.
Yoshitake5, T. Okada5, M. Abe5, and H. Yurimoto5, 6.
1
PTOC, Kyushu University (hashiguchi.minako.123@m.kyushu-u.ac.jp), 2Department of Geology and Mineralogy, Graduate School of Science, Kyoto University, 3Department of Earth Science, Tohoku University, 4 JASRI,
SPring-8, 5 ASRG, JAXA, 6 Natural History Sciences, Hokkaido University.
Introduction: About 730 particles of Hayabusa-returned sample of 10 to 300 µm size are collected by Extraterrestrial Sample Curation Center (ESCuC) in Astromaterials Science Research Group (ASRG) of JAXA, so far[1]. The preliminary examinations and international AOs revealed that Itokawa particles were equivalent toequilibrated LL chondrites [e.g. 2-10]. Some of the Hayabusa-returned particles show unique characteristics including mineralogy, composition, structure, and/or size. Therefore, consortium studies have been conducted byteam of ESCuC in order to obtain maximum scientific results from such particles [11-13].
We proposed a new consortium study of particle RB-QD04-0069 containing silica [14]. This is the only particle which contains silica coexist with other silicate minerals among catalogued Hayabusa-returned samples, sofar. Silica is widespread in ordinary chondrites, but its abundance is very low (usually < ~1 vol %) [15]. Therefore, the particle RB-QD04-0069 is precious and it should be investigated as consortium study. Evidence ofshock processes have been revealed from Hayabusa-returned particles by previous studies and shock and/or
thermal history of the particles were discussed [2, 8-10]. Because silica has many polymorph, it should be usefulindicator to constrain thermal and/or shock history of the particle [16]. In this paper, we report current status of
the consortium study of particle RB-QD04-0069.
Sample and Analytical flows: RB-QD04-0069 is a particle with a size of 33 µm, which was captured from thefirst touchdown site on Itokawa. The particle consists of olivine, high-Ca pyroxene, low-Ca pyroxene, plagioclase, and silica revealed by initial description by FE-SEM-EDS.
The XRD analysis will provide us crystallographic information of silica and other silicate minerals. Moreover, textural information of the particle will be obtained by the SR XCT imaging. After the synchrotron radiation
analyses, the particle will be embedded in epoxy resin EPON-812, followed by polishing until the surface of theparticle is exposed. Then, oxygen isotope compositions will be measured by SIMS in order to identify the originof the particle. Furthermore, FE-EMPA analysis and TEM observations will be carried out on the particle to obtain important constraints on formation condition of the particle, especially its shock and thermal history.
Current status: The particle RB-QD04-0069 was picked up from a slide glass in pure nitrogen-filled environment clean chamber in ESCuC by quartz glass probe using manipulator system last year. Then, the particle wastried to attach to the top of C fiber with epoxy resin Embed-812 using manipulator system in a clean booth at
ESCuC for Synchrotron radiation (SR) XRD analysis and SR XCT imaging. However, during the procedure, theparticle RB-QD04-0069 was failed to attach to C fiber and fell down on the slide glass or Al foil on heater used
for the handling.
By optical microscope and SEM-EDS analysis, three candidate particles were found from Al foil on theheater. We plan to analyze these candidate particles by detailed FESEM-EDS to narrow down the candidates.
Then, the surrounding region (Al foil) of the candidates will be cut by FIB at Kyoto University and attach themto C fiber using Pt depo for SR-XRD and XCT analysis to identify true particle using characteristics of silica,
olivine, pyroxene, and plagioclase.
References: [1] Yada T. et al. (2017) 80th MetSoc, #6204. [2] Nakamura T. et al. (2011) Science 333, 1113.
[3] Yurimoto H. et al. (2011) Science 333, 1116. [4] Ebihara M. et al. (2011) Science 333, 1119. [5] Noguchi T.
et al. (2011) Science 333, 1121. [6] Tsuchiyama A. et al. (2011) Science 333, 1125. [7] Nagao K. et al. (2011)
Science 333, 1128. [8] Zolensky M. et al. (2012) LPS XLIII #1477. [9] Mikouchi T. et al. (2014), EPS, 66, 82[10] Harries D. et al. (2016) EPSL, 337. [11] Yada T. et al. (2014) LPS XLIV #1759. [12] Uesugi M. et al.
(2014) 77th Ann. Meeting Meteorit. Soc., #5226. [13] Karouji Y. et al. (2014) 77th Ann. Meeting Meteorit. Soc.,#5240. [14] Hashiguchi M. et al. (2015) 78th MetSoc, #5193. [15] Hezel D. et al. (2006) GCA, 70, 1548. [16]Swamy V. et al., (1994) J. Geophys. Research. 99, 787.