PPS04-01

Room:A03

Time:May 27 12:00-12:25

How we built ALMA
HASEGAWA, Tetsuo1∗
1National Astronomical Observatory of Japan

The Atacama Large Millimeter/submillimeter Array (ALMA), an international partnership of the European Organisation for
Astronomical Research in the Southern Hemisphere (ESO), the U.S. National Science Foundation (NSF) and the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Republic of Chile, is the largest astronomical project inexistence. ALMA is a single telescope of revolutionary design, composed initially of 66 high precision antennas located on the
Chajnantor plateau, 5000 meters altitude in northern Chile. The National Astronomical Observatory of Japan (NAOJ), a branchof NINS, is taking the role of the Executive for the 25% contribution from East Asia to the project. ALMA is now in its fulloperation and producing exciting scientific data, such as the astonishing image of the grooved protoplanetary disk surrounding
HL Tau.
In this paper, I will introduce the lights and shadows of this worldwide collaboration that built ALMA, based on my 7-year
experience in Chile working for the project.
Keywords: radio astronomy, ground-based, international collaboration, large project

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PPS04-02

Room:A03

Time:May 27 12:25-12:45

International collaboration in space solar physics
TSUNETA, Saku1∗
1

ISAS/JAXA

Before coming to ISAS on April, 2013, I had worked for the National Astronomical Observatory of Japan as an astronomer,
and had been involved in 4 satellites, 2 balloons, and 2 sounding rocket experiments. I have been observing the sun with thesemissions in the past 30 years.
I started my career with hard X-ray and gamma ray instrumentation in 1970s in ISAS Hinotori solar satellite as a graduate
student, then moving to the development of the soft X-ray telescope with NASA in 1980s for ISAS Yohkoh mission, proceeding
to the visible light space telescope again developed with NASA from late 1990s for ISAS Hinode satellite. I had proposed thebasic concepts of both the Yohkoh and the Hinode missions with my colleagues. Solar physics has been enjoying the golden age
in the past 25 years with Yohkoh and Hinode. In particular, very successful Yohkoh changed the dim scenery of the discipline,
and paved the way for series of space solar missions thereafter.
Yohkoh and GEOTAIL would be the first two missions for which NASA decided to work with Japan in a significant way. That
happened as early as 1986. Missions such as Hinode, Suzaku, ASCA, GEOTAIL and Yohkoh were tremendous success affecting
not only that disciplines but to all space science. International collaboration as a means to combine assets scattered in the world
namely good people, technology and money has to be pursued ever more in this turbulent era for the sake of science. ISAS/JAXA
is always seeing for collaboration with international partners for any ISAS/JAXA missions. We are also eager to participate in
missions led by foreign agencies.

Keywords: Space Science

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PPS04-03

Room:A03

Time:May 27 14:15-14:30

International collaboration driven by the STPP sub-committee under the Science Councilof Japan
OBARA, Takahiro1∗
1Planetary Plasma and Atmospheric Research Center

To date, the Solar Terrestrial Physics Program (STPP) sub-committee has been promoting and supporting several international
programs. For example, it supported International Heliophysical Year (IHY), a major initiative launched by the United Nations
from 2007 to 2009. In broad terms, IHY dealt with the solar system, paying a particular attention to the effects of the Sun on the
Earth’s upper atmosphere and on the space environment in the vicinity of the Earth. The United Nations Office for Outer Space
Affairs (UNOOSA) coordinated observation campaigns and drew scientists and engineers from all over the world to enhance its
Basic Space Science Initiative (BSSI). Several international workshops were organized by UNOOSA to advance the benefits of
IHY to all corners of the world. To maintain the international momentum created by IHY, UNOOSA developed the International
Space Weather Initiative (ISWI) to achieve more basic understanding of the solar terrestrial relationship. ISWI ran from 2010 to2014, and there was an international workshop for each year of ISWI (i.e., at Cairo, Abuja, Quito, and Graz).
From another vantage point, UNOOSA established in 2010 a new working group (WG): Long Term Sustainability of Outer
Space Activity (LTSOSA). This working group was created to cover a wide area: From the natural space environment (Space
Weather) to the artificial space environment (Space Delis). The LTSOSA WG set up four expert groups in 2011. Expert Groupfor Space Weather is one of the expert groups and the author (T. Obara) was assigned to be one of the co-chairs of the space
weather expert group.
The space weather expert group members gathered several times, and compiled a 50-page working group report (A/AC.105/C.1/2014/CRP
UN COPUOS REPORT, 2014). This report contains:
Identification of risks from space weather,
Observations, models, tools for space weather prediction,
Comprehensive network space weather services,
Coordination on data and services to safeguard space activities,
Engineering approaches to mitigate space environment effects,
Recommended guidelines for the long-term sustainability of space activities.
The Solar Terrestrial Physics Program (STPP) sub-committee of the Science Council of Japan has been in charge of theseUN-mandated programs for the interface with Japan. The STPP is considering to propose follow-on UN programs, and the STTP
is also considering to take on responsibility for other programs such as multinational and international space weather programs,
such as AOSWA (Asia Oceania Space Weather Alliance).
In this presentation, details shall be presented to give a better idea about the goals and functions of STPP.

Keywords: STPP sub-committee, the Science Council of Japan, International Collaboration, Past and Future

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PPS04-04

Room:A03

Time:May 27 14:30-14:45

Variability of the Sun and Its Terrestrial Impact (VarSITI): SCOSTEP’s scientific programin 2014-2018
SHIOKAWA, Kazuo1∗ ; GEORGIEVA, Katya2
1

Solar-Terrestrial Environment Laboratory, Nagoya University, 2 Space Research and Technologies Institute, Bulgarian Academyof Sciences
During the last solar minimum, solar activity was extremely low for an extended period, and the present maximum of sunspot
cycle 24 is the lowest in the last 100 years. It is not clear what long-term solar activity variations we can expect in the future:whether this is just the end of the recent decades of high solar activity, or whether the Sun is entering a Maunder-type minimum.
Moreover, it is not clear to what extend our present understanding of how the Sun influences the geospace - which is based on
instrumental observations taken during only the period of high solar activity in the second part of the 20th century - will holdduring periods of more moderate to low solar activity that may follow. And it is still more unclear how all this would affectglobal climate change, or how important becomes the penetration of various inputs from the Earth’s lower atmosphere to theionosphere and plasmasphere. In 2014-2018 the Scientific Committee On Solar-TErrestrial Physics (SCOSTEP) operates thescientific program ”Variability of the Sun and Its Terrestrial Impact” (VarSITI) which will focus on the recent and expected
future solar activity and its consequences for the Earth, for various time scales from the order of thousands years to milliseconds,
and for various locations and their connections from the solar interior to the Earth’s atmosphere. In order to elucidate thesevarious Sun-Earth connections, we encourage much closer communications between solar scientists (solar interior, atmosphere,
and heliosphere) and geospace scientists (magnetosphere, ionosphere, and atmosphere). Campaign observations/data analysis forparticular intervals, VarSITI web pages (http://www.varsiti.org/), mailing lists, and newsletters, are developed for this purpose.
Four scientific projects are carried out under the VarSITI program: (1) Solar Evolution and Extrema (SEE), (2) International Studyof Earth-Affecting Solar Transients (ISEST/MiniMax24), (3) Specification and Prediction of the Coupled Inner-Magnetospheric
Environment (SPeCIMEN), and (4) Role Of the Sun and the Middle atmosphere/thermosphere/ionosphere In Climate (ROSMIC).
These four projects will be carried out in collaboration with relevant satellite and ground-based missions as well as modeling
efforts to facilitate the implementation of the projects. We will also discuss the collaboration with other on-going international
projects like the UN-based space weather activities, particularly for promoting VarSITI-related science in developing countries,
and ICSU World Data System (ICSU-WDS).
Keywords: VarSITI, solar activity, climate change, heliosphere, magnetosphere, atmosphere

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PPS04-05

Room:A03

Time:May 27 14:45-15:00

The International Space Weather Initiative (ISWI)GOPALSWAMY, Nat1∗ ; YOSHIKAWA, Akimasa2
1

NASA Goddard Space Flight Center, 2 ICSWSE, Kyushu University

The International Space Weather Initiative (ISWI) is a scientific program of global cooperation to understand the external
drivers of space weather. The science and applications of space weather has been brought to prominence because of the rapid
development of space based technology that is useful for all human beings. The ISWI program has its roots in the successful
International Heliophysical Year (IHY) program that ran during 2007 - 2009. The primary objective of the ISWI program isto advance the space weather science by a combination of instrument deployment, analysis and interpretation of space weather
data from the deployed instruments in conjunction with space data, and communicate the results to the public and students. Like
the IHY, the ISWI will be a grass roots organization with key participation from national coordinators in cooperation with aninternational steering committee. There have been more than 1000 deployments from 17 instrument concepts forming several
instrument networks. This talk outlines the ISWI program including its organization and summarizes a few scientific results.

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PPS04-06

Room:A03

Time:May 27 15:00-15:20

International collaboration in ground-based magnetometer observations via ULTIMA: A
tribute to Professor Kiyohumi Yumoto
CHI, Peter1∗ ; YOSHIKAWA, Akimasa2 ; MANN, Ian31
3

Department of Earth Planetary and Space Sciences, UCLA, 2 Department of Earth and Planetary Sciences, Kyushu University,
Department of Physics, University of Alberta

Ground-based magnetometers provide not only the measurements of the geomagnetic field but also integrative information
about of the electric currents in the magnetosphere and the ionosphere, revealing the dynamics of the magnetic storms, substorms, and various types of MHD and plasma waves in the geospace. Ground-based magnetometers are installed and operated
by university teams and government agencies, most of which manage regional arrays for specific scientific objectives or national
interests. Nonetheless, a global network of ground-based magnetometers is required to understand the complex geospace and its
response to solar activity.
As the Principal Investigator of the world’s largest magnetometer array operated by a single group, Professor Kiyohumi Yumoto envisioned that international collaboration was the only way to global magnetometer observations. In 2006, he and six othermagnetometer arrays in Australia, Canada, and the United States founded the Ultra Large Terrestrial International Magnetometer
Array (ULTIMA) consortium, of which he was elected as the first Chair. The main objective of ULTIMA is to promote collaborative research on the magnetosphere, ionosphere, and upper atmosphere through the use of ground-based magnetic observatories.
The number of ULTIMA members doubled in size during Professor Yumoto’s tenure between 2006 and 2014. Today, ULTIMA
consists of 17 member arrays with over 250 stations located in all continents of the world. ULTIMA also received recognition
from the International Association of Geomagnetism and Aeronomy (IAGA) in 2013.
We present a review of the establishment and development of ULTIMA, as well as lessons learned regarding collaboration
among magnetometer teams in multiple nations. As geospace research has moved into a new era where collaborative opportunities among different types of observations are growing, we also demonstrate ongoing and upcoming synergetic activities
participated by ULTIMA.

Keywords: ground-based magnetometers, ULTIMA, international collaboration, magnetic field, geospace

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PPS04-07

Room:A03

Time:May 27 15:20-15:40

BepiColombo Euro-Japan Joint mission to Mercury
HAYAKAWA, Hajime1∗ ; MAEJIMA, Hironori1
1

ISAS/JAXA

BepiColombo is a ESA-JAXA joint mission to Mercury with the aim to understand the process of planetary formation andevolution in the hottest part of the proto-planetary nebula as well as to understand similarities and differences between themagnetospheres of Mercury and Earth.
The baseline mission consists of two spacecraft, i.e. the Mercury Planetary Orbiter (MPO) and the Mercury MagnetosphericOrbiter (MMO). JAXA is responsible for the development and operation of MMO, while ESA is responsible for the development
and operation of MPO as well as the launch, transport, and the insertion of two spacecraft into their dedicated orbits.
MMO is designed as a spin-stabilized spacecraft to be placed in a 400 km x 12000 km polar orbit. The spacecraft willaccommodate instruments mostly dedicated to the study of the magnetic field, waves, and particles near Mercury. While MPO is
designed as a 3-axis stabilized spacecraft to be placed in a 400km x 1500 km polar orbit. Both spacecraft will be in same orbital
plane.
Critical Design Review(CDR) for MMO project is completed in November 2011 while ESA Spacecraft CDR is completed in
Novemver 2013. MMO stand alone FM AIV is expected to be finished on early March this year. MMO FM will be transported
to ESA/ESTEC on April. After some stand alone activity for MMO, JAXA will handover MMO to ESA to attend stack level(MCS) final AIV. BepiColombo is expected to be launched in summer 2016.
BepiColombo science working team (SWT) meeting, which discusses science related matters, is held once a year. In thispaper, BepiColombo project as a test case of large collaboration between ESA and JAXA will be reported.

Keywords: Mercury, Planetary Exploration, International Collaboration

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PPS04-08

Room:A03

Time:May 27 15:40-16:00

STRATEGIC MAP FOR EXPLORING THE OCEAN-WORLD ENCELADUS
SHERWOOD, Brent1∗
1

Jet Propulsion Laboratory, California Institute of Technology

Introduction: Cassini’s discovery of jets emitting salty water from the Saturn’s small moon Enceladus is one of its mostastounding results. Measurement of salts and organic species in the resulting plume, finding that tidal stretching at apocrone
valves the jet activity, modeled lifetime of E-ring particles, and gravitational inference of a long-lived, large water reservoir
in contact with the rock core all indicate that Enceladus meets textbook conditions for habitability: liquid water, biologicallyavailable elements, energy source, and longevity of conducive conditions. Enceladus is among the best places in our solar system
to search for direct evidence of biomarkers.
Exploring an ocean world: Enceladus also proffers the simplest access by a flight mission to telltale molecules, ions, isotopes,
and potential cytofragments, since its plume continuously expresses material from the ocean directly into space. In situ mass
spectroscopy of the plume, plume sample return, in situ investigation of plume snow on the surface, direct sulcus and ventexploration, and eventually submarine exploration can all be envisioned.
However, the strategic urgency and feasibility of planning and funding elaborate in situ exploration of this ocean world will
hinge on new data revealing promising results. The very first steps of the roadmap are pivotal.
Two straightforward mission concepts, one Discovery-class and one New Frontiers-class, are: flythrough plume analysis using
gas and particle mass spectrometers, upgrading the Cassini INMS and CDA measurements but with modern, high-resolution
instruments; and collection of plume ice particles, dust, and gas upon Stardust-like flythrough, followed by sample retrieval forcomprehensive analysis in terrestrial laboratories.
Building a strategic map: The mission waypoints on an integrated strategic map each require unique capabilities, address
focused science questions, and yield results important for setting priorities and making subsequent in-vestments. However,overlaid on this logical sequence are important, mutually competing programmatic constraints: astrobiology pursuits at otherocean worlds and Mars, and exoplanet spectroscopy; cadence of realistic opportunities for mission selections and formal sciencecommunity planning cycles via Decadal Surveys; programmatic and even popular impatience to await interim results before
vectoring investments in enabling capabilities; and alignment of US exploration strategies with international partner goals. As
with Mars for many years, anticipation of interesting eventual results may be a key driver of strategic intent, able to withstandabsence of validation for many years. And as for major exploration pursuits like Cassini-Huygens and the International Space
Station, synergy among international partners may prove key for establishing and sustaining programmatic intent and momentum.
Key enabling elements for long-term exploration of the ocean-world Enceladus include: coherent sequence of science questions
addressable by various type of mission; technologies that mature at the right time to enable both mission performance andapproval (e.g., planetary protection); integrated concepts whose cost estimates survive review; lessons learned from analog
exploration (e.g., terrestrial oceanography and extremophile research), and community momentum and international partnerships.
Decision levers and opportunities for action: Analysis of these elements of the strategic map yields a short list of decisionpressure points for the next two decades. Using these opportunities the community may systematically prosecute the grandobjective of finding and exploring an alien ecosystem within the working lifetime of today’s graduate students. If missed,
however, progress toward an age of comparative ocean exploration will be episodic, haphazard, and slow. Windows for making
significant advances are sparse, and much remains to be done to prepare to take advantage of them.
Keywords: Enceladus, ocean world, life, plume, in situ, sample return

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PPS04-09

Room:A03

Time:May 27 16:15-16:30

New Challenges in Planetary Protection for International Astrobiology-Driven Explorations
YANO, Hajime1∗
1

Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency

Planetary protection is an international and interdisciplinary activity among scientific, technological, operational and administrative countermeasures to preserve biospheres of both the Earth and exploration targets, should they have a scientific potential
to have one, including Mars and some icy satellites of Jupiter and Saturn such as Europa, Ganymede, Enceladus and Tian. It
also deals with all sample return missions to assess risks of each returned sample if they may endanger the terrestrial biosphere,according to a scientifically internationally agreed evaluation process endorsed by COSPAR Planetary Protection Panel, theworldwide authority to which all major spaced agencies follow their compliance.
In the coming decades, deep space exploration will focus on astrobiology-driven missions more than ever. Thus international
space exploration community must work closely with the planetary protection issues of following respective missions to makethem an enabler, rather than a show stopper.
Mars exploration now faces how to prevent terrestrial contamination at potentially inhabited regions like recurring slope lineae
in order to search for direct evidence of indigenous life there. Also human landing and habitation, no matter sortie for the NASAplan or even permanently for Mars One, pauses serious contradiction with robotic life detection missions.
D/P-type asteroids such as the Martian satellites and Jupiter Trojans are now considered to be realistic targets for next generation robotic sample return missions while they still lack definite analog meteoritic samples on the earth, unlike S-type and C-type
asteroids. Their present status of the restricted Earth return must be re-evaluated with the most updated scientific knowledge
today, before COSPAR will endorse any of these sample return missions.
Sample returns of plume particles from icy bodies are a game changer of deep habitat research. Yet there have been few studies of planetary protection and contamination/alteration control at the sampling, return cruising, earth re-entry and subsequent
laboratory analyses.
This presentation explains the above challenges and summarizes current efforts and future prospects how to overcome them.

Keywords: Planetary Protection, Sample Return, Mars, Icy Plumes, D/P-type Asteroids, COSPAR

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PPS04-10

Room:A03

Time:May 27 16:30-16:45

Hayabusa 2 and OSIRIS-REx: international collaborations on sample retrun missions
CONNOLLY JR., Harold C.1∗ ; LAURETTA, Dante S.2 ; TACHIBANA, Shogo1 ; YOSHIKAWA, Makoto3
1

Dept. of Natural History, Hokkaido Univ. Sapporo 060-0810, Japan, 2 LPL, Univ. of Arizona, Tucson, AZ 85721, USA, 3 ISAS,
JAXA, Sagamihara, Kanagawa 252-5210 JapanThe Origins Spectral Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) asteroid sample
return mission was selected by NASA in May 2011 as the third New Frontiers mission. The target, (101955) Bennu, is a Btype asteroid, hypothesized to be similar to CI or CM carbonaceous chondrites. The key science objectives of the mission aresummarized in [1] with the major goal of returning pristine asteroid regolith. It is scheduled to launch in September 2016.
Hayabusa2 is an asteroid sample return mission to the C-type asteroid, 1999 JU3 , and builds off of the successful Hayabusa
mission, the first mission to return a sample from an asteroid. Hayabusa2 launched in December 2014.
The OSIRIS-REx science team is an international team including Co-Is and collaborators from the United States, Canada,
France, and the United Kingdom with the Canadian Space Agency contributing an instrument (OSIRIS-REx Laser Altimeter)
to the mission [2]. In addition, in November 2014, a Memorandum of Understanding (MOU) was signed between NASA andJAXA for cooperation between the Hayabusa2 and OSIRIS-REX missions. The Hayabusa2 science team is an internationalteam including Co-Is and collaborators from Japan, Germany, France, the United States, Korea, the United Kingdom, Australia,
Switzerland, and Italy. A lander MASCOT (Mobile Asteroid Surface Scout) for the Hayabusa2 was developed by DLR and
CNES [3].
The official collaboration between the Hayabusa2 and OSIRIS-REx as defined in the MOU presents an important series ofchallenges for both missions. These challenges focus on sharing data from both science and engineering elements of the mission,
including during asteroid operations and, ultimately, sample analysis and actual returned samples. It also provides an opportunity
for the two missions to learn about each cultural systems and how both science and engineering are approached from the humanelement. The two projects will develop a mutually agreed upon Joint Sample Exchange Curation and Analysis Plan that will
support the mutual participation of scientist in both missions.
Hayabusa2 and OSIRIS-REx are sample return missions, and the exchange of samples between the two agencies will occur,building on lessons learned from the past. From JAXA, a total of 10% by mass of a representative and unprocessed portion of
the returned Hayabusa2 sample will be jointly separated for full transfer to NASA no later than 1 year after Earth return. NASAwill deliver a total of 0.5% by mass of the OSIRIS-REx sample no later than 1 year after Earth return and will jointly separate a
representative and unprocessed sample. A key challenge for the two missions and agencies will be to determine and agree upon
what constitutes a representative sample, in part because any agreed upon criteria for establishing what is representative could
inevitably need to be re-evaluated upon sample return do to unexpected results in sampling.
[1] Lauretta et al. (2014) The OSIRIS-REx Target Asteroid 101955 Bennu: Constraints on its Physical, Geological, andDynamical Nature from Astronomical Observations. Meteorit. Planet. Sci. 49. [2] Dickinson et al. (2012) AN OVERVIEW OF
THE OSIRIS REX LASER ALTIMETER OLA. 43rd LPSC 1447. [3] Lange et al. 7th International Planetary Probe Workshop
Proceedings, Barcelona, Spain. 2010.

Keywords: OSIRIS-REx, Hayabusa2, Sample Return, Missions, NASA, JAXA

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PPS04-11

Room:A03

Time:May 27 16:45-17:00

The Nautilus Space Mission: Unveiling the Origin of the Diversity of the Asteroid Beltand of Earth Water
LAMY, Philippe1∗ ; VERNAZZA, P1 ; CASTILLO-ROGEZ, J2 ; BECK, P3 ; NAUTILUS, Team41
4

Laboratoire Astrophysique de Marseille, 2 Jet Propulsion Laboratory, 3 Institut de Planetologie et d’Astrophysique de Grenoble,
Nautilus TeamWe present the Nautilus space mission recently proposed to ESA in the framework of the M4 call. The overarching science
goal of the Nautilus mission, proposed by a team of European scientists with a strong participation of US scientists and otherinternational scientists, is to explore a volatile-rich asteroid not represented in our meteorite collections (C- or D-type), andultimately cast light on these aspects of the early history of the solar system. Its payload will allow performing high resolution
imaging, ultra-violet, visible, near-infrared, mid-infrared and microwave spectroscopy, mass spectrometry of the gas phase,magnetic field measurements, and radio science. This proposal is supported by a team of ˜170 scientists that includes prominent,
world-class experts of primitive solar system bodies and of space instrumentation. In this presentation, we will highlight thechallenges of this space mission and invite broader support from the international community.

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PPS04-12

Room:A03

Time:May 27 17:00-17:15

Personal involvement in the international astronomical projects
ABE, Shinsuke1∗
1

Department of Aerospace Engineering, Nihon University

International collaboration is the key to lead the large-scale mission to the success. The large-scale project or big-science
projects require coordinating multi-country teams and the budget. There are several ways to be involved in such a big project evenan individual researcher can join. Here I will present my experiences, individual participation, such as (1) NASA Leonid MAC(Multi-Instrument Aircraft Campaign) which brought ˜50 researchers from nine countries together in two aircraft to observe
the Leonid meteor storms, (2) Pan-STARRS1 sky survey telescopic project on Mount Haleakala in Hawaii operated by the
consortium which was made up of astronomers from 10 institutions from four countries (Japan was not included), (3) Asteroid
sample return mission Hayabusa and so on.
Keywords: Asteroids, Comets, Meteors, International projets

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PPS04-13

Room:A03

Time:May 27 17:15-17:30

Telescopes Dedicated to the Observations of Planets and Exoplanets at Haleakala, Hawaii
KASABA, Yasumasa1∗ ; SAKANOI, Takeshi1 ; NAKAGAWA, Hiromu1 ; KAGITANI, Masato1 ; OBARA, Takahiro1 ;OKANO, Shoichi2 ; JEFF, Kuhn2 ; YONEDA, Mizuki3 ; BERDYUGINA, Svetlana3
1

Tohoku Univ., 2 IfA, Univ. Hawaii, 3 Kiepenheuer Institute for Solar Physics

In this paper, we introduce the University-sized small but unique telescope project at the summit of Mt. Haleakala of Maui
Island, Hawaii.
Clear sky and good seeing condition are definitely important for any ground-based observations. The Haleakala High Altitude
Observatories at the summit of Mt. Haleakala is not the highest place (3050m), but one of the best sites with clear sky, goodseeing, and low humidity conditions. Operation is relatively easy because we can access to the airport, major towns, and a goodengineering facility, ATRC (Advanced Technology Research Center) of IfA/UH within 1-2 hour drive from summit.
On the summit, our group has been operating a 40 cm Schmidt-Cassegrain telescope (T40), observing faint atmosphericfeatures such as Io torus, Mercury, Lunar sodium tail, and so on. From fall 2013, ISAS Hisaki/Exceed EUV space telescope runon the orbit. The T40 telescope has uniquely provided long-term Io torus activities for this project. T40 will also link to Juno
mission that will start Jovian observation from 2016.
Atmospheres and its escapes from planets and exoplanets are next extensions. From the late 2000s, we started the project todevelop the telescope dedicated to planets and exoplanets, under the international consortium formed with IfA/UH and several
groups in USA, Mexico, Canada, and Europe. This telescope project consists of several parts: The main is the new constructionof the 1.8m off-axis telescope named PLANETS.
Associated with this project, we also moved our 60 cm telescope (T60) from Tohoku Univ. Iitate Observatory, and started theoperation from Sep. 2014. T60 is equatorial-mount Cassegrain telescope. By the acceptance of this move by IfA, we adjusted
its mount angle to the Hawaiian latitude, and moved to Haleakala in spring of 2014. This telescope can observe infrared lightcovering many molecular lines in planetary atmospheres. This telescope has Coude focus that can allow relatively large-sized
instruments. Using this feature, our telescope is now providing the first capability of long-term operation of Infrared heterodyne
spectrometer (MIRAHI) developed by us. It can achieve the spectral resolution of ˜107, and resolve the atmospheric lines behind
the terrestrial absorption lines and atmospheric velocity field in several 10 m/s resolutions. With other instruments, Venus, Mars,and Jupiter observations are planned in 2015. They will be linked to the observations of orbiter projects like Mars Express,
MAVEN, Mars Trace Gas orbiter for Mars and Akatsuki for Venus, like T40 linked to Jupiter.
The 1.8m PLANETS (Polarized Light from Atmospheres of Nearby Extra Terrestrial Planets) telescope will have the first lightin 2016 in the earliest case. It has an off-axis primary mirror (provided from Tohoku Univ.) with a diameter of 1.8 m. By thetelescope structure optimization, we can avoid diffraction due to a spider structure that holds a secondary mirror and to minimize
the scattered light from mirror surfaces as far as possible. With the instruments set to Gregorian focus on an equatorial mount, it
can provide us a unique facility for spectroscopic and polarimetric observations of faint environments around the bright bodies,like planetary environments, stellar disks, etc.
T60 has also equatorial mount, and provides a test bench of instruments for PLANETS. One of examples is the exoplanet
polarimetric instrument ’DiPol2’, which tries to detect the reflected polarized light from exoplanet in the non-polarized motherstar continuum. This test run was also from Jan 2015.
It is welcomed to any planet and exoplanet observation scientists who have interest to use our facility or expect to attach theirown instruments for specific objectives. For promoting such activities, M. Kagitani, H. Nakagawa, and M. Yoneda stay in or visit
frequently to Maui, and are contributing to the telescope/instrumental operations and developments.

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PPS04-14

Room:A03

Time:May 27 17:30-17:45

International Cooperation in NAOJ Mizusawa : Result of Kaguya, and possibility in the
future.
HANADA, Hideo1∗
1

RISE Project, National Astronomical Observatory of Japan

In the Japanese lunar explorer SELENE (Kaguya), which was launched on September
14th, 2007, VLBI observations were made for the purpose of improvement of the lunar gravity field model, through an international network as well as Japanese VERA (VLBI Exploration of Radio Astrometry) network. The international network consistsof Shanghai and Urumqi (China), Wettzell (Germany)and Hobart (Australia) stations. They participated in VLBI observations,data reduction and data analysis based on the MOU for cooperative research, and the cooperation contributed not only to thesuccess of Kaguya mission but to produce more scientific results.
RISE project of NAOJ (National Astronomical Observatoryof Japan) were continuing the cooperation with Shanghai Astronomical Observatory, Xinjian Observatory (China) and Kazan Federal University (Russia) before Kaguya mission in the fieldof space geodesy, selenodesy, geodynamics and geophysics, astronomy and astrophysics. The International Earth Rotation andReference Systems Service (IERS) which Mizusawa observatory contributed for long years is one of the basis of these cooperative researches. These cooperative researches are continuing for future lunar and planetary missions by exchange researchersand students and having international meetings.

Keywords: International cooperation, MOU, VLBI, Earth rotation, Space geodesy, Lunar mission

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PPS04-P01

Room:Convention Hall

Time:May 27 18:15-19:30

Activities of SCOSTEP (Scientific Committee on Solar-Terrestrial Physics)
NAKAMURA, Takuji1∗
1

NIPR

The Scientific Committee on Solar Terrestrial Physics (SCOSTEP) is an interdisciplinary body of the International Council
for Science (ICSU). The main task of the committee is to organize and conduct international program on solar-terrestrial physics(STP) of finite duration in cooperation with other ICSU bodies. The committee was founded in 1966, and has carried out
various international programs such as International Magnetospheric Study (IMS: 1976-79); Solar Maximum Year (SMY: 197981); Middle Atmosphere Program (MAP: 1982-85); and Solar-Terrestrial Energy Program (STEP: 1990-97). Four Post-STEP
programmes over the period 1998-2002 include: STEP-Results, Applications, and Modeling Phase (SRAMP); International Solar
Cycle Study (ISCS); Planetary Scale Mesopause Observing System (PSMOS); and Equatorial Processes Including Coupling(EPIC ). After that, Climate and Weather of the Sun-Earth System (CAWSES: 2004-2008) and CAWSES-II(2009-2013) werecarried out. Detail of the current program, VarSITI (Variability of the Sun and Its Terrestrial Impact) will be presented by anothertalk, but this paper will introduces the history, the structure and the activities of SCOSTEP, and relations with other international
bodies.
Keywords: Sun, Earth, SCOSTEP, Earth and planets

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PPS04-P02

Room:Convention Hall

Time:May 27 18:15-19:30

COSPAR (The COmmittee on SPace Research)
SASAKI, Sho1∗
1

Dept. Earth and Space Science, Osaka University

The COmmittee on SPAce Research (COSPAR), frequently consdiered as ”International Union of Space Sciences”, was established by the International Council of Scientific Unions (ICSU) in October 1958 to continue the cooperative programmes ofrocket and satellite research successfully undertaken during the International Geophysical Year of 1957-58. The ICSU resolution
creating COSPAR stated that the primary purpose of COSPAR was to provide the world scientific community with the means
whereby it may exploit the possibilities of satellites and space probes of all kinds for scientific purposes, and exchange the resulting data on a cooperative basis. Therefore, COSPAR is an interdisciplinary scientific organization concerned with progress on aninternational scale of all kinds of scientific investigations carried out with space vehicles, rockets and balloons.COSPAR’s objectives are carried out by the international community of scientists working through ICSU and its adhering national academies andinternational scientific unions. Under the rules of ICSU, COSPAR ignores political considerations and considers all questions
solely from the scientific viewpoint.
COSPAR has 8 scientific commisions and several panels:
Commission A Space Studies of the Earth’s Surface, Meteorology and Climate
Commission B Space Studies of the Earth-Moon System, Planets, and Small Bodies of the Solar System
Commission C Space Studies of the Upper Atmospheres of the Earth and Planets Including Reference Atmospheres
Commission D Space Plasmas in the Solar System, Including Planetary Magnetospheres
Commission E Research in Astrophysics from Space
Commission F Life Sciences as Related to Space
Commission G Materials Sciences in Space
Commission H Fundamental Physics in SpaceThe main event of COSPAR is biannual scientific assembly, where usually more than 2000 scientists gather from all over theworld. In Japan, COSPAR activity is supported by Science Council of Japan.

Keywords: space sciences, international collaboration, scientific satellites, balloon experiments, solar system explorations, microgravity experiments

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PPS04-P03

Room:Convention Hall

Time:May 27 18:15-19:30

Introduction to MAGDAS of ICSWSE and to International Capacity Building of ISWIYOSHIKAWA, Akimasa1∗
1

International Center for Space Weather Science and Education, Kyushu University

ISWI stands for International Space Weather Initiative. It is a global scientific effort to advance space weather research by
involving developing nations. Space weather research requires data from ground-based observation from all over the world. Thisrequires the cooperation of developing nations. To enable this, developed nations must support education efforts in developing
nations – this is International Capacity Building. ISWI makes use of existing ground-based arrays. One such array is MAGDAS,
which has 72 magnetometers installed all over the world. The MAGDAS Project is managed by ICSWSE of Kyushu University.
The contributions of MAGDAS to ISWI are outlined in this talk. It is the hope of ICSWSE that the members of AOSWA and otherresearchers of Asia will join the International Space Weather Initiative, which was initially established by the United Nations.
Keywords: ISWI, Capacity Building, Asia and Africa, MAGDAS

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PPS04-P04

Room:Convention Hall

Time:May 27 18:15-19:30

Science objectives and implementation of Software-type Wave-Particle Interaction Analyzer (SWPIA) by RPWI for JUICE
KATOH, Yuto1∗ ; KOJIMA, Hirotsugu2 ; ASAMURA, Kazushi3 ; KASABA, Yasumasa1 ; TSUCHIYA, Fuminori1 ;KASAHARA, Yoshiya4 ; IMACHI, Tomohiko4 ; MISAWA, Hiroaki1 ; KUMAMOTO, Atsushi1 ; YAGITANI, Satoshi4 ;ISHISAKA, Keigo5 ; KIMURA, Tomoki3 ; MIYOSHI, Yoshizumi6 ; RPWI-JAPAN, Team1
1
4

Graduate School of Science, Tohoku University, 2 Research Institute for Sustainable Humanosphere, Kyoto University, 3 ISAS/JAXA,
Univ. Kanazawa, 5 Toyama Pref. Univ., 6 STEL, Nagoya Univ.

We present science objectives of Software-type Wave-Particle Interaction Analyzer (SWPIA), which will be realized as a software function of Langmuir probes (LP) running on the DPU of RPWI (Radio and Plasma Waves Investigation; PI: J.-E. Wahlund,
IRF-Uppsala, Sweden) for the ESA JUICE mission. SWPIA conducts onboard computations of physical quantities indicating
the energy exchange between plasma waves and energetic ions. SWPIA cannot be achieved without onboard inter-instruments
communications, which will be realized by efforts of RPWI, PEP (Particle Environment Package; PI: Stas Barabash, IR-Kiruna,
Sweden) and J-MAG (JUICE Magnetometer; PI: M. Dougherty, ICL, UK). By providing the direct evidence of ion energization
processes by plasma waves around Jovian satellites, SWPIA contributes scientific output of JUICE as much as possible withkeeping its impact on the telemetry data size to a minimum.
SWPIA measures the energy transfer process between energetic particles and electromagnetic plasma waves [Fukuhara et al.,EPS 2009; Katoh et al., AnGeo 2013]. SWPIA will be firstly realized in the ERG satellite mission in the Earth’s inner magnetosphere to measure interactions between energetic electrons and whistler-mode chorus. We will apply SWPIA to ion-scalewave-particle interactions occurring in the Jovian magnetosphere. SWPIA clarifies where/when/how heavy ions are energized bywaves in the region close to Ganymede and other Jovian satellites. In SWPIA of RPWI for JUICE, we focus on the interactions
between energetic ions (a few to tens of keV) and ion cyclotron waves (typically less than 1 Hz). SWPIA uses wave electromagnetic field and ion velocity vectors provided by RPWI sensors and PEP, respectively, with referring three-components of the
background magnetic field detected by J-MAG. SWPIA measures a relative phase angle between the velocity vector vi of i-th
particle of charge qi and the wave electric field vector at the timing of particle’s detection (E(ti )) and computes an inner productof W(ti ) = qi E(ti ) · vi , where W(ti ) corresponds∑ to the variation of the kinetic energy of the i-th energetic particle. We accumulate
W for detected particles to obtain Wint = i W(ti ), and we expect statistically significant values of Wint for the case of themeasurement at the site of efficient wave-particle interactions. In this presentation, we discuss details of the implementation of
SWPIA of RPWI and inter-instruments communications among RPWI-PEP-J-MAG of JUICE.
Keywords: Jovian magnetosphere, Jovian satellite, wave-particle interactions

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PPS04-P05

Room:Convention Hall

Time:May 27 18:15-19:30

THE ATMOSPHERIC CHARACTERIZATION FOR EXPLORATION AND SCIENCE(ACES) INSTRUMENT SUITE FOR MARS.
RAFKIN, Scot1∗ ; BANFIELD, Don2 ; ANDREWS, John1 ; NOWICKI, Keith1 ; CASE, Traci1 ; DISSLY, Richard3 ;DWYER-CIANCIOLO, Alicia4 ; FENTON, Lori5 ; GENZER, Maria6 ; KARATEKIN, Ozgur7 ; LANGE, Carlos8 ;MERRISON, John9 ; NEAL, Kerry115Southwest Research Institute, 2 Cornell University, 3 Ball Aerospace and Technology Corp., 4 NASA Langley Research Center,
SETI, 6 Finnish Meteorological Institute, 7 Royal Belgian Observatory, 8 University of Alberta, 9 University of Aarhus

The Atmospheric Characterization for Exploration and Science (ACES) instrument suite is designed to address the highest
priority, lower atmosphere goals and investigations identified by MEPAG[1] and to address both exploration technology Strategic Knowledge Gaps (SKGs)[2]. The ACES instrument suite measures atmospheric dust properties, fundamental atmosphericparameters, and the energy inputs that drive the atmosphere in ways that far exceed previous landed experiments.
The data to be returned by ACES is the compre-hensive and necessary type of information that has been sought after by
the atmospheric, aeolian, and Entry, Descent, and Landing (EDL) communities since the Viking Landers provided the first in
situ glimpse of Martian meteorology. The intervening experiments since Viking have only marginally increased the knowledge
necessary to address Mars Exploration Program and Human Exploration and Operations Mission Directorate (HEOMD) goals;
continuing to repeat these meteorological experiments is an exercise in diminishing returns.
In addition to temperature, pressure, and relative humidity, ACES measures for the first time airborne particle concentrationand size distribution, 3D wind components, and infrared and visible radiative fluxes. By combining the unique capabilities of
ACES to de-termine turbulent eddy momentum fluxes and dust characteristics, ACES also measures the wind stress that lifts
sand and dust.
The ACES instrument sensors may be accomodat-ed on a rover (Figure 1) or an a stationary lander. A boom for wind andtemperature and in some cases vis and IR radiation flux minimizes potential thermal, mechanical and radiative contamination by
the space-craft.
ACES is strengthened by internationally contribut-ed sensors and electronics from the U.S.A., Finland, Denmark, Canada, andBelgium. The ACES science team is comprised of exceptional scientists and engi-neers from each of these countries.
Details on the capabilities and response of each in-strument, power requirements, accommodation, ob-servation strategy, anddata products and volume will be detailed in the talk.
References[1] MEPAG (2008), Mars Scientific Goals, Objectives, Investigations, and Priorities: 2008, J.R. Johnson, ed. [2] Precursor
Strategy Analysis Group (P-SAG) (2012) Report.

Keywords: Mars, Meteorology, Atmosphere, Instrumentation, Mars Mission

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PPS04-P05

Room:Convention Hall

Time:May 27 18:15-19:30

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PPS04-P06

Room:Convention Hall

Time:May 27 18:15-19:30

International collaboration in planetary and space sciences: Past, present, and future
SASAKI, Sho1∗ ; YOSHIKAWA, Akimasa21Dept. Earth and Space Science, Osaka University, 2 Dept. Earth and Planetary Sciences, Kyushu University

International collaborations are becoming an important aspect of successful planetary and space science projects. In today’s
research environment, scientists and engineers from all over the world must work increasingly together in a variety of research
projects, including ground-based observations, laboratory experiments, data analyses, archival studies, and numerical experiments. For future advancements in planetary and space sciences, it is important to consider the role of international collaboration, and facilitate interactions among researchers at all career levels from countries all over the world. However, international
collaboration comes with its own set of challenges.
Here in this session, we discuss recent recent achievements and current status of various international projects and also we
confirm roles of international organizations which are mostly scientifically-oriented.
Keywords: planetary and space sciences, international collaborationo

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