Hayabusa 2021 Symposium Schedule (Online Meeting)(8th ISAS Symposium of the Solar System Materials )16th(Tue)‐17th(Wed) of November 2021

version. 20211111

Oral : Zoom Meeting (10+5 min for Invited and normal talks, 7+3 min for 10 min short talks)
Poster : Zoom Meeting Breakout Rooms
Non‐real time discussion : Slack
Day‐1 (Nov 16th) : Poster Session
JST

GMT

EST

PST

No.

Title
Poster Session and chat (2 hours)

19:15

10:15

05:15

02:15

:

Author/Presenter

R. Fukai, T. Hayashi

P‐1

The fundamental deformation of cosmic bodies not depending of their sizes and compositions(from asteroids to Universe)

Gennady Gregory Kochemasov

P‐2

Exogenous copper sulfide in a returned grain from asteroid Itokawa

Katherine D Burgess

P‐3

A Series of Recent Falls of Carbonaceous Chondrites ‐ Perfect Analogues for Returned Hayabusa 2 and Osiris Rex Asteroidal Materials

Viktor H Hoffmann

P‐4

Heated Synthetic Murchison Reflectance Spectra

Sahejpal Sidhu

P‐5

Status of the Curatorial Database System for the Ryugu Samples

Masahiro Nishimura

P‐6

Methodology of MicrOmega data acquisition/processing in initial description of Ryugu returned samples

Kasumi Yogata

P‐7Comparison of ion‐ and laser‐weathered spectra of olivines and pyroxenesKateřina Chrbolková

P‐8

Solid Materials of Mineral and Rock on the Solar System: X‐ray Unit and Mixed Status

Yasunori Miura

P‐9Model of Material Characteristics of Carbonaceous Meteorites from Texture of Carbon‐Bearing Grains

Yasunori Miura

P‐10

Neural network for classification of asteroid spectraDavid Korda

P‐11

Assessment of organic, inorganic, and microbial contamination in the facilities of the Extraterrestrial Sample Curation Center of JAXA

Yuya Hitomi

InvitedThe fundamental deformation of cosmic bodies not depending of their sizes and compositions (fromasteroids to Universe)
Kochemasov G. G. IGEM RAS,Moscow,kochem.36@mail.ru
Abstract: Orbits make structures. Not depending sizes and compositions of celestial bodies they acquire
tectonic dichotomy (two hemispheres) connected with warping action of fundamental wave.
Keywords; cosmic bodies. orbits, galaxies, planets, satellites, asteroids, fundamental wave
The main point of the wave planetology is: “Orbits make structures”. It means that movement in nonround orbits makes waves creating structures (Fig. 1-10) However, any cosmic body moves in several
orbits. They all participate in structuring [1]. Their frequencies are divided and multiplied creating new
frequencies and corresponding them structures. They are (frequencies) very small and very big. Veryslow but very energetic rotation of large cosmic formations (galaxies and the larger assemblies) makevery fine oscillations up to microwaves, roentgen and gamma radiations infilling cosmos. From theother end, oscillations passed through fundamental wave and corresponding it tectonic dichotomy ofany body. In figures are examples of bodies of various sizes from the Galaxy to small asteroids (Fig.1-8)
The row is finished with small asteroids Itokawa and Ryugu. Both reveal tectonic dichotomy;
especially sharp in Itokawa with its convexo-concave shape. Ryugu has unique longitudinal variation ingeomorphology: the western side of it has a smooth surface and a sharp equatorial ridge (bulge) [3]. On
the opposite side Fossae Tokoyo and Horai occur. Some peculiarities show crater distribution (morethan 20 meters in diameter). There are fewer craters in the western bulge and more around themeridian. This cannot be explained by the randomness of cratering [2].
The other end of this row include giant cosmic formations like galaxies and larger ones finishing atUniverse. The Universe also is dichotomist divided at uplifted and subsided halves. The humankind
occupies the uplifted halve-in the religious sense “paradise”, the subsided halve thus is “hell”.

1

2Fig, 1. A spiral Galaxy. ESO 510-613. PIA04213.
Fig.2. PIA22113.Coronal hole all spread out.

3
Fig. 3. PIA23356. NASA’s AIRS maps carbon monoxide from Brazil fires.

4

Fig. 4. PIA14011. Moon’s nearside

5

6

Fig. 5. Asteroid Eros. Convexo-concave shape.
Fig. 6. Asteroid Itokawa. Convexo-concave shape.

78Fig. 7. Asteroid Ryugu. Ab278776d6ce43e581d669ef938497fa.jpg
Fig. 8. Asteroid Ryugu. Dichotomy shows.image_5c91c15458e6c0.69646182.jpg

9

10

Fig.9, 10. Fundamental wave in line and circle.
Referencs:[1] Kochemasov G.G. Modulated wave frequencies in the Solar system and Universe // Journalof Physics and Application 12(4): 68-75, 2018. Doi:10.13189/ujpa.2018.120402.
[2 ] N.Hirata, T. Morota, Y.Cho et al. The spatial distribution of impact craters on Ryugu// Icarus , v.338,
1, March 2020, 113527, httys:// doi.org/10.1016/j.icarus.2019.113527[3] ] H. Masatoshi, T. Eri, M. Hideaki et al. The western Bulge of 162173Ryugu formed as a result of arotationally driven deformation process // The Astronomical Journal: journal-IOP Publishing, 2019March (vol.874, #1-P. L10.-ISSN 0004-637X-doi:10.3847/2041-8213/ab0e8b-Bibcode:
2019ApJ…874L.10N-arXiv:1904.03480.

Exogenous copper sulfide in a returned grain from asteroid Itokawa
K. D. Burgess and R. M. Stroud
U.S. Naval Research Laboratory, Washington, DC 20375
Asteroid 25143 Itokawa is an S-type asteroid, and the returned samples are dominated by equilibrated, weakly shocked LL5
and LL6 ordinary chondrite material with some weakly equilibrated LL4 material [1,2]. We present evidence of the presenceof a cubanite-chalcopyrite-pyrrhotite-troilite assemblage consistent with low-temperature aqueous alteration in a particle from
Itokawa [3]. Most of the materials from Itokawa equilibrated at temperatures near 800°C, with slow cooling to ~600°C [2,4],
which indicates this sulfide assemblage must have become part of Itokawa after thermal alteration. Cu-bearing sulfides havebeen reported in only a few meteorite types [5,6], which suggests the conditions necessary to form such phases occur on only alimited number of planetary bodies. Specifically, cubanite has only been reported in CI chondrites and Wild2 material [7].
Thus, we conclude that this grain, and the other Cu-sulfides noted on Itokawa samples [8] likely originated on a primitive,
hydrated asteroid source such as CI chondrite-like parent body or D- or P-type asteroids previously linked to unique, aqueously
altered meteorites [9,10].
Particle RB-CV-0038 (C0038) was mounted in epoxy such that most of the grain was available for imaging, then coated by 80
nm of evaporated carbon. SEM images and FIB samples were obtained with an FEI Helios G3 equipped with an Oxford 150
mm2 SDD energy dispersive X-ray spectrometer (EDS). After imaging, protective straps of C were deposited on regions ofinterest, and multiple sections suitable for STEM analysis were extracted using standard techniques. One section, known from
SEM-EDS to contain Cu, was attached to a Mo grid. STEM analysis was performed with the Nion UltraSTEM200-X at NRL.
The microscope is equipped with a Gatan Enfinium ER spectrometer for electron energy loss spectroscopy (EELS) and awindowless, 0.7 sr Bruker SDD-EDS detector. Selected area diffraction patterns were collected using a JEOL 2200FS. Data
were collected at 200 kV.

Figure 1. (a,b) Secondary electron (SE) images of particle RB-CV-0038 showing location of cubanite with Fe-sulfide and approximate
location of FIB section. (c) HAADF montage of FIB section with cubnaite (cb), troilite-cubanite-chalcopyrite (tr+cb+cp) mottled region, andpyrrhotite (4C-po) with “flame” texture.

C0038 is a multiphase grain, ~40 µm across. The particle is predominantly composed of olivine and iron sulfide with minor(adhered?) plagioclase or glass (Fig. 1a). A ~2×5 µm cubanite grain was present in contact with the Fe-sulfide (Fig. 1b). STEM
data show several different grains are present within the Fe-sulfide in the FIB section (Fig. 1c). The Cu-Fe-sulfide contains
several cracks are, one of which is perpendicular to the FIB section (Fig. 2a). The crack has oxidized Fe-rich edges and isdecorated by Cu metal nanoparticles. The cubanite itself shows a tripling of the c axis, apparent in SAED patterns (Fig. 2b).
Adjacent to the cubanite, the sulfide has a mottled texture (Fig. 2a), and a small amount of Cu is present (~2 at%), concentrated
in the bright spots. SAED patterns from the region index to troilite with faint chalcopyrite spots (Fig. 2d). Further from thechalcopyrite, there is no Cu, and the Fe-sulfide has a “flame” exsolution texture of two types of pyrrhotite (Fig. 2c). The
pyrrhotite can be indexed to 4C-pyrrhotite. The average measured Fe/S composition for the grain (x = ~0.09 in Fe1-xS) is
consistent with a 4C-pyrrhotite or a mixture of 4C and NC-pyrrhotites. In NC-pyrrhotites, NC indicates a variable, non-integral
superstructure based on the NiAs-type unit cell where troilite is 2C.

Figure 2. (a,c) HAADF images of cubanite, mottled Fe-sulfide, and pyrrhotite with flame texture. (b) SAED pattern for the cubanite, whichshows a tripling of the c axis. (d) SAED pattern for the mottled Fe-sulfide, which has ~2 at% Cu and shows reflections for cubanite andchalcopyrite in addition to troilite.

The presence of cubanite, which forms and is stable only at temperatures below ~250°C [11], together in this grain with 4Cpyrrhotite [7], indicates that this grain must have been brought to Itokawa after thermal alteration and equilibration of the LLtype material. This combination of sulfide phases has previously been identified only in CI chondrite material [7]. However,unlike CI chondrites, no Ni was detected in these sulfides. This could indicate variation in the CI parent body, or that the
impactor seen here was from a different parent body, such as the aqueously altered D- or P-type asteroids.
Acknowledgements
The authors thank JAXA and the Hayabusa curation team for access to the samples. Funding was provided by NASA LARS
award 80HQTR20T0050 and NNH17AE44I to RMS.
References[1] Mikouchi, T., et al. (2014) Earth, Planets and Space, 66, 82. [2] Noguchi, T., et al. (2011) Science, 333, 1121. [3] Burgess,
K.D., and Stroud, R.M. (2021) Communications Earth & Environment, 2, 115. [4] Harries, D., and Langenhorst, F. (2018)
Geochimica et Cosmochimica Acta, 222, 53. [5] Rubin, A.E. (1997) Meteoritics & Planetary Science, 32, 231. [6] Rubin, A.E.,
and Ma, C. (2017) Geochemistry, 77, 325. [7] Berger, E.L., et al. (2011) Geochimica et Cosmochimica Acta, 75, 3501. [8]Nakamura, E., et al. (2012) Proceedings of the National Academy of Sciences of the United States of America, 109, E624. [9]Brown, P.G., et al. (2000) Science, 290, 320. [10] Kebukawa, Y., et al. (2019) Scientific Reports, 9, 3169. [11] Dutrizac, J.
(1976) The Canadian Mineralogist, 14, 172.

A Series of Recent Falls of Carbonaceous Chondrites - Perfect Analogues for Returned
Hayabusa 2 and Osiris Rex Asteroidal Materials
V.H. Hoffmann1, K. Wimmer2, M. Kaliwoda1,3, W. Schmahl1,3, P. Schmitt-Kopplin4. 1Faculty of Geosciences, Dep. Earthand Environmental Sciences, Univ. Munich; 2Nördlingen; 3Mineralogical State Collection Munich, SNSB; 4Helmholtz-Center,
Munich; Germany.
Introduction
In recent years, a series of meteorite falls have been reported which produced various types of primitive chondrites. In ourcontribution we will focus on samples of the following witnessed falls: Flensburg (2019), Kolang and Tarda (both 2020), while
Mukundpura (fall 2017) was topic of our earlier studies [1-3]. These meteorites belong to the class of carbonaceous chondrites
and play a prominent role in terms of the Hayabusa 2 (successful sample return from asteroid Ryugu in December 2020) andOsiris Rex (sample return from asteroid Bennu planned in 2023) missions [4,5] Both probed asteroids belong to the C typeasteroids and are believed to mainly consist of carbon rich materials with a similar composition as primitive chondrites.
The Flensburg meteorite fell in September 2019 in Northern Germany and was classified as a C1 ungrouped carbonaceouschondrite, the first reported fall of this type. Only one small stone was found so far (24.5 gr). For all further details we refer to[2]. The Tarda meteorite fall was reported from Southern Morocco in august 2020, the meteorite (about 4 kg total mass) wasclassified as a C2 ungrouped carbonaceous chondrite [1,2,6,7]. Only four witnessed falls of this type are known, whereby
Tagish Lake is probably the most famous one (fall 2000, [1]). The Kolang meteorite fireball and fall was reportedly observedin Indonesia in august 2020 (four stones with a total mass of 2550 gr). Kolang was classified as a CM 1/2 chondrite and is thefirst and only witnessed fall known from this meteorite group [8,9].
In our contribution (poster) we will compile our earlier and provide new results of detailed and systematic investigations on themineral phase composition and distribution of three new meteorite falls [10,11]. Our focus was mainly on the rare/accessory
mineralogical components of these meteorites. Specifically we are interested on the carbon-bearing and the magnetic phases.
Several unprepared fragments and one individual of Tarda were used for our studies, and additionally one small unpreparedfragment of Kolang. Concerning Flensburg, we had a small fragment and a PTS (provided by A. Bischoff, Univ. Münster). We
used optical microscopy, LASER Micro Raman Spectroscopy (Horiba XploRa Raman System, MSM/ SNSB) for our study
which is perfectly suited for identifying and mapping minor/accessory phases. Being fully non-destructive, allowing highresolution mapping on natural, broken surfaces without any preparation in 2D or 3D are some of the major advantages of thistechnique. The surface morphology and mineralogy of the uncoated samples was investigated using a Phenom ProX scanningelectron microscope (SEM) in backscattered electron mode equipped with an energy dispersive X-ray spectrometer (EDS) foranalyzing the element composition. Magnetic susceptibility was investigated systematically by an SM30 (Hulka Comp., CR).
The results of our Raman spectroscopy experiments on Kolang have to be seen as preliminary as we had only one small
fragment for our project. Generally, performing successful LASER Raman experiments on carbonaceous chondrites, here
specifically on Flensburg, Tarda and Kolang, required the design of a highly sophisticated experimental setup to avoid or atleast minimize alteration effects already during the measurements on the one hand and to guarantee a reasonable signal/noise
relationship on the other. Due to the significant brecciation and very fine grained matrix / phases, experiments on Kolang arequite complex. Generally, several phases which have been detected in these primitive carbonaceous chondrites are extremely
sensitive against (even minor) heating effects, and therefore any kind of preparation (cutting/grinding etc.), specifically interrestrial atmospheric conditions has to be minimized. In order to avoid any such effects we decided to investigate only
naturally broken unprepared sample materials (PTS of Flensburg is a necessary exception because of representativity but wealso had a fragment). The representativity of the data obtained on the available sample material was also topic of our studies:large sets of high resolution mappings in 2D/3D can help to overcome the problem of tiny samples / fragments. Our
experiences from the earlier investigations on Hayabusa 1 materials (asteroid Itokawa) were highly profitable in this context[12-14].
Consequently, our main interests were on optimizing and fine tuning our experimental setup. So the series of recent meteorite
falls which produced a new set of primitive carbonaceous chondrites provided us directly with unique fresh analogue materials
for Hayabusa 2 and Bennu asteroidal samples in our laboratories. We plan to extend our investigations in near future to
additional recent falls such as Aquas Zarcas (2019, Costa Rica, CM2) or most recently Winchcombe (2021, England/UK,
CM2) [1,3].

References[1] Meteor. Bull. Database 10/2021: Flensburg , Tarda, Kolang, Aquas Zarcas, Winchcombe, Mukundpura, Tagish Lake.
[2] Bischoff A. et al., 2021. The old, unique C1 chondrite Flensburg – Insight into the rst processes of aqueous alteration,
brecciation, and the diversity of water-bearing parent bodies and lithologies. Geochem. Cosmochem. Acta, 293, 142-186.
[3] https://www.karmaka.de (10/2021)[4] Hayabusa 2 mission to asteroid Ryugu (finished 12/2020), JAXA: https://www.hayabusa2.jaxa.jp/en/[5] Osiris Rex mission to asteroid Bennu, NASA: https://www.nasa.gov/osiris-rex[6] Chennaoui H.A., et al., 2021. Tarda (C2-ung): a new and unusual carbonaceous chondrite meteorite fall from Morocco.
52nd LPSC 2021, #1928.
[7] Dey S., et al., 2021. Exploring the planetary genealogy of Tarda – a unique new carbonaceous chondrite. 52nd LPSC 2021,# 2517.
[8] King A.J., et al., 2021. The bulk mineralogy and water contents of the carbonaceous chondrite falls Kolang and Tarda. 52nd
LPSC 2021, #1909.
[9] Jenkins L.E., et al., 2021. Identification of clasts in CM chondrite fall Kolang with S and Ca. 84th Meteor. Soc. Conf.,#6161.
[10] Hoffmann V., et al., 2021. The Kolang (CM1/2) and Tarda (C2 ungrouped) meteorite falls from 2020: first systematic
mineralogical investigations by LASER Raman spectroscopy and SEM/EDX. 52nd LPSC 2021, # 2458.
[11] Hoffmann V., et al., 2021. The Flensburg (C1 ungrouped) 2019 meteorite fall: Raman spectroscopy and compilation ofmagnetic susceptibility data on C-ungrouped falls/finds. 52nd LPSC 2021, # 2443.
[12] Mikouchi T., Hoffmann V.H. et. al., 2014. Mineralogy and crystallography of some Itokawa particles returned by the
Hayabusa mission. LPSC 2021, #2239.
[13] Mikouchi T., Hoffmann V.H., et al., 2013. Mineralogy and crystallography of Itokawa particles by electron beam andsynchrotron radiation X-ray analyses. Hayabusa Conf. 2013.
[14] Mikouchi T. and Hayabusa Consortium, 2014. Mineralogy and crystallography of some Itokawa particles returned by the
Hayabusa asteroidal sample return mission. Earth, Planets and Space, 66/82, 9pp.

Heated Synthetic Murchison Reflectance Spectra

1

S. Sidhu1, P. Mann2 and E. Cloutis1
Centre for Terrestrial and Planetary Exploration (C-TAPE), The University of Winnipeg
2
Department of Geography, The University of Winnipeg

Introduction: Several carbonaceous chondrites (CCs) display evidence of thermal alteration [1]. Remote sensing data from the
JAXA Hayabusa2 asteroid sample return mission suggests that asteroid (162173) Ryugu’s parent body may have undergoneinternal or impact-generated heating prior to breakup [2]. Furthermore, models of orbital and thermal evolution of Ryugu suggestthat the asteroid was likely exposed to surficial heating during close passes to the Sun. [3]. Recently, geomorphological features
observed on Bennu’s surface indicate alteration of rocks due to thermal fatigue [4]. Constraining the spectral characteristics ofheating will aid in identifying the timing and intensity of heating experienced by Ryugu and its parent body, as well as otherextraterrestrial bodies which may have also undergone a period of thermal alteration.
Methods: The Centre for Terrestrial and Planetary Exploration (C-TAPE) at the University of Winnipeg conducted aheating experiment on a synthetic Murchison simulant. The synthetic mixture, named WMM, consisted of various major
representative phases in CM carbonaceous chondrites as following: 85 wt. % ASB267, a dark serpentinite representative of CM
phyllosilicates. 5 wt. % SHU102, shungite, terrestrial organic representative of organic phases. 5 wt. % TRO203, synthetic
troilite representative of sulfides, and 5 wt. % MAG200, magnetite. The simulant consisted of <63 µm powders of serpentinite,shungite, and troilite, and ~20 nm sized magnetite that appeared to be maghemite from X-ray diffractometry (likely due to surface
oxidation of the nanoparticles). The samples were heated up to 1200qC at 100qC increments. XRD and reflectance spectra werecollected prior to heating, and after each temperature increment. A new sample powder was used for each increment, and samples
were heated under continuous nitrogen flow. Samples were heated for one week at intervals of 100qC to 1000qC. However, due
to the oven’s constraints, samples were only heated for 2 hours at 1100qC and half an hour at 1200qC. The reflectance spectrum
for 300qC is unavailable due to an accidental sample spill while removing the powder from the oven. The spectra were collectedwith an Analytical Spectral Devices (Boulder, CO) LabSpec 4 Hi-Res® spectrophotometer between 350 and 2500 nm. Spectra
were measured at a viewing geometry of i = 30º and e = 0º with incident light being provided by an in-house 150 W quartztungsten-halogen collimated light source. Sample spectra were measured relative to a Labsphere Spectralon ® 100% diffuse
reflectance standard and corrected for minor (less than ~2%) irregularities in its absolute reflectance.
Results: Heating the Murchison simulant samples resulted in spectral variation across the temperature increments. The
spectra show little change up to ~500qC (Figure 1). Beyond 500qC, the spectra display features associated with Fe3+
oxyhydroxides, such as low reflectance below ~500nm, a steep red slope in the visible region, and absorption features near 870
nm. Absorption bands associated with serpentine, at 1400 and 2320 nm, are evident up to ~600-700qC. The spectra generally
become brighter up to ~800qC, and then darken substantially beyond this temperature. At and above 1100qC, the spectra are
generally dark and featureless, with a broad absorption region centered near 1600 nm.
1Absolute Reflectance

0.8
0.6
0.4
0.2
0
300

800
Before Heating
500°C
900°C
Figure 1.

100°C
600°C
1000°C

1300
1800
Wavelength (nm)
200°C
700°C
1100°C

Reflectance Spectra of Simulated Murchison Mixture WMM.

2300
400°C
800°C
1200°C

Additionally, we heated end members used to produce the Murchison simulant to better understand the causes of thespectral changes observed. These samples (serpentine, shungite, troilite, and magnetite) were heated under the same conditions
as the simulant. Serpentine spectra remained unchanged up to ~200qC, after which the spectra display an increasing red slope
below ~700 nm and an absorption feature near 860 nm, both of which are ascribed to Fe3+ oxyhydroxides. Furthermore, theOH absorption bands near 1400 and 2320 nm associated with serpentine were evident up to ~700qC. Reflectance generally
increased up to ~600qC, and decreased at higher temperatures. Shungite was stable up to ~500qC. However, at 600qC, theorganic component of the sample was volatilized. Troilite remained stable up to ~300qC, after which Fe3+ oxyhydroxides were
evident in its spectra. Fine-grained magnetite remained stable up to ~100qC, after which it also transformed to Fe3+
oxyhydroxides.
Discussion: Temperature-induced spectral changes are evident in the Murchison simulant used in this study. XRD
measurements confirm that the changes seen in the spectra can be related to the changes in the mineralogy of the samples. The
spectral changes occur in multiple wavelength regions, suggesting that various spectral metrics could be robust indicators oftemperatures experienced by a serpentine-rich carbonaceous chondrite.
Spectral changes observed in this study are associated with short heating periods (hours to days), and are thus,
applicable to short-term heating events such as impact heating. The applicability of these results to long-term heating events,
such as internal heating within larger asteroids, is unknown. Furthermore, the dry nitrogen environment under which thisheating experiment was conducted only represents one scenario of the conditions which may have prevailed on carbonaceouschondrite parent bodies during any heating events. Nevertheless, the results of our experiments suggest that spectroscopic datain the 350-2500 nm can provide insights into the intensity and duration of heating events affecting carbonaceous chondrite
asteroids. It is also worth noting that naturally-heated carbonaceous chondrites show spectral differences associated withchanges in mineralogy [1]. We are in the process of relating the results of these experiments to other carbonaceous chondrite
heating experiments [5, 6, 7, 8] and naturally-heated carbonaceous chondrites [9] to better understand the full applicability of
our results to observational data.
References[1] Cloutis E. et al. 2012. Icarus 220:586-617. [2] Sugita S. et al. 2019. Science 6437:252. [3] Michel P. & Delbo M. 2010.
Icarus 209:520-534. [4] Molaro J.L. et al. 2020. Nature Communications 11:2913. [5] Hiroi T. et al. 1993. Science 261:10161018. [6] Hiroi T. et al. 1993. Symposium on Antarctic Meteorites 18:93-96. [7] Hiroi T. et al. 1994. Proceedings of the NIPR
Symposium on Antarctic Meteorites 7:230-243. [8] Hiroi T. et al. 1996. Meteoritics and Planetary Science 31:321-327. [9]Hiroi T. et al. 1997. Lunar and Planetary Science Conference 28:577-578.

Status of the Curatorial Database System for the Ryugu Samples
M. Nishimura1, T. Yada1, M. Abe1, A. Nakato1, K. Yogata1, A. Miyazaki1, K. Kumagai2, K. Hatakeda2,
T. Okada1, Y. Hitomi2, H. Soejima2, K. Nagashima1, T. Usui1, and S. Tachibana1,3
1Inst. Space Astronaut. Sci. (ISAS), Japan Aerosp. Explor. Agency (JAXA), Kanagawa 252-5210, Japan(nishimura.masahiro2@jaxa.jp), Japan, 2Marine Works Japan Ltd., Yokosuka 237-0063, Japan, 3UTOPS, Grad. Sch. Sci.,
Univ. Tokyo, Tokyo 113-0033

The JAXA’s Hayabusa2 spacecraft explored C-type near-Earth asteroid (162173) Ryugu and successfully returned its
reentry capsule on December 6, 2020. Particles exceeding ~5 grams in total were safely extracted from two sample chambersin the clean chamber system dedicated to Ryugu samples [1, 2]. After a six-month preliminary examination without exposure
to the air by the JAXA Astromaterials Research Group (ASRG), a part of Ryugu samples have been studied by the initial
analysis team led by the Hayabusa2 project [3]. Some samples have also been characterized by Phase-2 curation teams outside
ASRG [4]. The rest of the samples are continued to be investigated in the clean chamber to be catalogued in a curatorial
database system for Ryugu samples (Ryugu DBS), which will be archived to the community in early 2022 for theannouncement of opportunity (AO). In this presentation, we report the aim and features of the Ryugu DBS.
The Ryugu DBS has been designed and built to provide the Ryugu sample catalog with the research community andto help the researchers make the sample request through the announcement of opportunity.
The concept design of the Ryugu DBS was made in md 2019 based on lessons-learned from the operation of DBS for Itokawa
samples (Itokawa DBS) [5]. A mockup was first made to check the web interface and the user-friendliness of the system inearly 2020. The database system was then developed based on the feedback from the mockup review in Oct. 2020. The system
has been used by limited members for further feedback, major updates were made, and a supplemental system such as a data
input system was also developed. The Ryugu DBS is run using opensource technologies, such as PHP, PostgreSQL, andApache, and data servers on Data ARchives and Transmission System (DARTS) at ISAS/JAXA.
The Ryugu DBS provides the information on each individual grain (typically larger than 1 mm along the longest
dimension) and on aggregate samples. Because of the presence of large amount of fine particles (relative to Itokawa particles),fine grains are planned to be examined as an aggregate sample put in a single dish. The basic information listed in the DBS
includes photomicrographs, weight, size, and spectroscopic data, all of which are obtained in the clean chamber system
without exposure to the air. The spectroscopic data can be downloaded with the CSV format. Along with such basic
information, the analysis history and data obtained in previous analysis can also be found for each sample. The data obtainedby the project-led initial analysis and that from curation work outside JAXA will also be archived in the future.
The release of the Ryugu DBS to the community will be in early 2022.
References[1] Tachibana S. et al. (2021) LPS, XXXXXII, Abstract #1289. [2] Yada T. et al. (2021) LPS, XXXXXII, Abstract #2008. [3]Tachibana S. et al. (2021) submitting for Hayabusa 2021 symposium. [4] Ito M. et al. (2021) submitting for Hayabusa 2021
symposium. [5] Uesugi M et al. (2016) Journal of Space Science Informatics Japan: Vol 5, 59-70.

Fig. 1. The interface of the Ryugu DBS.

Methodology of MicrOmega data acquisition/processing in initial description of
Ryugu returned samples
Kasumi Yogata1, Tatsuaki Okada1,2, Kentaro Hatakeda1,3, Toru Yada1, Masahiro Nishimura1, Aiko Nakato1, Akiko Miyazaki1,
Kazuya Kumagai1,3, Yuya Hitomi1,3, Hiromichi Soejima1,3, Kana Nagashima1, Ritsuko Sawada1,3, Shogo Tachibana1,2,
Masanao Abe1,4, Tomohiro Usui1, Jean-Pierre Bibring5, Cedric Pilorget5, Vincent Hamm5, Rosario Brunetto5, Damien
Loizeau5, Lucie Riu1,5, Lionel Lourit5, Guillaume Lequertier5, and Hayabusa2 MicrOmega-Curation team1,51Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 2University of Tokyo, 3Marine Works
Japan, Ltd., 4The Graduate University for Advanced Studies (SOKENDAI), 5Institut d'Astrophysique Spatiale, Université
Paris-Saclay
The Hayabusa2 spacecraft successfully brought samples back to Earth in December 2020, collected at two different
locations on the surface of the C-type asteroid Ryugu. The samples, weighing about 5.4 g, have been transported to theExtraterrestrial Samples Curation Center of JAXA and have been installed in vacuum chambers or pure nitrogen-purgedchambers. JAXA curation is currently in the progress of producing catalog data to be included in the database, which is planned
to be open in early 2022 towards sample allocation for Announcement of Opportunity [2]. Within this work, basic properties ofreturn samples, for both the aggregate and individually picked-up grains, are acquired using microscopy, weighing, andvisible/near-infrared spectroscopy and imaging analyzer. One of the methods is near-infrared hyperspectral microscopy by
MicrOmega, developed at IAS (Orsay, France) [3].
MicrOmega is installed in a class 1000 clean room, in contact with a sapphire viewport window of a nitrogen-purged
clean chamber. By distant monochromatic light illumination of MicrOmega, it enables non-destructive ultraclean analysis
without exposure of the samples to the atmosphere and protecting them from contamination such as water and human-derived
organics. MicrOmega has a 5x5 mm Field of View (FOV) and 250x256 pixels with a resolution of 22.5 µm/pixel, and generates
a hyperspectral (x,y,λ) cube within the 0.99 to 3.65 µm wavelength range. The performance above can mark the presence ofabsorption bands suggestive of hydrous minerals at 1.4, 1.9, and 2.7-3.0 µm, and of organics and carbonates at 3.4 µm. Also, its
FOV can cover the entire body of a single grain, most of which are about a few mm in size, and the image resolution allows to
distinguish interstitial materials such as meteoritic inclusions more than 50-100 µm in diameter.
In the production of data for the catalog, it is important to be careful about the shape-dependent signals of grains. The
image often shows strong specular reflection and/or the shadow effect at a certain angle due to the instrument's light illumination
incidence angle: 35 degrees. Therefore, for the catalog, two monochromatic images with different angles are generated for eachsingle grain to show the effect of angular dependence. In addition, since the FOV usually includes signal from the sapphire
sample dish where the grain sits, we extract the average spectra of the grain area only. Furthermore, if there are areas that show
distinctive signatures different from most of the others, specific ROIs are also extracted. The database will contain images
showing the ROIs and their spectral data, with comments on the inclusions and minerals they may imply.
In this presentation, we will introduce the MicrOmega data acquisition and data processing, including approaches in
the presence of angle-dependent effects and sorting strategies for the curatorial initial description, and the characteristics oftypical samples based on results obtained so far for each individual grain.

Figure 1. (a) Monochromatic image of A0015 grain at 2.50um at 0 deg,

Figure 2. Average reflectance of A0015

and (b) at 180 deg, showing angular dependence on the reflectance.

at different angles and focal positions.

References: [1] Yada et al. submitted to Nature Astron., [2] Nishimura M. et al. (2021), Astromaterials Data Management in
the Era of Sample-Return Missions Community Workshop, Abstract, [3] Pilorget et al. submitted to Nature Astron.

Comparison of ion- and laser-weathered spectra of olivines and pyroxenes
K. Chrbolková1,2,3, R. Brunetto4, J. Ďurech2, T. Kohout1,3, K. Mizohata5, P. Malý6, V. Dědič7, C. Lantz4, A. Penttilä8, F.
Trojánek6, and A. Maturilli9
1
Department of Geosciences and Geography, University of Helsinki, Gustaf Hällströmin katu 2, 00560 Helsinki, Finland(katerina.chrbolkova@helsinki.fi)
2
Astronomical Institute of Charles University, V Holešovičkách 2, 18000 Prague 8, Czech Republic
3
Institute of Geology, The Czech Academy of Sciences, Rozvojová 269, 16500 Prague 6, Czech Republic
4
Université Paris-Saclay, CNRS, Institut d'Astrophysique Spatiale, 91405 Orsay, France
5
Department of Physics, Faculty of Science, University of Helsinki, Pietari Kalmin katu 2, 00560 Helsinki, Finland
6
Department of Chemical Physics and Optics, Faculty of Mathematics and Physics, Charles University, Ke Karlovu 3, 12116
Prague, Czech Republic
7
Institute of Physics, Faculty of Mathematics and Physics, Charles University, Ke Karlovu 5, 12116 Prague, Czech Republic
8
Department of Physics, Faculty of Science, University of Helsinki, Gustaf Hällströmin katu 2, 00560 Helsinki, Finland
9
Institute of Planetary Research, DLR German Aerospace Centre, Rutherfordstrasse 2, 12489 Berlin, Germany

Introduction: Irradiation by solar wind ions and impacts of micrometeoroids are the leading processes that weather surfacesof airless planetary bodies in the solar system. As a result, key diagnostic features of their spectra get altered. The mostprominent changes in the silicate-rich bodies in the visible (VIS) and near-infrared (NIR) wavelengths are increase in the
spectral slope, reduction of the albedo, and flattening of the mineral absorption bands (see, for example, [1]).
Our laboratory experiments aimed at understanding what are the similarities and differences between the effect of the solar
wind ions and micrometeoroid impacts on the final spectra of the silicate-rich bodies.
Methods: We have used two different terrestrial minerals, olivine and pyroxene, which we ground , dry-sieved, and pressed
into pellets.
Hydrogen (H) irradiations proceeded at the Accelerator Laboratory of the University of Helsinki, using 5 keV ions withvarying fluences from 1014 to 1018 ions/cm2. Helium and argon irradiations were done using the INGMAR set-up (IASCSNSM, Orsay) with 20 and 40 keV ions and with fluences from 1015 to 1017 ions/cm2.
Individual 100-fs laser pulses were shot into a square grid on the pellets’ surface to simulate the micrometeoroid impacts (as in[2]) in the laboratories at Charles University. Various densities of the pulses per cm 2 simulated different weathering stages.
Subsequent spectral measurements covered wavelengths from 0.54 to 13 μm, i.e. VIS to mid-infrared wavelengths. After themeasurements, we evaluated the evolution of the spectral parameters estimated using the Modified Gaussian Model [3, 4].
Results: We found that the variation of the spectra in the VIS range was similar for H+- and laser-irradiated samples, but wehave identified a difference in the NIR wavelength range. Laser irradiation caused greater changes in NIR than any of the ions
we used, see Fig. 1. The reason for such difference in behaviour may be that the penetration depth of the laser pulses is muchlarger than in the case of the ions. The relative contribution of the irradiated material in the spectra is then smaller in the ioncase than in the laser case.
Otherwise, we found that the original mineralogy of the surface is the leading factor influencing the evolution of the spectral
parameters. While olivine and pyroxene showed albedo variations of a similar order, the evolution of pyroxene’s spectral slope
was negligible when compared to olivine. This has implications for olivine-pyroxene mixtures and their evolution. E.g. in thecase of asteroid (433) Eros, the variation of the spectral slope is minor, but other spectral parameters show some variation. As
the surface of Eros is old, we hypothesise that spectral slope changes induced by olivine alteration already saturated and theleading source of the spectral variation is pyroxene, which does not show large variations in the slope. In contrast asteroid(25143) Itokawa is younger and thus still shows variations in the spectral slope as it has not saturated yet.

Figure 1. Spectral differences caused by laser and hydrogen ion (H+) irradiation. Each bar connects at the upper end the reflectance, R, ofthe fresh material and at the lower end R of the material weathered to the level marked in the legend.

References[1] Hapke, B. 2001, J. Geophys. Res., 106, 10039[2] Fazio, A., Harries, D., Matthäus, G., et al. 2018, Icarus, 299, 240[3] Sunshine, J. M., Pieters, C. M., & Pratt, S. F. 1990, J. Geophys. Res., 95, 6955
[4] Sunshine, J. M., Pieters, C. M., Pratt, S. F., & McNaron-Brown, K. S. 1999, in Lunar and Planetary Inst. Technical Report,
Vol. 30, Lunar and Planetary Science Conference, 1306

Solid Materials of Mineral and Rock on the Solar System: X-ray Unit and Mixed Status
Yasunori Miura1 and Toshio Kato2
Faculty of Science, Yamaguchi University, Yoshida, Yamaguchi, Yamaguchi, JAPAN
2
Department of Earth System Sciences, Faculty of Science, Yamaguchi University, Yoshida, Yamaguchi, Yamaguchi, JAPAN1

Introduction: Solid materials of all celestial bodies on the Solar System (with technical limits of whole observation andcollection by man-made satellites) should be defined clearly as main purpose of this paper based on academic data of thosesolids from the Earth’s definition relatively.
Academic definition: All mineral crystals on Earth are defined with X-ray determination (as arrangement of 0.1nm unit)
and chemical composition (as stoichiometric compound) with its occurrence on the academic material database (as Earth’s
mineral), where the rock is composed on many mineral crystals or mineral with mixed irregular solids (with light or heavy
elements) usually. This Earth’s definition is easily applied to investigate and determination to unknown samples including
extraterrestrial samples on Earth and visiting collections on the Moon (and Mars and Asteroids etc.). However, basic definitionof solid samples on extraterrestrial sources is not enough to be defined (especially on its developed status as the Celestialbodies) as shown in Table 1.
New concept of the Solar System’s material: Solid bodies of the Solar System have been accepted mainly from their
movements from the geo-centered theory to the Helio-centered theory through many astrophysical investigators based on theMoon and nearest planetary tracking data. Therefore, we should investigate by solid material database (rock and/or mineralcrystal) of each Celestial body. This is main reason why a) mineral spices are completely different with the water-planet Earth(three systems of rock, ocean water and atmosphere as the mineral differentiation) and other Celestial bodies (mainly rockand/or atmosphere systems as different generation of mineral and rock compared with the planet Earth), b) previous collected
extraterrestrial rocks (without chondrules or not) shows different evolution of glass and mineral, c) final mineral grains (soils,
carbonates and silica) of the Earth’s sedimentary process cannot be obtained clearly on extraterrestrial samples so far, and d)various mineral deposits of light element of carbon (from extreme to lower conditions) are obtained from macroscopic tomicroscopically as shown in Table 1.

Existence of fluid-related grains: Carbon-bearing grains show only light element to exist all phase states from solid toliquid to vapor condition with various compositions, texture and atomic structure. Therefore, it is significant indicator to detect
its formed process with or without fluid on water-planet Earth (to form final global carbonate minerals and its rocks) , theMoon (to form global carbon distribution rich in fine regolith soils on surface), Mars (to form global carbon-rich grains anddeposits) and Asteroids (carbon-rich in fine regolith grains and/or carbon-bearing grains and rocks) as shown in Table 2.
Discussion: Earth’s minerals formed as large mineral crystals are defined by atomic structure and chemistry based on Xray analysis and EPMA-ATEM/SEM microanalyses in laboratory on Earth. On the other hand, extraterrestrial samples of theMoon, Mars and Asteroids have no large crystal of mineral grains (due to no global water system on these bodies). Therefore,
Earth’s mineral crystal cannot be obtained at any other planets and Asteroids without the global water system. Remote-sensing
detectors by the IR and Visible wavelengths are mainly instant data obtained from mainly molecular data (atom-atom
distances) which are different with Earth’s mineral definition. This suggests that extraterrestrial mineral rocks (or rockyminerals) are considered to be imperfect solids compared with Earth-type mineral crystal, which means that main X-ray peaksof crystal planes (hkl) are mainly formed during the developed processes with short extreme condition of simple or multiple
impact heating and cooling processes on the extraterrestrial bodies. In short, all celestial bodies at the Solar System arecompletely different on its process and fluid contribution for rocky mineral or mineral rock formation (including the Hayabusa
samples), which means that solid bodies of the Solar System might be the Helio-centered theory-type material rocks which are
not used by the Earth-type mineral rocks to all other extraterrestrial bodies (not as the Earth (geo)-centered materials as used in
the astronomical scale previously).

Summary: The following data are summarized in this study. 1) Solid materials of all Celestial bodies on the Solar
System are discussed on the solid data from the Earth’s definition relatively to the extraterrestrial Celestial bodies. 2) All
mineral crystals on Earth are defined with X-ray determination and chemical composition with its occurrence on the material
database, though basic definition of extraterrestrial sample is not enough to be defined from less crystalline rocks. 3) The
Earth’s minerals show absolutely huge numbers of mineral species, well differentiated minerals, various Earth’s sedimentary
process, and various mineral deposits of carbon-bearing grains. 4) Carbon-bearing grains show various grains, texture andcompounds which are indicators of the detailed formation process on each Celestial body including the Hayabusa samples. 5)
The material data of the samples might indicate that all material data of mineral and rock are different from the Celestialbodies of the Solar System.
References:
Cresswell R., Beukens R., Rucklidge J. and Miura Y., Distinguishing spallogenic from non-spallogenic carbon in chondrites
using gas and temperature separations. Nuclear Intruments and Methods in Physics Research Section B (NIM-B) (Elsevier
Science, North-Holland), 92, 505-509, 1994.
Kato T. and Miura Y., The crystal structures of Jarosite and svanbergite. Mineralogical Journal, 8, 419-430, 1977.
Miura Y., Comparative consideration of Earth’s mineral from three major events: Solid formation of other Celestial bodies,
JAMS-2021 (Hiroshima Univ.), R5-01, 2021.
Miura Y., Carbon and carbon dioxides gas fixing by dynamic processes, Publication of JP5958889B2 (Active to 2028), 2016.
Miura Y., Complex texture and structure of shocked quartz mineral with graphite grain., Acta Crsyt., 64, 55, 2008.
Miura Y. , Material evidence for compositional change of dusts by collision applied to the Solar System's formation and theAsteroid belt. The ASP Conf. Series, 63, 286-288, 1994.
Miura Y. and Kato T., Shock waves in cosmic space and planetary materials. American Institute of Physics (AIP) Conf. Proc.,
283 (Earth and Space Science Information Systems), 488-492, 1993.
Miura Y., Accelerator mass spectrometry facilities in Japan. The Future of AMS Requirements in Canada (NSERC), 1, 45,
1991.
Miura Y. and Tomisaka T., Composition and structural substitution of meteoritic plagioclases. Mem. Natl Inst. Polar Res.,
Spec. Issue (NIPR, Tokyo), 35, 210-225,1984.
Miura Y., Computer simulation of anomalous composition of Mg-Fe plagioclase in meteorite. Mem. Natl Inst. Polar Res.,
Spec. Issue (NIPR, Tokyo), 35, 226-242, 1984.
Smith D.G.W., Miura Y. and Launspach S., Fe, Ni and Co variations in the metals of some Antarctic chondrites. Earth andPlanetary Science Letters, 120, 487-498, 1993.

Model of Material Characteristics of Carbonaceous Meteorites from Texture of Carbon-Bearing
GrainsYasunori Miura
Faculty of Science, Yamaguchi University, Yoshida, Yamaguchi, Yamaguchi, JAPANIntroduction: Carbonaceous meteorites are unique meteorites in the extraterrestrial rocks. In this study author reports
proposed model of previous unknown characteristics of hard samples with voids, carbon-bearing texture, Ca-Al-rich grains(with H, C, S) and detailed model of carbon-bearing grains in the carbonaceous meteorite which are applied to the Hayabusa
samples as the present purpose here.
Characteristics of Carbonaceous chondrite: Carbonaceous chondrites contain ususally Ca and C elements (with Mg, Na
ions and H2O molecules), where these ions can form molecular gel (polymer) and amorphous (poorly crystallized Emblyo-typeof carbonates (calcite and aragonite in mineral crystal). This suggests that extraterestial Celestial body is started as 1)
Ordinary chondrite-type micrograins and intercluster pores (as less 2nm) followed gel pores (2 to 20nm in size) withoutcarbonated calcium silicate matrixes, and 2) Carbonaceous chondrite-type micrograins show Ca-modified silica gel clusters
mixed with amorphous calcium carbonates (ACC) with pores (4 to 10nm) as shown in Table 1. This model can be explain
why the meteorite shows porous rocks and harder rock (than normal porous crystalline rocks with light weight). These gel toamorphous grain can be formed in present laboratory and industrial application as Ca-Al-rich grains (with H, C, S) as low
carbon binders. This is just by accident in natural meteorite field academically because author has been investigated carbon
origin and its application in science filed (including the AMS carbon dating projects) used in terrestrial age of the Antarctic
meteorites (also in the Apollo samples as its carbon origins), and recent project of carbon and carbon dioxides gas fixing by
dynamic processes (as the public University project). If it can be confirmed in science filed, then we can apply thatcarbonceous meteorites (and Moon rocks) has similar texture to fix carbon (or carbon dioxides) by its sources anddevelopment of its extraterrestrial rocks (model of grains of ions-gel polymer-amorphouse calcium carbonates as shown in
Table 1, followed clear calcite crystal as in water planet Earth finally). This can be applied it also to decrease the climate
warning scientifically and inductrially (as well-known Japanese scientist indicated by calculated estimates from global
environmental data). The paper is dicussed it as material data with proposed model in the Hayabusa Symposium in Tokyo.

Summary: Author proposes model of hard samples with voids, carbon-bearing texture, Ca-Al-rich grains (with H, C, S)
and carbon-bearing grains in the carbonaceous meteorite (also including the Hayabusa samples).
References:
Miura Y., Comparative consideration of Earth’s mineral from three major events: Solid formation of other Celestial bodies,
JAMS-2021 (Hiroshima Univ.), R5-01, 2021.
Miura Y., Carbon and carbon dioxides gas fixing by dynamic processes, Publication of JP5958889B2 (Active to 2028), 2016.
MiuraY. and Tanosaki T., Characterization of products from the nuclear and fire-electric facilities (in Japanese), University
Report (Yamaguchi, Japan), 1-64, 2009.
Miura Y. , Material evidence for compositional change of dusts by collision applied to the Solar System's formation and theAsteroid belt. The ASP Conf. Series, 63, 286-288, 1994.
Miura Y. and Kato T., Shock waves in cosmic space and planetary materials. American Institute of Physics (AIP) Conf. Proc.,
283 (Earth and Space Science Information Systems), 488-492, 1993.
Smith D.G.W., Miura Y. and Launspach S., Fe, Ni and Co variations in the metals of some Antarctic chondrites. Earth andPlanetary Science Letters, 120, 487-498, 1993.
Miura Y., Computer simulation of anomalous composition of Mg-Fe plagioclase in meteorite. Mem. Natl Inst. Polar Res.,
Spec. Issue (NIPR, Tokyo), 35, 210-242, 1984.

Neural network for classification of asteroid spectraDavid Korda1 , Antti Penttilä2 , Arto Klami3 , and Tomáš Kohout1,4
1

Department of Geosciences and Geography, University of Helsinki, Finland2
Department of Physics, University of Helsinki, Finland3
Department of Computer Science, University of Helsinki, Finland
4
Institute of Geology, Czech Academy of Sciences, Czech Republic

Introduction
Asteroid mineral composition is important parameter in planetary science, planetary
defence, and in-space resource utilisation. Currently-used methods provide us mainly
quantitative information about the asteroid composition. The methods are based on
empirical relations between spectral parameters (band areas, positions, depths), or on
spectral unmixing, and are highly sensitive to quality and consistency of input reflectancespectra. We test artificial neural networks as a tool which can infer mineral composition
directly from the reflectance values.

Methods
Artificial neural networks are used in tasks which are very difficult to define with exact
mathematics. A sensitivity of the networks to quality of input data (e.g., absolutereflectance values or variations in spectral slope) can be partially suppressed. The
networks are made of layers of neurons. Each neuron in a layer is non-linearly connectedwith neurons in the previous and following layers. The non-linearity and complexity ofneural network enable them to solve various tasks.
We use neural network for computing of mineral composition of the most common
silicates presented in meteorites (olivine, orthopyroxene, clinopyroxene, and plagioclase).
Our neural network composed of the input layer with reflectance values, one ‘intermediate’layer (hidden layer), and the output layer. The outputs are modal composition of theminerals and their chemical composition represented with end-members.

Data
We utilised measured reflectance spectra from the Relab database1 . We are motivated by
the ASPECT instrument (part of Hera/Milany CubSat) which will carry-out observations
in visible and near-infrared part of spectra. For this reason, we chose spectra which coverinterval between 350 nm and 2550 nm with the resolution 15 nm or better.

Results
Olivine and orthopyroxene are the most common minerals in ordinary chondrites. Therefore, we firstly applied the neural network on a set of olivine and pyroxene spectra.
1

http://www.planetary.brown.edu/relabdata/

1

Figure 1: Results of chemical composition. Top row: olivine. Bottom row: pyroxene.
The neural network contained only one hidden layer with 30 neurons. The outputs
were volume fractions of the minerals and their chemical composition. We trained the
network on about 80% of the whole dataset and used the remaining 20% to test theaccuracy of the predictions. The results obtained from the 20% are shown in Fig. 1.
The vertical axes show the correct (previously published) values while the horizontal
axes the values predicted by the neural network. In the top row, there are iron andmagnesium composition in olivine. In the bottom row, there are iron, magnesium, andcalcium composition in pyroxene.

Discussion
Except a few outlier, the predicted composition is usually within about 10% from theactual composition. The outliers might be a consequence of a limited training dataset or
ambiguously determined actual composition. In the near future, the predictive capabilityof the network will be improved via optimisation of its architecture and due to increase
number of training samples. In the next step, we will train the network on synthetic
spectra of olivine, orthopyroxene, and plagioclase and evaluate the network on real
ordinary chondrites.

2

Assessment of organic, inorganic and microbial contamination in the facilities of theExtraterrestrial Sample Curation Center of JAXA
*Yuya Hitomi1, Toru Yada2, Aiko Nakato2, Miwa Yoshitake1,3, Kana Nagashima2, Haruna Sugahara2, Shino Suzuki2, Masahiro
Nishimura2, Kazuya Kumagai1, Masanao Abe2, Tatsuaki Okada2, Shogo Tachibana2,4, and Tomohiro Usui2
1
Marine Works Japan Ltd., Yokosuka, Kanagawa 237-0063, Japan, 2Institute of Space and Astronautical Science (ISAS),
Japan Aerospace Exploration Agency, Sagamihara, Kanagawa 252-5210 Japan, 3 Japan Patent Office, Chiyoda-ku, Tokyo
100-8915, Japan, 4UTOPS, Grad. Sch. Sci., Univ. Tokyo, Tokyo 113-0033, Japan.
The Extraterrestrial Sample Curation Center of JAXA (ESCuC) have received samples from S-type near-Earth asteroid
25143 Itokawa returned by Hayabusa and C-type near-Earth asteroid 162173 Ryugu by Hayabusa2 [1, 2]. The samples havebeen taken out from sample containers, investigated in a non-destruvtive way, and stored in high vacuum and purified nitrogen
circulating clean chambers installed in ISO Class 6 clean rooms in the ESCuC. A series of cleaning procedures for tools, jigs,
and sample storage/transport containers has been established for the usage in the clean chambers to avoid potential
contamination of samples [3].
Along with the contamination control, it is also important to keep monitoring the cleanliness of clean rooms and cleanchambers. For instance, several biotic amino acids were once detected from contamination coupons set inside the cleanchamber for Itokawa grains [4], of which contamination level was similar to that reported at the curation facility at NASA
Johnson Space Center [5, 6]. In recent years, contamination of organics has been assessed regularly through exposure ofwafers for 15-20 hours in the clean rooms and clean chambers. The regular assessment has found that the clean rooms is kept
at the ISO-SCC Class -8 level and the clean chambers at the ISO-SCC Class -9 for organics. Regular contamination assessmentof metallic elements has shown that both clean rooms and clean chambers maintain the level of ISO-SCC Class -10 or higher
for all measured elements although elements contained in equipments and tools, such as Fe, Cu, Ni, Cr, Al, Zn, Mn, and Co,
were often detected at a higher level in the clean chambers than in the cleanrooms. The contamination levels of Na and K, bothof which are good indicators of contamination from human beings, are low enough to be at the ISO-SCC class -11 level forboth clean chambers and cleanrooms. In addition to organic and inorganic monitoring, assessment of microbial contaminationlevel is scheduled for the cleanrooms and clean chambers in this fiscal year.
References[1] Yada T. et al. (2014) Meteoritics Planet. Sci. 49, 135-153. [2] Yada, T. et al. (2021) LPSC 52, #2008. [3] Yoshitake M. etal. (2021) JAXA-RR-20-004E, 1-30. [4] Sugahara H. et al. (2018) Earth Planets Space 70, 194. [5] Dworkin et al. (2018)OSIRIS-REx contamination control strategy and implementation. Space Sci Rev 214:9. [6] McLain et al. (2015)
Contamination Knowledge Report JSC Curation Cabinets, personal communication.