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Visiting Researcher |
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Recognition, analysis and expression of images and letters are studied in the multimedia
systems laboratory. The 3-D motion and the 3-D shapes of the object are analyzed, understood and expressed by computer from the images taken by multi TV camera or video camera in the study of computer vision and/or the 3-D stereovision. Our work has greatly contributed in Hayabusa project. The succession of landing on Itokawa by Hayabusa in November, 2005 owed to preciseness of 3D shape model of Itokawa by University of Aizu very much. And also development of HARMONICS (HAyabusa Remote MONItering & Commanding System) has contributed very much in operation. Three lab members are also energetically contributing in KAGUYA (SELENE) project, the Japanese lunar exploring mission and playing a major role in LISM, the remote sensing camera system. The major research targets are centered on lunar shape recognition, such as lunar terrain analyses, crater counting, understanding and detailed whole lunar geographic mapping. Furthermore, they are engaged in analyzing the lunar mineral composition using the category classification technique from color information of lunar images and investigating the future moon surface land usage. We are considering almost all kind of computer method to contribute lunar exploration, such as automatic crater counting, operation plan and log managing system, integration of lunar topological map from both Terrain camera (TC) data and Laser Altimeter (LALT) data, and so on. Furthermore, we are engaged also in space exploration programs in Japan including planetary and an asteroid exploration inquiry plan and contributing in research in lunar and planetary science. In the on-line handwriting character recognition system, the fundamental study to use the handwriting letter as the input system of the computer is investigated. The character recognition is one of the most important fields on the image processing. And also collaborations with the Republic of Korea are implemented by this lab. Laboratory members have participated actively in scientific meetings, both in Japan and abroad. They have presented and participated in seminars, and in presentation of scientific results in fully refereed publications. |
Refereed Journal Papers
| [asada-01:2008] |
Junichi Haruyama, Tsuneo Matsunaga, Makiko Ohtake, Tomokatsu Morota,
Chikatoshi Honda, Yasuhiro Yokota, Masaya Torii, Yoshiko Ogawa, and
the LISM Working Group (N. Asada). Global lunar-surface mapping experiment
using the Lunar Imager/Spectrometer on SELENE. Earth Planets and
Space, 60:243–255, 2008. |
| The Moon is the nearest celestial body to the Earth. Understanding the Moon is
the most important issue confronting geosciences and planetary sciences. Japan will
launch the lunar polar orbiter SELENE (Kaguya) (Kato et al., 2007) in 2007 as the
first mission of the Japanese long-term lunar exploration program and acquire data
for scientific knowledge and possible utilization of the Moon. An optical sensing instrument
called the Lunar Imager/Spectrometer (LISM) is loaded on SELENE. The
LISM requirements for the SELENE project are intended to provide high-resolution
digital imagery and spectroscopic data for the entire lunar surface, acquiring these
data for scientific knowledge and possible utilization of the Moon. Actually, LISM
was designed to include three specialized sub-instruments: a terrain camera (TC),
a multi-band imager (MI), and a spectral profiler (SP). The TC is a high-resolution
stereo camera with 10-m spatial resolution from a SELENE nominal altitude of 100
km and a stereo angle of 30 to provide stereo pairs from which digital terrain models
(DTMs) with a height resolution of 20 m or better will be produced. The MI is a
multi-spectral imager with four and five color bands with 20 m and 60 m spatial
resolution in visible and near-infrared ranges, which will provide data to be used to
distinguish the geological units in detail. The SP is a line spectral profiler with a
400-m-wide footprint and 300 spectral bands with 68 nm spectral resolution in the
visible to near-infrared ranges. The SP data will be sufficiently powerful to identify
the lunar surface ’s mineral composition. Moreover, LISM will provide data with a
spatial resolution, signal-to-noise ratio, and covered spectral range superior to that
of past Earth-based and spacecraft-based observations. In addition to the hardware
instrumentation, we have studied operation plans for global data acquisition
within the limited total data volume allotment per day. Results show that the TC
and MI can achieve global observations within the restrictions by sharing the TC
and MI observation periods, adopting appropriate data compression, and executing
necessary SELENE orbital plane change operations to ensure global coverage by
MI. Pre-launch operation planning has resulted in possible global TC high-contrast
imagery, TC stereoscopic imagery, and MI 9-band imagery in one nominal mission
period. The SP will also acquire spectral line profiling data for nearly the entire lunar
surface. The east-west interval of the SP strip data will be 34 km at the equator
by the end of the mission and shorter at higher latitudes. We have proposed execution
of SELENE roll cant operations three times during the nominal mission period
to execute calibration site observations, and have reached agreement on this matter
with the SELENE project. We present LISM global surface mapping experiments
for instrumentation and operation plans. The ground processing systems and the
data release plan for LISM data are discussed briefly. |
|
| [asada-02:2008] |
Noriaki Asada, Naoto Miura, Hirohide Demura, and Naru Hirata. Au
tomatic tracking of impact fragments. Int. J. Information Technology and
Management, in press, 2009. |
| In general, it is difficult to understand how the object was before collision and what
had happened during collision after a collision has destroyed them. The motion
analysis of the collision destruction phenomenon is extremely important as a help
of the total analysis of the destruction process and the automation of the motion
analysis of impact fragments has been requested in the field of hypervelocity impact
experiments. Some fragments were automatically tracked on images cut from an
impact experiment moving picture. A combination method of the two dimensional
continuous dynamic programming (2DCDP) method proposed by Oka (1998) and
the Helmert transform is proposed and applied in tracking fragments. After some
improvements, tracking of fragments was performed sufficiently and the effectiveness
of this method was confirmed. As a result, physical quantities of impact fragments
such as translation velocities, rotation velocities and so on were derived from the
analysis. |
|
| [asada-03:2008] |
Makiko Ohtake, Junichi Haruyama, Tsuneo Matsunaga, Yasuhiro
Yokota, Tomokatsu Morota, Chikatoshi Honda, and LISM team (N. Asada).
Performance and scientific objectives of the SELENE (KAGUYA) Multiband
Imager. Earth Planets and Space, 60:257–264, 2008. |
| The Multiband Imager (MI) is one of the 14 instruments for the Japanese SELENE
(KAGUYA) mission. Goal of the SELENE (KAGUYA) mission is to understand
origin and evolution of the Moon by obtaining global element and mineral compositions,
topological structure, gravity field of the whole Moon, and electromagnetic
and particle environment of the Moon. MI is designed to be a high-resolution multiband
imaging camera with a spatial resolution in visible bands of 20 m and a spatial
resolution in near-infrared bands of 62 m from the 100 km SELENE (KAGUYA)
orbit altitude. The MI flight model has been manufactured and integrated. MTF,
viewing vector, over-all sensibility, sensor linearity and electrical noise level (S/N
estimation test) were measured, and the results indicate that the MI will provide
sufficient MTF and low-noise data, just as estimated in the MI design phase. Operation
and data analyses plans have been established, and related tools and algorithms
have been developed and checked. One of MI scientific objectives is to investigate
small but scientifically very important areas such as crater central peaks and crater
walls and to investigate magnesian anorthosites. |
|
| [asada-04:2008, demura-01:2008, naru-001] |
Tsuneo Matsunaga, Makiko Ohtake, Junichi
Haruyama, Yoshiko Ogawa, Ryosuke Nakamura, Yasuhiro Yokota,
Tomokatsu Morota, Chikatoshi Honda, Masaya Torii, Masanao Abe,
Tokuhiro Nimura, Takahiro Hiroi, Tomoko Arai, Kazuto Saiki, Hiroshi
Takeda, Naru Hirata, Shinsuke Kodama, Takamitsu Sugihara, Hirohide Demura,
Noriaki Asada, Junya Terazono, and Hisashi Otake. Discoveries on
the lithology of lunar crater central peaks by SELENE Spectral Profiler.
Geophysical Research Letters, 35:L23201, 2008. |
| The Spectral Profiler (SP) onboard the Japanese SELENE (KAGUYA) spacecraft
is now providing global high spectral resolution visible-near infrared continuous reflectance
spectra of the Moon. The reflectance spectra of impact craters on the far
side of the Moon reveal lithologies that were not previously identified. The achievements
of SP so far include: the most definite detection of crystalline ironbearing
plagioclase with its characteristic 1.3 mm absorption band on the Moon; a new
interpretation of the lithology of Tsiolkovsky crater central peaks, previously classified
as‘‘ olivine-rich, ’’as mixtures of plagioclase and pyroxene; and the lower
limit of Mg number of low-Ca pyroxene found at Antoniadi crater central peak and
peak ring which were estimated through direct comparison with laboratory spectra
of natural and synthetic pyroxene samples. |
|
| [asada-05:2008, demura-02:2008, naru-02:2008] |
Junichi Haruyama, Makiko Ohtake,
Tsuneo Matsunaga, Tomokatsu Morota, Chikatoshi Honda, Yasuhiro
Yokota, Masanao Abe, Yoshiko Ogawa, Hideaki Miyamonto, Akira Iwasaki,
Carlie M. Pieters, Noriaki Asada, Hirohide Demura, Naru Hirata, Junya
Terazono, Sho Sasaki, Kazuto Saiki, Atsushi Yamaji, Masaya Torii, and
Jean-Luc Josset. Long-Lived Volcanism on the Lunar Farside Revealed by
SELENE Terrain Camera. Science, 323:905–908, 2009. |
| We determined model ages of mare deposits on the lunar farside based on the
crater frequency distributions in 10- m-resolution images obtained by the Terrain
Camera on SELENE (KAGUYA). Most mare volcanism that formed mare deposits
on the lunar farside ceased at 3.0 Ga, suggesting that mare volcanism on the Moon
significantly reduced globally during this period. However, several mare deposits at
various locations on the lunar farside also show a much younger age, clustering at
2.5 Ga. These young ages indicate that mare volcanism on the lunar farside lasted
longer than previously considered and may have occurred episodically. |
|
| [asada-06:2008] |
Noriaki Asada, Naru Hirata, Hirohide Demura, Naoto Harada,
Yuto Shibata, Shota Kikuchi, Tomoki Hodokuma, Junichi Haruyama,
Makiko Ohtake, Tsuneo Matsunaga, Yasuhiro Yokota, Tomokatsu Morota,
Chikatoshi Honda, Yoshiko Ogawa, Masaya Torii, Tokuhiro Nimura, Hiroshi
Araki, and Seiichi Tazawa. Computational Geology for Lunar Data Analysis
from LISM on KAGUYA. Advances in Geosciences, in press, 2009. |
| The huge volume of Lunar Imager/Spectrometer (LISM) data (over 10 TBytes)
returned from the moon requires computer processing. Previous automatic crater
recognition algorithms to detect craters on photographs are strongly affected by the
solar elevation angle. On the other hand, automatic crater counting on a digital
terrain model (DTM) can avoid the influence of the solar elevation angle. Crater
chronology is expected to be developed through detailed analysis of data from the
LISMs Terrain Camera (TC) aboard the KAGUYA lunar orbiter. The TC has a
spatial resolution of 10 m/pixel. By using textural features of detailed topographic
data obtained from the TC, as well as detailed spectral information from images
acquired by the Multi-band Imager (MI), a more detailed mapping of the moon is
possible. Reliable classification for geological mapping may be obtained by using
a k-means method, which classifies the mineral composition and degree of spaceweathering
in addition to highland areas and mare. |
|
| [demura-03:2008, naru-03:2008] |
R. W. Gaskell, O. S. Barnouin-Jha, D. J. Scheeres,
A. S.Konopliv, T. Mukai, S. Abe, J. Saito, M. Ishiguro, T. Kubota,
T. Hashimoto, J. Kawaguchi, M. Yoshikawa, K. Shirakawa, T. Kominato,
N. Hirata, and H. Demura. Characterizing and navigating small bodies with
imaging data. Meteoritics & Planetary Science, 43(6):1049–1061, 2008. |
| Recent advances in the characterization of small body surfaces with stereophotoclinometry
are discussed. The principal data output is an ensemble of landmark
maps (L-maps), high-resolution topography/albedo maps of varying resolution that
tile the surface of the body. Because they can have a resolution comparable to the
best images, and can be located on a global reference frame to high accuracy, Lmaps
provide a significant improvement in discriminatory power for studies of small
bodies, ranging from regolith processes to interior structure. These techniques are
now being used to map larger bodies such as the Moon and Mercury. L-maps are
combined to produce a standard global topography model (GTM) with about 1.57
million vectors and having a wide variety of applications. They can also be combined
to produce high-resolution topography maps that describe local areas with
much greater detail than the GTM. When combined with nominal predictions from
other data sources and available data from other instruments such as LIDAR or
RADAR, solutions for the spacecraft position and camera pointing are the most
accurate available. Examples are drawn from studies of Phobos, Eros, and Itokawa,
including surface characterization, gravity analysis, spacecraft navigation, and incorporation
of LIDAR or RADAR data. This work has important implications for
potential future missions such as Deep Interior and the level of navigation and
science that can be achieved. |
|
| [demura-04:2008] |
J. Haruyama, M. Ohtake, T. Matsunaga, T. Morota, Y. Yokota,
C. Honda, N. Hirata, H. Demura, A. Iwasaki, R. Nakamura, S. Kodama,
and LISM working Group. Planned Radiometrically Calibrated and Geometrically
Corrected Products of Lunar High-Resolution Terrain Camera on
Selene. Advances in Space Research, 42:310–316, 2008. |
| Planning Ground Data Processing Procedures and Calibration Procedures |
|
| [demura-05:2008, naru-04:2008] |
N. Hirata, Olivier S. Barnouin-Jha, C. Honda, R Nakamura,
H. Miyamoto, S. Sasaki, H. Demura, Akiko M. Nakamura,
T. Michikami, Robert W. Gaskell, and J. Saito. A survey of possible impact
structures on 25143 Itokawa. Icarus, 200(2):486–502, 2009. |
| We determined the morphologies and dimensions of possible impact craters on the
surface of Asteroid 25143 Itokawa from images taken by the Hayabusa spacecraft.
Circular depressions, circular features with flat floors or convex floors, and circular
features with smooth surfaces were identified as possible craters. The survey identified
38 candidates with widely varying morphologies including rough, smooth and
saddle-shaped floors, a lack of raised rims and fresh material exposures. The average
depth/diameter ratio was 0.080.03: these craters are very shallow relative to craters
observed on other asteroids. These shallow craters are a result of (1) target curvature
influencing the cratering process, (2) raised rim not being generated by this
process, and (3) fines infilling the craters. As many of the crater candidates have an
unusual appearance, we used a classification scheme that reflects the likelihood of
an observed candidate’s formation by a hypervelocity impact. We considered a variety
of alternative interpretations while developing this scheme, including inherited
features from a proto-Itokawa, spall scars created by the disruption of the proto-
Itokawa, spall scars following the formation of a large crater on Itokawa itself, and
apparent depressions due to random arrangements of boulders. The size-frequency
distribution of the crater candidates was close to the empirical saturation line at
the largest diameter, and then decline with decreasing diameter. |
|
| [naru-05:2008] |
A. M. Nakamura, T. Michikami, N. Hirata, A. Fujiwara, R. Nakamura,
M. Ishiguro, H. Miyamoto, H. Demura, K. Hiraoka, T. Honda, C. Honda,
J. Saito, T. Hashimoto, , and T. Kubota. Impact process of boulders on
the surface of asteroid 25143 Itokawa―fragments from collisional disruption.
Earth, Planets and Space, 60:7–12, 2008. |
| The subkilometer-size asteroid 25143 Itokawa is considered to have a gravitationally
bounded rubble-pile structure. Boulders appearing in high-resolution images
retrieved by the Hayabusa mission revealed the genuine outcome of the collisional
event involving the asteroid’s parent body. Here we report that the boulders’ shapes
and structures are strikingly similar to laboratory rock impact fragments despite
differences of orders of magnitude in scale and complexities of the physical processes.
These similarities suggest the universal character of the process throughout
the range of these scales, and the brittle and structurally continuous nature regarding
the parent body of the boulders. The similarity was likely preserved because
of relatively lesser comminuting processes acting on individual boulders; the close
assemblages of similar appearing boulders (a boulder family) represent the impact
destruction of boulders on the surface. |
|
| [naru-06:2008] |
O. S. Barnouin-Jha, A. F. Cheng, T. Mukai, S. Abe, N. Hirata, R. Nakamura,
R. W. Gaskell, J. Saito, and B. E. Clark. Small-scale topography of
25143 Itokawa from the Hayabusa laser altimeter. Icarus, 198:108–124, 2008. |
| The surface topography of Asteroid 25143 Itokawa is explored using the LIght Detection
And Ranging instrument (LIDAR). The data confirm the presence of a rough
highland and a smooth lowland. The highland is dominated by boulders, but also
possesses topography associated with surface lineaments and broad surface facets.
The boulders ensure that the roughness of the highlands over short distances is typically
greater relative to most surfaces on 433 Eros. Over larger distances, Itokawa
is always smoother than Eros possibly because of its smaller size and weak rubblepile
structure. The lowlands of Itokawa are very smooth, and are typically devoid
of boulders. Some transitional regions midway between the highlands and lowlands
also exist. In these areas, craters that retain their regolith fill possess flat floors
and resemble “ponds” seen on 433 Eros. Analyses of surface elevation, imagery and
a quantitative measure of surface roughness are consistent with regolith flowing
downhill from the highlands to fill in the low areas of Itokawa, probably covering
up any pre-existing rough terrain. Using this interpretation, we find a minimum
2.30.4 m thick layer of regolith in the lowlands, which, if spread evenly across the
entire asteroid, corresponds to a 421 cm thick layer. It is very difficult to generate
this amount of regolith with the population of craters seen on Itokawa. However,
an Itokawa composed of several large masses may have retained this regolith during
its formation. The presence of such large masses could account for the observed
lineaments and what appear to be exposures of bedrock on the largest steep slope
observed. |
|
| [naru-07:2008] |
N. Hirata, K. Kurita, and T. Sekine. Simulation experiments for shocked
primitive materials in the Solar System. Physics of the Earth and Planetary
Interiors, 174:227–241, 2009. |
| Shock recovery experiments were conducted on porous mixtures (initial porosity
35 +/- 5%) in silicate-metal and silicate-metal-sulfide systems in an attempt to
simulate impact phenomena of unconsolidated porous materials similar to ordinary
chondrites in a wide range of shock pressures from 20 to 70 GPa. The textures
and chemical compositions of shocked samples were investigated in detail. Features
such as grain deformation, fracture density decrease, and heterogeneous meltings
are found. At ¡ 30 GPa, mechanical effects of the shock process, such as silicate
fracturing and metal elongation, are dominant. Morphological analysis of metal
grains in shocked samples reveals good correlation between the degree of deformation
and the shock pressure. The metal grain aspect ratio may be a good indicator
of shock pressure. At higher pressures, thermal effects, which are enhanced in the
shock compression of porous media, become prominent. Above 30 GPa, silicate
grain fractures disappear, and silicate darkening dominates. Shock-induced melting
in the shock veins and melt networks is observed and interpreted as localized in situ
melting features, the heat source of which is frictional heating between grains. Thin
veins and melt pockets of sulfide-metal melt are the principal characteristics in this
type of sample. Melting features of metal-sulfide systems alter the spectral property
of meteoritic bodies. The initial porosity of a target may have been an important
factor in impact processes in the early Solar System. |
|
| [naru-08:2008] |
P. Michel, D. P. O’Brien, S. Abe, and N. Hirata. Itokawa’s cratering
record as observed by Hayabusa: Implications for its age and collisional
history. Icarus, 200:503–513, 2009. |
| In this paper, we study cratering and crater erasure processes and provide an age
estimate for the near-Earth Asteroid (25143) Itokawa, the target of the mission
Hayabusa, based on its crater history since the time when it was formed in the
main belt by catastrophic disruption or experienced a global resetting event. Using
a model which was applied to the study of the crater history of Gaspra, Ida, Mathilde
and Eros [O’Brien, D.P., Greenberg, R., Richardson, J.E., 2006. Icarus 183, 79–92],
we calculate the time needed to accumulate the craters on Itokawa’s surface, taking
into account several processes which can affect crater formation and crater erasure
on such a low-gravity object, such as seismic shaking. We use two models of the
projectile population and two scaling laws to relate crater diameter to projectile size.
Both models of the projectile population provide similar results, and depending on
the scaling law used, we find that the time necessary to accumulate Itokawa’s craters
was at least ?75 Myr, and maybe as long as 1 Gyr. Moreover, using the same model
and similar parameters (scaled accordingly), we provide a good match not only to
Itokawa’s craters, but also to those of Eros, which has also been imaged at high
enough resolution to give crater counts in a similar size range to those on Itokawa.
We show that, as for Eros, the lack of small craters on Itokawa is consistent with
erasure by seismic shaking, although for Itokawa, the pronounced deficiency of the
smallest craters (¡10 m in diameter) requires another process or event in addition
to just seismic shaking. A small body such as Itokawa is highly sensitive to specific
events that may occur during its history. For example, the two parts of Itokawa,
called head and body, may well have joined each other by a low-velocity impact
within the last hundred thousand years [Scheeres, D.J., Abe, M., Yoshikawa, M.,
Nakamura, R., Gaskell, R.W., Abell, P.A., 2007. Icarus 188, 425–429]. In addition
to providing an erasure mechanism for small craters, the proposed timescale of that
event is consistent with the timescale necessary in our model to form the current,
depleted population of just a few small (¡10 m) craters on Itokawa, suggesting that
it may be the explanation for the discrepancy between Itokawa’s cratering record
and that obtained from our equilibrium seismic shaking model. Other explanations
for the depletion of the smallest craters on Itokawa, such as armoring by boulders
lying on the surface, cannot be ruled out. |
|
| [naru-09:2008] |
K. Saiki, K. Saito, H. Okuno, A. Suzuki, Y. Yamanoi, N. Hirata, , and
R. Nakamura. Estimation of the lunar reflectance by ground-based observation
using a tunable liquid-crystal filter telescope. Earth, Planets, and
Space, 60:417–424, 2008. |
| Lunar reflectance data are useful not only for lithological identification of the lunar
surface but also for radiometric calibration and determination of exposure time for
optical sensors of lunar probes. To gain data on lunar reflectance, we acquired multiband
images (five bands: 650, 750, 900, 950, and 1000 nm) of the lunar surface and
those of some standard stars using a liquid-crystal tunable filter (LCTF) telescope
located on the peak of Mt. Haleakala (Hawaii, USA). The data obtained indicate
that the reflectance data of Clementine UV/VIS is too high and that the correction
factor is 0.590.06 at 950 nm. Our new reflectance data are available to the public
at the web site of one of authors (K.S.). We report here our method of deriving the
lunar reflectance images from the ground-based observation with a hyperspectral
telescope for the users of our reflectance data. The results suggest that ground-based
observation is more suitable for the radiometric calibration of the sensor of a lunar
probe than laboratory data. |
|
| [naru-10:2008] |
T. Michikami, A. M. Nakamura, N. Hirata, R. Gaskell, R. Nakamura,
T. Honda, C. Honda, K. Hiraoka, J. Saito, H. Demura, M. Ishiguro, , and
H. Miyamoto. Size-frequency statistics of boulders on global surface of asteroid
25143 Itokawa. Earth, Planets and Space, 60:13–20, 2008. |
| he surface of asteroid 25143 Itokawa is covered with numerous boulders although
gravity is very small compared with that of other asteroids previously observed from
spacecraft. Here we report the size-frequency statistics of boulders on the entire
surface of Itokawa based on high-resolution images (1 pixel -0.4 m) obtained by the
Hayabusa spacecraft. There are 373 boulders larger than 5 m in mean horizontal
dimension on the entire surface―0.393 km2―and the number density is nearly
103/km2. The cumulative boulder size distribution on the entire surface has a powerindex
of -3.1 ± 0.1. For the east and west sides and the head and body portions
of Itokawa, the power-index of the size distributions and the number densities of
boulders of these areas are thought to be similar from the statistical point of view.
A global mapping of boulders shows that there is no apparent correlation in the
locations of boulders and craters. The ratio of the total volume of the boulders to
the total excavated volume of the craters on Itokawa is -25% when only craters
larger than 50 m in mean diameter are considered, and this ratio is extremely larger
than that on Eros and the Moon, respectively. The origin of boulders on the surface
of Itokawa was examined quantitatively by calculating the number of boulders and
the size of the largest boulder using a model based on impact cratering experiments.
The result indicated that the boulders on the surface of Itokawa cannot solely be
the product of craters. Our results suggest that the boulders originated from the
disruption of the larger parent body of Itokawa, as has been described in previous
papers (Fujiwata et al., Science, 312, 1330-1334, 2006; Saito et al., Science, 312,
1341-1344, 2006). |
Refereed Proceeding Papers
| [asada-07:2008] |
J. Terazono, N. Asada, H. Demura, N. Hirata, K. Saiki, A. Iwasaki,
R. Oka, T. Hayashi, T. Suzuki, H. Miyamoto a nd J. Haruyama, M. Ohtake,
T. Matsunaga, S. Sobue, H. Okumura, T. Fujita, and A. Yamamoto. Integrated
Lunar Web-GIS Environment using Data Obtained by Lunar Exploration.
In 40th Lunar and Planetary Science Conference (LPSC 2009), page
1232, Houston, March 2009. LPI and NASA JSC. |
| The dissemination of Web-GIS (Geographical Information System) in the research
field demonstrates that the map, shown in the web pages, are the most basic data for
the scientific activity. This fact also have an effect on lunar exploration. In Kaguya
project, the handling of huge quantities of data will be the key to promote research.
Most of the data are obtaind by LISM, Lunar Imager and Spec-trometer, consists of
Multiband Imager (MI), Spectral Profiler (SP) and Terrain Camera (TC). The image
data will form the base of the Kaguya data for global mapping and topographical
understanding of the moon. The network-based collaboration environment enables
them to utilize those image data without carry-ing them on in the meeting and share
their result on the net. It will contribute in the increasing of scientific productivity
and indurate future style of research in lunar exploration. In this presentation,
we will show current imple-mentation status of the Web-GIS based collaboration
environment using lunar exploration data. |
|
| [asada-08:2008] |
J. Haruyama, M. Ohtake, T. Matunaga, T. Morota, C. Honda,
Y. Yokota, Y. Ogawa, and LISM working group (N. Asada). SELENE
(KAGUYA) Terrain Camera Observation Results of Nominal Mission Period.
In 40th Lunar and Planetary Science Conference (LPSC 2009), page
1553, Houston, March 2009. LPI and NASA JSC. |
| On 31 October 2008, the Japanese Moon explorer SELENE (KAGUYA) com-pleted
its nominal observation period of about one-year from December 2007 and entered
the extended-mission period that is expected to be about a half year using surplus
fuel. During the SELENE nominal mission period, the push-broom Terrain Camera
(TC) [1] aboard KAGUYA, successfully acquired 10 m-resolution stereoscopic data
at solar elevation angles of around 30 °and monoscopic data at angles of less than
30 °for almost the entire surface of the Moon. The rate of discrete cosine transform
(DCT) com-pression of TC data was 10 to 20% (100% without compression). There
was very little or no block noise due to compression. Most image data was acquired
by TC in sequential revolutions of SELENE (interval of about 2 hours) and thus was
easily superposed with sequential overlapped image data to yield large mosaicked
data. Unobserved areas that totaled less than 5% of the whole surface of the Moon
and are planned to be observed in the extended-mission pe-riod. The TC is currently
working very well after the end of the nominal-mission period. No defective pix-els
have been found so far. |
|
| [asada-09:2008] |
Noriaki Asada, Naoto Miura, Hirohide Demura, and Naru Hirata. Automatic
tracking of impact fragments. In 5th International Conference on
Information Technology and Applications (ICITA 2008), pages 767–770,
Cairns, June 2008. ICITA, IEEE and ACM. |
| Automation for the motion analysis of fragments has been requested in the field
of collision and destruction experiments. While extracting and tracking targeted
fragments is used to be analyzed manually in a sequence of images and movie,
two dimensional continuous dynamic programming (2DCDP) with guaranteeing
monotonous continuity isintroduced in this research . Four large fragments in test
data were succeeded in handling and measuring velocities and sizes of them. Furthermore,
a new method to prepare a better reference image for every frame by
a combination of 2DCDP and Helmert transformation is introduced. These laborsaving
procedures are confirmed to be effective in analyses of objects in movies,
such as velocities, rotational velocities, area reduction and so on. |
|
| [asada-10:2008] |
N. Hirata, J. Haruyama, M. Ohtake, T. Matsunaga, Y. Yokota, T. Morota,
C. Honda, Y. Ogawa, T. Sugihara, H. Miyamoto, H. Demura, and
N. Asada. Morphological Analyses of Tycho Crater with KAGUYA Data.
In 40th Lunar and Planetary Science Conference (LPSC 2009), page 1514,
Houston, March 2009. LPI and NASA JSC. |
| We investigated a large lunar crater Tycho with KAGUYA/LISM data to reconstruct
the impact event forming the crater from distributions of its ejecta and other
associated features. The asymmetric distribution of the ray system of Tycho is
widely accepted as a piece of evidence that it was formed by an oblique impact in
the east-to-west direction [1]. Several researchers [2- 5] described other morphological
features of Tycho with data from previous missions or projects, and discussed
relationships between them and effects of the oblique impact. Although their conclusions
are generally consistent with the west-to-east oblique impact, comprehensive
discussions of various features have not been published. Moreover, we find inconsistency
between observed alignments of crater features and the proposed impact
direction. A group of researchers pointed out that slumping structures on the inner
wall are most developed in the uprange direction [3], but the maximum slumping
structure isn ’t found in the western inner wall, but in the southwestern inner wall
[2]. |
|
| [asada-11:2008] |
T. Matsunaga, M. Ohtake, J. Haruyama, Y. Ogawa, R. Nakamura,
Y. Yokota, T. Morota, C. Honda, M. Torii, M. Abe, T. Nimura, T. Hiroi,
T. Arai, K. Saiki, H. Takeda, N. Hirata, S. Kodama, T. Sugihara, H. Demura,
N. Asada, J. Terazono, and H. Otake. Current Status and First Scientific
Results of SELENE Spectral Profiler. In 40th Lunar and Planetary Science
Conference (LPSC 2009), page 2133, Houston, March 2009. LPI and NASA
JSC. |
| Spectral Profiler (SP) is a visible - near infrared grating spectrometer onboard
Japanese SELENE (Kaguya) Lunar explorer launched in September 2007. SP consists
of one reflective telescope, two plane gratings, three linear detectors, one threestage
peltier cooler, and two halogen lamps with a filter for radiometric and spectral
calibration. Data being obtained by SP since November 2007 are lunar surface spectral
reflectance in the 0.5 - 2.6 !m spectral region with 6 - 8 nm spectral sampling
interval, 500 m spatial sampling interval (along-track direction), and 500 m swath
(cross-track direction). SP’s spectral coverage and sampling interval are optimized
for the survey of plagioclase, pyroxene, and olivine which are major minerals on the
lunar surface. SP is the first instrument which provides such visible to near infrared
continuous reflectance spectra for both sides of the Moon. SP’s first light data and
early inflight performance were reported in [1]. In this paper, the current status and
the first scientific results of SP [2] are presented. |
|
| [asada-12:2008] |
Y. Shibata, N. Hirata, H. Demura, N. Asada, Y. Yokota an d T. Morota,
C. Honda, T. Matsunaga, M. Ohtake, and J. Haruyama. Semi-Automatic
Recognition of Lunar Geologic Units Based on Texture and Spectral Features
Using Image Data observed by KAGUYA, LISM TC/MI. In 40th Lunar and
Planetary Science Conference (LPSC 2009), page 1615, Houston, March
2009. LPI and NASA JSC. |
| Recognition of geologic units on image data is a fundamental analytical step of
remote sensing. A single geologic unit could be defined as a region with its own
particular features, which represent its origin. The same units have common photogeological
characteristics. Criteria for determining the units are varied between
previous and recent researches. In 1960 ’s and 1970 ’s, researchers in lunar science
used panchromatic photographs to make lunar geologic maps. Their basic criteria
of geologic units are defined by surface textures and topographic features in the
photographs. Recently, variation of remote sensing data has greatly expanded. Resolution
and coverage of image data are increase, and multi-spectral images of the
moon have been obtained through modern lunar missions [1]. We especially focus on
recognition of geologic units by combining texture and spectral features extracted
from image data. |
|
| [asada-13:2008] |
T. Hodokuma, K. Kuriki, N. Asada, H. Demura, J. Terazono, N. Hirata,
J. Haruyama, M. Ohtake, T. Matsunaga, and H. Araki. Integration of Multi-
Instrumental Data Sets of KAGUYA, LISM AND LALT. In 40th Lunar and
Planetary Science Conference (LPSC 2009), page 1637, Houston, March
2009. LPI and NASA JSC. |
| Integration science based on KAGUYA and other missions requires spatial registration
of different types of data sets. For example, two types of topographic data
sets; Digital Terrain Model (DTM) in 10m/pixel based on stereoscopic images of
Terrain Camera (TC) in the Lunar Imager/Spectrometer (LISM) and lunar surface
profiles in 1km interval derived from Laser Altimeter (LALT). The former is areal
data and the latter is linear one. Combining both data at certain areas provides
detailed views of morphology for geological interpretations. Another two types of
spectral data sets are also remarked; multiband color images and spectral profiles
derived from and Spectral Profiler (SP) and Multiband Imager (MI) in LISM. This
also shows the same relationship, the former is areal data and the latter is linear
one. Here we report current status on our project to develop the procedures. |
|
| [asada-14:2008, demura-06:2008] |
N. Asdada, N. Hirata, H. Demura, N. Harada, Y. Shibata,
J. Haruyama, M. Ohtake, T. Matsunaga, Y. Yokota, T. Morota,
C. Honda, Y. Ogawa, M. Torii, T. Nimura, H. Araki, and S. tazawa. Computational
Geology for Lunar Data Analysis from LISM, KAGUYA. In 5th Annual
Meeting Asia Oceania Geosciences Society (AOGS 2008), pages PS14–
A035, Busan, June 2008. Asia Oceania Geosci. Soc., KOFST and KOSEF. |
| Since LISM data carried back from the moon is too huge over 10 TByte, computer
processing is inevitably demanded. Crater chronology is expected to be developed
by detailed analysis of data from the Terrain Camera (TC) of LISM, KAGUYA,
which has the spatial resolution of 10m/pixel. Crater recognition procedures for
Digital Terrain Model (DTM) made from TC data is proposed as an application
of generalized Hough transform [1][2]. 1. Pre-processing — Enhancing process from
histogram information 2. Edge detection a. Binarization after high pass filtering
by Haar wavelet transform b. Noise elimination, connection and thinning 3. Crater
recognition — An application of generalized Hough transform a. Determination of
the ellipsoid parameters – Determination of the tangent, the center and crater edges
Effectiveness of this procedure in the field of planetary science is shown in a result
of the Cumulative Size Frequency Distribution (CSFD) curve. A more accurate geological
mapping on the moon is possible if it is done from both texture features of
more detailed topographic data from TC and detailed spectral information on images
taken by Multi-band Imager (MI). An automatic method listing up candidates
of geological mapping is proposed [3]. 1. Registration of images including spatial
resolution 2. Filtering process for extracting variances of pixels as texture features
3. Calculation of rational images as spectral features extraction 4. Classification
by k-means clustering method after normalization Ridges, grabens, and craters are
classified, while two types of basaltic sediments are classified in a preliminary experiment
using ”Apollo” and ”Clementine” images. |
|
| [asada-15:2008] |
Y. Ogawa, T. Matsunaga, R. Nakamura, H. Takeda, M. Ohtake, T. Morota,
T. Hiroi, T. Arai, K. Saiki, T. Sugihara, J. Haruyama, Y. Yokota,
C. Honda, T. Nimura, N. Hirata, H. Demura, N. Asada, and J. Terazono.
Mineral Compositions of the Bright Rayed Craters and Lunar Far-side Crust
Revealed by the Continuous VIS-NIR Spectra by Spectral Profiler on SELENE/
KAGUYA. In 40th Lunar and Planetary Science Conference (LPSC
2009), page 1650, Houston, March 2009. LPI and NASA JSC. |
| The Spectral Profiler (hereafter we write SP) is a visible and near infrared spectrometer
onboard SELENE/KAGUYA satellite. It covers 500- 2600 nm in wavelength
with spectral resolutions of 6-8 nm and high SNRs of 2300@810-860 nm, accompanying
three detectors (VIS: 513-1010 nm, NIR1: 884- 1676 nm and NIR2: 1702-2588
nm). SP data include very critical information to identify the mineralogical com
positions of the lunar surface with unprecedented accuracy. By its nominal mission
for about 1 year, the SP data accumulated so far amount to more than 4500 polar
orbits at the end of November, 2008. We obtained the global set of continuous
spectra of the lunar surface. The observed points by SP are every 500 m along the
tracks and the gaps across the tracks are less than a several kilometers on average,
which definitely contributes to the completion of the global mapping of the mineral
distribution [1]. |
|
| [asada-16:2008] |
M. Ohtake, T. Matsunaga, Y. Yokota, T. Morota, C. Honda, Y. Ogawa,
T. Sugihara, H. Miyamoto, H. Demura, and N. Asada. Morphological Analyses
of Tycho Crater with KAGUYA Data. In 40th Lunar and Planetary
Science Conference (LPSC 2009), page 1514, Houston, March 2009. LPI
and NASA JSC. |
| We investigated a large lunar crater Tycho with KAGUYA/LISM data to reconstruct
the impact event forming the crater from distributions of its ejecta and other
associated features. The asymmetric distribution of the ray system of Tycho is
widely accepted as a piece of evidence that it was formed by an oblique impact in
the east-to-west direction [1]. Several researchers [2- 5] described other morphological
features of Tycho with data from previous missions or projects, and discussed
relationships between them and effects of the oblique impact. Although their conclusions
are generally consistent with the west-to-east oblique impact, comprehensive
discussions of various features have not been published. Moreover, we find inconsistency
between observed alignments of crater features and the proposed impact
direction. A group of researchers pointed out that slumping structures on the inner
wall are most developed in the uprange direction [3], but the maximum slumping
structure isn ’t found in the western inner wall, but in the southwestern inner wall
[2]. |
|
| [asada-17:2008] |
M. Ohtake, T. Mastunaga, Y. Yokota, J. Haruyama, H. Miyamoto,
T. Arai, N. Hirata, H. Takeda, R. Nakamura, T. Morota, C. Honda,
Y. Ogawa, K. Kitazato, and LISM Team (N. Asada). Anorthosite with
100% Plagioclase on the Moon Detected by the SELENE Multiband Imager.
In 40th Lunar and Planetary Science Conference (LPSC 2009), page
1557, Houston, March 2009. LPI and NASA JSC. |
| MI is a high-resolution multiband imaging camera consisting of visible and nearinfrared
sensors (spectral band assignments are 415, 750, 900, 950 and 1000 nm
for visible and 1000, 1050, 1250 and 1550 nm for near infrared). MI takes pushbroom
imaging data by using selected lines of area arrays. The spatial resolution
of visible bands is 20 m, and that of near infrared bands is 62 m from the 100
km SELENE orbital altitude. First lunar images by MI were taken successfully on
November 3, 2007 during check out period of the SELENE mission. Since the first
nominal observation started on January 18, MI has been covered more than 95% of
the whole moon. MTF, dark current, flat field, responsibility and other performance
have been checked and were confirmed to be good and have not change drastically
compare to the pre-flight test data. |
|
| [asada-18:2008] |
Y. Yokota, T. Matsunaga, M. Ohtake, J. Haruyama, Y. Ogawa, R. Nakamura,
C. Honda, T. Morota, K. Saiki, S. Kawabe, K. Nagasawa, K. Kitazato,
and LISM Working Group (N. Asada). Lunar Phase Curve at VIS/NIR
Wavelength Observed by SELENE Spectral Profiler. In 40th Lunar and
Planetary Science Conference (LPSC 2009), page 2525, Houston, March
2009. LPI and NASA JSC. |
| SELENE Spectral Profiler (SP) obtains Lunar Visible to NIR spectral data at spatial
resolution of 500 m [1]. Since brightness of lunar surface depends on the viewing
geometry, we have to correct these data to the values under certain standard observation
geometry prior to the detailed analysis by an adequate phase curve. Although
many researchers had proposed photometric models and parameters of the moon
(e.g., [2-6]), extensive study is still important in following aspects: (1) Large incidence
angle. High latitude regions are usually observed at large incidence angle.
Accurate photometric parameters suites for such incidence angle range are required
for precise analysis of those regions. (2)Wavelength dependence. Clementine UVVIS
data significantly contributed to the photometric studies [e.g. 2-5] at 5 bands ranging
from 415nm to 1000nm. However, SP and other recent remote-sensing observations
require much longer wavelength coverage. (3) Geology dependence. Lunar phase
curve also has a dependence on geological types such as the Highland and Mare [3,
5]. We report preliminary results of Disk-resolved lunar phase curve at highland in
Vis/NIR wavelength range by SP data. |
|
| [demura-07:2008] |
N. Hirata, S. Abe, M. Ishiguro, k. Kitazato, R. Nakamura,
H. Miyamoto, H. Demura, M. Abe, and S. Sasaki. Geologic Processes on
the Surface of a Small Asteroid Itokawa. In 71st Annual Meeting of the
Meteoritical Society, 2008. |
| Geomorphological discussion for the origin and evolution of asteroid Itokawa |
|
| [demura-08:2008] |
N. Hirata, J. Haruyama, M. Ohtake, T. Matsunaga, Y. Yokota, T. Morota,
C. Honda, Y. Ogawa, M. Torii, H. Demura, and N. Asada. Morphological
Analyses of Large Lunar Craters with LISM/Kaguya Images. In 71st
Annual Meeting of the Meteoritical Society, 2008. |
| Geomorphological Discussion for oblique impacts features on the moon based on
image data sets of Kaguya/LISM |
|
| [jpshin-01:2008] |
Won-Du Chang and Jungpil Shin. DPW Approach for Random Forgery
Problem in Online Handwritten Signature Verification. In J. Kim, editor,
Proceedings of 4th International Conference on Networked Computing
and Advanced Information Management, pages 347–352. Sogang University,
IEEE, Sep. 2008. |
| In this paper, we refer a phenomenon of relatively high error rates against random
forgeries in online signature verification. Though human can easily distinguish
random forgeries from genuine signatures, the most published research results during
last decades have reported high error rates against them, compared to the
error rates against skilled forgeries. This paper suggests taking DPW (dynamic
positional warping) approach for the problem, which supplies high accuracy and
robustness against affine transform of online shapes. In addition, the effects of distance
normalization and slope constraints are tested to DPW and conventional
DTW (dynamic time warping). Our approach was compared to conventional DTW
method with consequential xy difference information with SVC2004 task1 database:
0.17against random and skilled forgeries, respectively. Comparing to the best result
of the conventional approach, the proposed approach reduced the error rates into
about 27costs. |
|
| [jpshin-02:2008 |
Won-Du Chang and Jungpil Shin. A Stochastic Stroke Model for Variable
and Personalized Handwriting Synthesis. In Proceedings of Fourth International
Conference on Intelligent Computing and Information Systems,
pages 705–711, New York, Mar. 2009. ACM. |
| This paper proposes a stochastic stroke model which synthesizes variable handwritten
characters preserving one’s writing style. Our fundamental concept of the
stochastic model is thinking a stroke as consecutive state changes of segments. After
clustering segments into several states, a number of characters are presented as a
directed graph with probabilities of state changes. To support the model, two modifications
of dynamic time warping techniques are presented: one is allowing division
to ensure one-to-one matching between segments, not loosing detailed shape information;
the other is a method of generating a template to align segments among
many signals. By employing stochastic method at segment levels, our model enables
generating various and natural handwritten characters with small number of training
data. We synthesized 3,600 English alphabets and numbers from 180 training
characters showing the variance of synthesized characters, and their DP distance
proved that the synthesized characters keep one’s writing style well. |
|
Chapters in Book
| [demura-09:2008] |
J. Watanabe, H. Demura, N. Hirata, and J. Terazono. SAISHIN
TSUKI NO KAGAKU - NOKOSARETA NAZO WO TOKU - (The
newest Lunar Science -To solve remained problems- in Japanese), page 219
pages. NHK Books, 6 2008. Demura’s parts: Forewords, Chapts. 2, 3, 4, 5, and Afterwords. 1–11, 55-152, 213– 219 |
Grants
| [naru-11:2008] |
T. Mukai, A. Nakamura, Y. Okada, and N. Hirata. Grant-in-Aid for
Scientific Research 18340133, 2006-2008. |
| [naru-12:2008] |
N. Hirata. Grant-in-Aid for Scientific Research 19549003, 2007-2008. |
Academic Activities
| [jpshin-03:2008] |
Jungpil Shin, June 2008. Member of the Program Committee, The 2008 International Conference on Knowledge Generation, Communication and Management (KGCM 2008) |
| [jpshin-04:2008] |
Jungpil Shin, Jan. 2008. Conference Co-Chair, The 2008 International Conference on Ubiquitous City Technology (ICUCT 2008) |
| [jpshin-05:2008] |
Jungpil Shin, Sep. 2008. Member of the Program Committee, The 2008 International Conference on Knowledge- Based and Intelligent Information & Engineering Systems (KES2008) |
| [jpshin-06:2008] |
Jungpil Shin, Sep. 2008. Member of the Program Committee, The Tenth International Conference on Ubiquitous Computing |
| [naru-13:2008] |
N. Hirata, 2008. Member, and member of the committee for general affairs, The Japanese Society for Planetary Sciences |
Ph.D, Master and Bachelor Theses
| [asada-19:2008] |
Manabu Kanzawa. Master Thesis: Online Geographic Information System
Supporting CollaborativeWork for Multipli Users, University of Aizu, 2008. Thesis Advisor: N. Asada, Co-referee: T. Hayashi and K. Naruse |
| [asada-20:2008] |
Naoto Miura. Master Thesis: Automatic Tracking of Glass Fragments
in High-Speed Camera Movies, University of Aizu, 2008. Thesis Advisor: N. Asada, Co-referee; R. Oka and T. Hayashi |
| [asada-21:2008] |
Shota Kikuchi. Master Thesis: Development of Operation Plan and Log
Management System for LISM on KAGUYA, University of Aizu, 2008. Thesis Advisor: N. Asada, Co-referee; S. Bhalla and K. Naruse |
| [asada-22:2008] |
Tomoki Hodokuma. Master Thesis: Integration of Lunar Digital Terrain
Model and Topographic Profile Data from Kaguya, University of Aizu, 2008. Thesis Advisor: N. Asada, Co-referee; R. Oka and N. Hirata |
| [jpshin-07:2008] |
Michikazu Kikugawa. Graduation Thesis: Shape retrieval with dendrogram,
one of the clustering method, University of Aizu, 2008. Thesis Advisor: Jungpil Shin |
| [jpshin-08:2008] |
Hiroshi Naito. Graduation Thesis:Detecting Alcohol using difference
character of on-line signature, University of Aizu, 2008. Thesis Advisor: Jungpil Shin |
| [jpshin-09:2008] |
Junichi Sato. Graduation Thesis: Font Generation which use Automatic
HANE Generation, University of Aizu, 2008. Thesis Advisor: Jungpil Shin |
| [jpshin-10:2008] |
Masahiro Honma. Graduation Thesis: On-line Recognition of Handwritten
Waseda Shorthand for Faster Recording of Japanese Text, University
of Aizu, 2008. Thesis Advisor: Jungpil Shin |
| [jpshin-11:2008] |
Yukari Sato. Graduation Thesis: Random Fonts Simulation, University
of Aizu, 2008. Thesis Advisor: Jungpil Shin |
| [jpshin-12:2008] |
Tomomi Kikuchi. Graduation Thesis: On-Line Signature Evaluation
Using Fuzzy Set Theory, University of Aizu, 2008. Thesis Advisor: Jungpil Shin |
