1

Third JSPS Forum in France “The Universe:

Origin, Evolution, Future”

- Scientific Program -

Friday 19 November 2004 JSPS Strasbourg Office, Université Louis Pasteur

Strasbourg, France

1

The JSPS third forum is organised by:

JSPS Strasbourg Office, Université Louis Pasteur

With the support of:

Ministère délégué à la Recherche

Conseil Général du Bas-Rhin

Friday 19th November 2004

Atrium Building

Campus Universitaire de l’Esplanade Organizing Committee: Michel GRANET, Jean-Marie HAMEURY, Yoichi NAKATANI, Yuriko SEKI Scientific Adviser: Patrick PETITJEAN Assistants: Marie PASCHAKI, Julien BOUISSAC Technical Assistants: ULP Multimédia

Video of the forum is available on Canal U, the web-TV of French Ministry of Education and Research http://www.canal-u.education.fr/

1

PROGRAM

2

“The Universe: Origin, Evolution, Future” Third JSPS Forum in France

Friday 19th November 2004

08:30 – 09:30 Registration and Coffee 09:30 – 10:00 Opening: Welcome address Prof. Bernard CARRIERE President, Université Louis Pasteur Mr. Ryuichi SHOJI Consul General of Japan in Strasbourg Prof. Jean-Paul MONTAGNER Deputy Director of Research, Ministère de la Recherche Mr. Philippe RICHERT President, Conseil Général du Bas-Rhin Prof. Motoyuki ONO President, JSPS 10:00 – 10:50 Chairman : Prof. Jean-Luc ATTEIA, Observatoire Midi-Pyrenees

“Exploring the New Frontier: Human Space flight” Prof. Chiaki MUKAI

JAXA Astronaut, International Space University

10:50 – 11:10 Coffee break 11:10 – 12:00 Chairman : Prof. Tetsuichi ITO, International Space University

“Fundamental physics and the cosmic microwave background (CMB) observations” Prof. Jean-Loup PUGET Université Paris Sud

12:00 – 12:30 Presentation of JSPS Alumni Association Prof. Marie-Claire LETT Université Louis Pasteur President of JSPS Alumini Association

12:30 – 14:30 Lunch & Poster session

3

14:30 – 15:00 Presentation of JSPS International Scientific Cooperation

Ms. Yuriko SEKI Deputy Director, JSPS Strasbourg Office 15:00 – 15:50 Chairman: Prof. Olivier BIENAYME, Observatoire de Strasbourg

“Probing the Era of Galaxy Formation” Prof. Sadanori OKAMURA University of Tokyo 15:50 – 16:40 Chairman: Prof. Manfred PAKULL, Observatoire de Strasbourg

“European Southern Observatory: results and prospects” Prof. Catherine CESARSKY European Southern Observatory (ESO)

16:40 – 17:00 Coffee break 17:00 – 17:50 Chairman: Prof. Jean-Louis BOUGERET, Observatoire de Paris

“Exo-Solar-Planets: Present and Future” Prof. Norio KAIFU National Astronomical Observatory, Japan 17:50 – 18:00 Closing address

Jean-Marie HAMEURY, Yoichi NAKATANI

4

5

SEMINARS ABSTRACTS

6

EXPLORING THE NEW FRONTIER: HUMAN SPACE FLIGHT

Prof. Chiaki MUKAI Japan Aerospace Exploration Agency (JAXA) 7-44-1 Jindaiji Higashi-machi, Chofu-shi, Tokyo 182-8522 - Japan mukai.chiaki@jaxa.jp

Because of the tremendous advances we have made in science and technology, space has become an extension of our otherwise earth-bound living and working environment. Unique characteristics of the space environment include microgravity, high vacuum, abundant solar energy, a vast orbital field of view, cosmic radiation, and a ready site for laboratory work and science platform deployments. The space environment can be utilized for research areas in such fields as life science, biotechnology, space science, earth observation, microgravity science, and space technology. For example, the microgravity environment of space provides us with a laboratory where there is no sedimentation and no buoyancy, no thermal and density-driven convection, no container required for holding fluids, and no hydrostatic pressure gradient. Active use of the microgravity space environment for materials science, fluid physics, and other related research areas is, therefore, quite promising. However, the same physically unique characteristics of the microgravity environment that make space a remarkable laboratory for research and development also pose special challenges for the human body now exposed to conditions like cosmic radiation and a gravity-free environment. Space flight induces such physiological effects as balance disorders, cardiovascular deconditioning, decrease of bone mineralization, muscle disuse atrophy, reduction of immune response, and more. Many of these physiological changes are the result of adaptation to microgravity and the subsequent re-adaptation to earth’s 1-g environment. As we learn how living organisms react and adapt to such an alien environment as that posed by space, space life-science research will also help us to understand the role of gravity in shaping life as we know it. Interestingly, some of the transient physiological changes observed in healthy Astronauts during, and after, flight parallel certain earth-bound diseases and aging manifestations. Space research has already expanded scientific knowledge across a broad scope of disciplines from materials processing to human physiology, from earth resources observations to biotechnical research, and more. Further knowledge gained promises not only to increase dramatically our scientific understandings and capabilities on earth, but also to enable us to live and work on neighboring planetary bodies like the moon and Mars. Discussed will be some of the the past and current understandings gained from our human space-flight experience and the potential benefits to be gained from further research and exploration.

International Space University Parc d'Innovation 1 rue Jean-Dominique Cassini 67400 Illkirch-Graffenstaden - France

7

Born in Tatebayashi, Gunma Prefecture, Japan, Dr. Chiaki Mukai is a remarkably talented and spirited young woman whose commitment to others and fascination with life have motivated her to great achievements as a cardiovascular surgeon, as a university professor, and as a Japanese astronaut. A veteran of two Space Shuttle flights, Dr. Mukai has spent more than 566 hours in space. She is not only the first Japanese woman to fly in space, but she is also the first Japanese astronaut to fly twice in space. In fact, Chiaki Mukai has more space-flight time than any other Japanese astronaut during the 20th century. Her Space Shuttle flights include what was NASA’s second International Microgravity Laboratory flight. During this extended duration orbital mission, Dr. Mukai conducted a vast array of medical experiments focusing on the cardiovascular system, the autonomic nerve system, and bone and muscle metabolism. Particularly historic, her next mission paired Dr. Chiaki Mukai, the first Japanese woman to fly in space, with pioneering astronaut John Glenn, the first American to orbit the earth. Relying upon her medical expertise, Dr. Mukai worked with 77-year-old Senator Glenn to study spaceflight and its relationship to the aging process. Chiaki Mukai was only a child when she decided she wanted to become a doctor so that she might help people. Today, as a board-certified, cardiovascular surgeon, Dr. Mukai counts as among her most gratifying experiences the many opportunities she has had to have a positive and life-changing impact on the patients who have come under her care. As a doctor in Japan, she has worked on the medical staffs of the Keio University Hospital, Shimizu General Hospital, Saiseikai Kanagawa Hospital, and Saiseikai Utsunomiya Hospital. In the United State, she served in the Division of Cardiovascular Physiology at NASA’s Space Biomedical Research Institute. She is currently affiliated with the Baylor College of Medicine’s Department of Surgery and is a visiting professor in the Department of Surgery at Keio University School of Medicine in Tokyo. While awaiting a flight aboard the International Space Station, Dr. Mukai is also working as a visiting professor at the International Space University in Strasbourg, France. She is credited with more than 60 publications. Profoundly dedicated to broadening the scope of space research and utilization, Dr. Mukai is interested in promoting the arts in space and believes that painters, musicians, and writers will find special inspiration when space becomes a part of their living environment. During her last space mission, she involved the international community, including a United States president, in the creation of a traditional Japanese poem designed to celebrate the possibilities of spaceflight. In addition to being a world expert on the physiology of spaceflight, Dr. Mukai is an avid outdoors woman who excels at Alpine competitive skiing and scuba diving. She also enjoys tennis, photography, golf – and even bass fishing! Furthermore, her pleasure in the arts extends to a special interest in, and appreciation for, American literature. Dr. Chiaki Mukai has received many prestigious awards too numerous to be detailed here. However, a couple of honors that might be mentioned include a Special Citation from the Prime Minister of Japan and Special Recognition by the United States Congress.

Prof. Chiaki MUKAI

8

FUNDAMENTAL PHYSICS AND THE COSMIC MICROWAVE BACKGROUND (CMB) OBSERVATIONS Prof. Jean-Loup PUGET Institut d'astrophysique spatiale Bât. 121 - Université Paris-Sud F-91405 Orsay - France jean-loup.puget@ias.u-psud.fr Observations of the Cosmic microwave background has confirmed that they can bring unique informations about the global structure of the universe (geometry, relative contributions to its dynamics of components with different equations of state...) These observations also have the capability of testing models of the early universe at the time of generation of all the structures we see now. These models depends on physics beyond the standard model of particle physics which is, in some cases, impossible to test with accelerators. The Planck project of the European Space Agency will be the third generation satellite impoving by a factor of 30 the sensitivity of the WMAP NASA project flying today. The indirect detection of the gravity waves generated in the early universe through the polarization of the cosmic microwave background has been identified as a very high priority project by several agencies and will probably the next step.

9

Curriculum Vitae 1965-1969 Student of Ecole Normale Supérieure de Cachan 1970 - 1972 ESRO fellow at the University of Maryland and at Goddard Space Flight Center (NASA) 1973 Tenured research position at CNRS 1973 Ph D directed by Evry Schatzman ( Paris University) 1974 -1975 Post doctoral fellowship from NSF at Goddard Space Flight Center (NASA) 1978 - 1982 Deputy director of Institut d'Astrophysique de PARIS 1979 Stay at Goddard Space Flight Center, studies for the COBE science team 1982 -1983 Visiting Scientist at the Space Science Department ( Berkeley University), Cal Space fellowship 1982-1989 Physics department (radioastronomy) of Ecole Normale Superieure From 1989 Institut d'Astrophysique Spatiale - Orsay Deputy Director from 1990 1998- Director, Institut d’Astrophysique Spatiale Publications and other activities related to scientific research More than 200 scientific publications Mission scientist for the Infrared Space Observatory of the European Space Agency Principal investigator for Planck High Frequency Instrument Member or Chairman of a number of national and international science committees over the past 30 years (AWG and SSAC of ESA, Science Program Committee of CNES, Scientific Advisory committee of IRAM, …) at present Chairman of the Physical Sciences panel of the European Space Science committee of the ESF Chairman of the Scientific and Technical committee of the European Southern Observatory Distinctions - Médaille d'argent du CNRS 1988 - prix Ricard de la Société Française de Physique 1989 - Membre de l' Academia Europea, 1992 - Kingsley Distinguished visitor, Caltech 1997 - Miller professor University of Berkeley, 1998 - Membre de l'Académie des Sciences, Institut de France, 2002

Prof. Jean-Loup PUGET

10

PROBING THE ERA OF GALAXY FORMATION Prof. Sadanori OKAMURA Department of Astronomy, School of Science University of Tokyo 7-3-1 Hongo, Bunkyo-ku Tokyo, 113-0033 - Japan okamura@astron.s.u-tokyo.ac.jp 1. Big Bang Theory We begin with a brief introduction of the big bang theory, in which the universe was created at some 140 billion years ago as a tiny point of extremely high temperature and density. Recombination and re-ionization are important epochs in the history of the universe. 2. Redshift as a Measure of Cosmic Time Due to the expansion of the universe, the wavelength of light coming from distant galaxies is shifted toward longer (redder) side. The redshift parameter, z, is defined by the amount of the wavelength shift (∆λ) divided by the rest-frame wavelength of the light (λ0) as z=∆λ/λ0. The wavelength of light coming from a galaxy located at the distance of z is observed on the earth expanded by a factor of (1+z). The reshift, z, is a measure of cosmic time as well as that of the distance, increasing from the present (z=0) toward the past. Recombination epoch is at around z=1100. 3. Re-ionization Epoch: the End of Dark Age of the Universe At the recombination, about 370 thousand years after the big bang, when free electrons were captured by protons to form neutral atomic hydrogens, interaction between matter and photons terminated, and tiny fluctuations of matter density started to grow by the gravitational instability. Some time after the recombination, astronomical objects were born in the universe. Such first generation objects, probably galaxies and quasars, emitted strong ultraviolet radiation, which eventually re-ionized the intergalactic space. It is shown recently that first objects were born at around z=17 and that the re-ionization was completed at about z=7-6. 4. How were Galaxies and Large Scale Structures Born We show the result of a computer simulation which illustrates the evolution of density fluctuations. 5. Galaxies at High Redshifts We introduce two major classes of galaxies found at high redshifts (z>3), Lyman break galaxies and Lyman alpha emitters, together with the methods to identify them among numerous foreground galaxies. Impacts of the Hubble Deep Field on the study of high redshift galaxies are briefly mentioned. 6. Study of High Redshift Galaxies with Subaru Telescope Subaru telescope has a unique capability, among other 8-m class telescopes, to take the image of a very wide field of view using the prime focus camera, Suprime-Cam. Suprime-Cam is very powerful in the survey for high redshift galaxies. We now have large samples of Lyman break galaxies at z=4-5 and Lyman alpha emitters at z=5 and 6, far larger than any previous sample. We will discuss the evolution of luminosity function, number density as a function of luminosity, of Lyman break galaxies over the range z=0-5. We also show the primeval large scale structure delineated by Lyman alpha emitters at z=5 and 6.

11

Education 1966 Shimonoseki-Nishi senior high school 1970 University of Tokyo, B.Sc.(Astronomy) 1973 Graduate School, University of Tokyo, M.Sc. (Astronomy) 1977 Graduate School, University of Tokyo, D.Sc. (Astronomy) Positions Held 1976-1977 Fellow of Japan Society for the Promotion of Science for Japanese Junior Scientists 1978-1986 Research Associate, Kiso Observatory of the Tokyo Astro-nomical Observatory, University of Tokyo 1981-1982 Guest Research Fellow (British Council Fellow) at the Royal Observatory, Edinburgh 1986-1988 Associate Professor, Kiso Observatory of the Tokyo Astro-nomical Observatory, University of Tokyo 1988-1991 Associate Professor, Kiso Observatory of the Institute of Astronomy, University of Tokyo 1991-present Professor, Department of Astronomy, University of Tokyo 2000- Member of Senate, University of Tokyo 2003- Dean, School of Science, University of Tokyo Professonal Activities 1991-2004: Member of Committee for Astronomy, Science Council of Japan 1997-1999: Vice President, Commission 28 (Galaxies) of the International Astronomical Union 1997-1999: Vice President of the Astronomical Society of Japan 2000-2002: President, Commission 28 (Galaxies) of the International Astronomical Union 2003- : Vice President, Division VIII (Galaxies and the Universe) of the International Astronomical Union Major Scientic Interests Structure and Evolution of Galaxies, Observational Cosmology, Astronomical Image Data Processing Awards and Honours 1991: Toray Science Foundation Award 2001: Daiwa Adrian Prize

Prof. Sadanori OKAMURA

12

ESO: RESULTS AND PROSPECTS Prof. Catherine CESARSKY Director General European Southern Observatory Karl-Schwarzschild-Sts.2 85748 Garching bei Munchen - Germany ccesarsk@eso.org ESO, the European Southern Observatory, was created in 1962 by European states with the mission to establish and operate an astronomical observatory in the southern hemisphere, equipped with powerful instruments, with the aim of furthering and organising collaboration in astronomy. ESO has developed two observatories in Chile, La Silla since 1962 and Paranal since1991, and is now constructing a third observatory, ALMA, in collaboration with European, North American and Japanese laboratories and observatories. The Paranal Observatory, which was inaugurated five years ago, is the home of the Very Large Telescope (VLT), with four 8m telescopes and interferometric equipment. I will outline status and recent results from our observatories, as well as our future plans. Main Scientific Results of Catherine Césarsky Theoretical work on the propagation of galactic cosmic rays and their resonant interactions with hydromagnetic waves. Proponent of the energy dependent leaky-box model for galactic propagation; connexion with interstellar turbulence and with the heating of the interstellar medium. Studies and observations of radio recombination lines from the diffuse interstellar medium; the role of cold regions. Determination of the column of interstellar matter to the galactic center through studies of X-ray absorptionInterpretation of results on cosmic ray composition: implications for the origin and the propagation of theseparticles Diffuse gamma ray emission: a new measure of the density of the interstellar gas and of the spectrum of lowenergy cosmic ray electrons. Penetration of cosmic rays in molecular clouds Parker instability: Demonstration that curved equilibria of the cosmic ray, magnetic field and interstellar gas system, linked by flux conservation to unstable horizontal equilibria, are also unstable. Establishment of a stability criterion applicable to all type of horizontal equilibria. Particle acceleration in astrophysical shocks. In particular, establishment of an upper limit for the energy that cosmic rays can gain from the interaction with a supernova shock. Proponent of stellar winds of WR stars as accelerators of cosmic rays in the 1015 GeV range. Reacceleration of cosmic rays in the interstellar medium. The problem of the highest energy cosmic rays; role of galaxy collisions. Coordination of the ISOCAM Central Programme: infrared emission from the diffuse interstellar medium, dust formation in supernovae, infrared emission from high energy sources, star formation in molecular clouds and in galaxies, etc. Principal Investigator of the ITGES collaboration, which conducted deep surveys with ISOCAM. These deep surveys revealed a population of Luminous Infrared Galaxies with median redshift ~ 0.8, which are responsible for the bulk of the energy in the Cosmic Infrared Background. Follow-up studies of these objects with various telescopes, including VLT and HST are on going. Space experiments of Catherine Césarsky Co-Investigator of COSPIN on ULYSSES; GOLF on SOHO; EPIC on XMM; CIRS on CASSINI; Scientific associate of ISGRI, on INTEGRAL; Principal Investigator of ISOCAM on ISO; Scientific associate of HFI on PLANCK

13

Born in Ambazac, (Haute Vienne), France Education Universidad de Buenos Aires, Facultad de Ciencias Exactas y Naturales, Licenciada en Ciencias Fisicas 1959 - 1965 Harvard University, Cambridge, Mass. PhD in Astronomy 1966 - 1971 Professional Activities Instituto Argentino de Radioastronomia, Research Fellow 1965 – 1966 California Institute of Technology, Astronomy Department, Research Fellow 1971 – 1974 Staff member of the Service d’Astrophysique (Sap), Direction des Sciences de la Matière (DSM), CEA Saclay 1974 – 1978 Head of the theoretical group of the Sap 1978 – 1985 Head of the SAp 1985 - 1993 Director of DSM 1994 – 1999 Director General of ESO 1999 - Publications Author of more than 250 scientific papers Some other activities related to scientific research Member of the Astronomy Working Group at the European Space Agency 1977 – 1980 Chair of the Astronomy and Astrophysics Division of the European Physical Society 1980 – 1983 Editor in Chief of the Journal Astronomy and Astrophysics 1982 – 1985 President of IAU Commission no 48: High Energy Astrophysics 1985 – 1988 Chair of the Observing Programme Committee of the European Southern Observatory 1992 – 1993 Vice Chair of the ESO Council 1993 – 1994 Member of the Conseil Supérieur de la Recherche et de la Technologie, French Ministry of Research 1994 –1996 President of the French Society of Professional Astronomers 1994 – 1996 Vice President of the European Astronomical Society 1993 – 1997 Vice President of the International Astronomical Union 1997 – 2003 Member of the board of the European Research Advisory Board 2001 – 2004 Honorary Member of the American Astronomical Society 2002- President elect of the Astronomical Union 2003- Member of the European Research Advisory Board 2004- She also participated, in 1994, to the Report on the main objectives of research in France for the French Ministry of Research. In the framework of the "Consultation Nationale" conducted by the Minister of Research François Fillon, she chaired the Bordeaux colloquium: Recherche fondamentale: conforter les atouts de la France. C. Cesarsky is or has been a member of the Visiting Committees of Harvard College Observatory, Space Telescope Science Institute, European Southern Observatory. She also participates or has participated or chaired the Haut Comité de l’Observatoire de Paris, the Fachbeirat of the Max Planck Institute für Kernphysik (Heidelberg), as well as those of the Max Planck Institute für Astrophysik (Garching) and the Max Planck Insitute für Extraterrestrische Physik (Garching), or of ESRON (Netherlands). She is a member of the Academia Europaea and of the International Academy of Astronautics. She is a Foreign Associate of the National Academy of Sciences of the United States of America. Awards COSPAR Space Science Award 1998 Distinctions Chevalier de l’Ordre National du Mérite (1989) Chevalier de la Légion d’Honneur (1994) Officier de l’Ordre National du Mérite (1999) Officier de la Légion d’ Honneur (2004)

Prof. Catherine CESARSKY

14

EXO-SOLAR-PLANETS: PRESENT AND FUTURE Prof. Norio KAIFU Director General National Astronomical Observatory National Institutes of Natural Sciences Mitaka, Tokyo, 181-8588 - Japan kaifu@nao.ac.jp

Is the Earth only life-bearing planet in the universe, or just one among huge number of similar planets circulating around huge number of stars? The answer to this basic and long-term question is not easy to obtain because of the lack of scientific method to confirm the existence of exo-solar planets. Planets are so tiny and dim to observe beyond the tenth of light years distance even trough the 20th century. On the other hand the star formation process in cold and dusty interstellar clouds has been extensively investigated by means of mm-wave and infrared observations in the last quarter of the century. Combining with theoretical works on the origin of our Solar System with the observations astronomers come to the provisional but reliable conclusion that the formation of planetary system should be universal phenomena which immediately follows the formation of central star from dark clouds. The dark clouds were revealed to consist of very small grain particles of silicate, carbon and ice as well as gas of hydrogen molecules with rich species of organic molecules. Therefore the formation of Earth-like planets with ocean containing raw materials of life on the rock surface may also be natural process in the universe.

After the decades of tremendous efforts to detect exo-solar planets and a pile of unconfirmed

detection reports a breakthrough was made in the end of 20th century. A Swiss astronomer M. Mayor and his group reported the first reliable evidence of exo-solar planet in 1995. His observations show a half-Jupiter mass planet is orbiting around a star 51 Pegasus with period of only 4.23 day. It was not a direct detection of light from the planet, but was an indirect detection by Doppler method which precisely measured the periodic velocity change of the central star due to the orbiting motion of the planet around it. This detection was immediately examined and confirmed by various authors including a large number of similar detections towards nearby Sun-like stars. Now we count nearly 140 planets orbiting around stars other than the Sun, therefore based on the statistics the existence of a huge number of planets in the universe has been proved. Naturally the current target of astronomers is to detect the light of those exo-solar planets directly to learn about the physical and chemical characters of their atmosphere, although the objects are limited to Jupiter-like giant gas planets. Also the formation process of planetary system should be directly observed and examined by high spatial resolution observations. Such observations are already been under way by using the existing large optical-IR telescopes. Also new powerful telescopes like ALMA will extend the exploration of exo-solar planetary systems.

Detection of the Earth-like small planets and indication of existence of life on them requires two

orders of magnitude higher sensitivity compared with the current limit of observations, however, such target is so exciting and now been extensively discussed by world-wide astronomers. I summarize in this talk the current status of observations of exo-solar planets and what we have learned so far, the resent efforts of direct observations by the 8.2m Subaru telescope on Mauna Kea, and future prospects by coming or possible new generation telescopes.

15

Curriculum Vitae Since 2000 Director General, National Astronomical Observatory (NAOJ) 1997 - 2000 Director of the Subaru Telescope, NAOJ 1994 - 2000 Director of Subaru Project 1992 - 1996 Vice Director of NAOJ 1991 - 1994 Chair of the Subaru Project Office, NAOJ 1988 - 1991 Director of the Nobeyama Radio Observatory, NAOJ 1988 Professor of NAOJ 1979 Associate Professor of NAOJ 1972 –1974 Visiting Researcher of NRAO, USA 1969 Assistant Professor of the University of Tokyo (Department of Astronomy) Education 1966 - 1969 Graduate Course, Department of Astronomy, University of Tokyo 1964 - 1966 Under Graduate Course, Department of Fundamental Science, University of Tokyo 1962 - 1964 General Education, University of Tokyo Ph. D. 1972 University of Tokyo, “Structure and Activity of the Galactic Center” Publications 96 papers in refereed journals (1969-2001) Ed. 5 Books and Proceedings (in English, 1889-1996) 20 books for general and young generation readers (in Japanese, 1972-1999) Honors 1997 Japan Academy Award (“Study of Interstellar Matter”) 1987 Nishina Science Award (“Study and Development of Millimeter Astronomy”) Others Vice President of International Astronomical Union (IAU): 1997-2003 Associate of the Royal Astronomical Society, U.K.

Prof. Norio KAIFU

16

17

POSTERS ABSTRACTS

18

HETE-2 observation of gamma-ray bursts: fast localizations and broad-band spec-troscopy HETE-2 is a small satellite dedicated to the study of gamma-ray bursts, which has been launched in October 2000. Since then HETE-2 has detected over 200 GRBs and several hundred bursts from soft gamma repeaters and X-ray bursters. HETE-2 is the result of a close collaboration between the USA, Japan and France. This collaboration started with the design and the construction of the instruments and continues today with the opera-tion of the satellite, the management of the ground segment, and the scientific analysis of the observations.

We present here two remarkable results obtained with HETE-2: The observation of an early afterglow phase in the minutes fol-lowing GRB 021004 and GRB 021211, and the identification of a population of faint, soft GRBs which could constitute the bulk of the GRB population

Jean-Luc Atteia LA2T, Observatoire Midi-Pyrenees 14 Av. E. Belin 31400 Toulouse Cedex atteia@ast.obs-mip.fr

GRAPE (GRAvity PipE) - N-body simulations on your desk: a JSPS - CNRS col-laboration We present the long term collaboration between the Observatoire de Marseille and the University of Tokyo on the GRAPE project. This has enabled the Marseille group to make competitive simulations of a variety of extragalactic problems, the principal ones baring on the dynamical evolution of isolated disc galaxies, and of compact groups.

Albert Bosma Observatoire de Marseille 2 Pl. Le Verrier 13248 Marseille Cedex 04 bosma@oamp.fr

The radio waves and thermal electrostatic noise spectroscopy (Sorbet) experiment on the BepiColombo/MMO/PWI and the importance of radio HF measurements at Mercury M. Moncuquet (1), H. Matsumoto (2), J.-L. Bougeret (1), L. Blomberg (3), K. Issautier (1), Y. Kasaba (4), H. Kojima (2), M. Maksimovic (1), N. Meyer-Vernet (1), P. Zarka (1), and the PWI team. (1)LESIA, Observatoire de Paris, France; (2) RISH, Kyoto University, Japan; (3)KTH, Alfvèn laboratory, Sweden; (4) ISAS/JAXA, Sagamihara, Japan

SORBET (Spectroscopie des Ondes Radio & du Bruit Electrostatique Thermique) is a radio HF spectrometer designed for the radio and Plasma Waves Instrument (PWI) onboard BepiColombo/Mercury Magnetospheric Orbiter (MMO), which performs remote and in-situ measurements of waves (electromagnetic and electrostatic). Technically, SORBET includes a plasma wave spectrometer, with two E-field inputs from the two perpendicular electric antennas and one B-field input from a search coil, in the range 2.5 kHz - 640 kHz. This frequency band includes the local gyrofrequency and plasma frequency expected on most part of the MMO orbits. SORBET also includes a higher frequency radio receiver for remote sensing in the range 500kHz-10.2MHz.Owing to its capabilities, SORBET will be able to address the following scientific objectives: *High resolution mapping (~30 km) of electron density and temperature in the solar wind and in the Hermean magnetosphere and exo-ionosphere, via the technique of Quasi-Thermal Noise (QTN) spectroscopy. The quasi-thermal noise is due to the ther-mal motions of the particles, which produce electrostatic fluctuations. This noise is detected by any sensitive receiver at the ports of an electric antenna immersed in a plasma and can be used to measure in-situ the plasma density, temperature and bulk veloc-ity. The basic reason is that this noise can be formally calculated as a function of both the particle velocity distributions and the antenna geometry. So, conversely, the spectroscopy of this noise reveals the local plasma properties. This method is routinely used on Ulysses and Wind spacecraft in the solar wind or in planetary magnetospheres/ionospheres (Ulysses at Jupiter, Cassini at Venus, Earth and now at Saturn). This method has the advantage of being relatively immune to spacecraft potential and photo-electrons perturbations. These QTN measurements will be determinant for the dynamic modeling of the magnetosphereand will provide a fundamental input for the chemistry of cold ionized species (Na, K, O ...) in Mercury?s environment. *Detection and study of Hermean radio emissions, including possible cyclotron emissions (up to ~10-20 kHz) from mildly ener-getic electrons in most highly magnetized (polar?) regions, and possible synchrotron radiation (up to a few MHz?) frommore energetic electrons. Indeed no stable radiation belts are expected, due to the weakness of Mercury's magnetic field, but intense bursts of energetic particles were measured by Mariner 10 in the magnetotail. Short storm-like events with ~1 minuteduration (observed by Mariner 10), as well as Sodium aurorae, suggest an auroral activity at Mercury. Associated cyclotron emissions, due to keV electrons, would be produced near the gyrofrequency and below the plasma frequency in the surrounding solar wind, and thus be trapped inside the magnetospheric cavity. They can be detected only during relatively short crossings of the magnetosphere by MMO. *Monitoring of solar radio emissions up to ~10 MHz (type II and type III radio bursts, indicative of interplanetary transient shocks, CMEs, and energetic particle streams), in order to create a solar activity index from the view point of Mercury, allowing to correlate it with the Hermean magnetospheric response (i.e. "Space weather" at Mercury).

Jean –Louis Bougeret LESIA Observatoire de Paris 5 Place J. Janssen 92195 Meudon jean-louis.bougeret@obspm.fr

19

SUBARU observations of cooling neutron stars and ultraluminous X-ray sources Manfred W. Pakull, Christian Motch & Fabien Grisé (Observatoire Astronomique de Strasbourg, France), Takeshi Go Tsuru (Departments of Physics, Kyoto University, Ja-pan) and Kaz Sekiguchi (Subaru Telescope, NAOJ, Hilo, USA) The outcome of massive stellar evolution are neutron stars and black holes which are principally detected in the X-ray range. However, crucial information on these objects can be obtained by optical studies with the current generation of 8m class telescopes.

Here, we report on recent observations collected with the Japanese SUBARU telescope on top of Mauna Kea, Hawaii. They con-cern on the one hand the physics of cooling neutron stars in our Galaxy, surface emission properties and constraints on the equa-tion of state in star interior, and on the other hand the nature of very bright ('ultraluminous') variable X-ray sources (ULX) in nearby galaxies that have been proposed to contain 'Intermediate Mass Black Holes' in the mass range beween the stellar and the AGN-type variety. Among the interesting results of our study are the high spatial velocity of an X-ray bright isolated neutron star from which age and birth place could be derived and the discovery of emission lines in the optical counterparts of ULX which

Christian Motch Observatoire de Strasbourg 11 rue de l'Universite 67000 Strasbourg motch@astro.u-strasbg.fr

The International Virtual Observatory Alliance F. Genova (CDS, Strasbourg Observatory) and M. Ohishi (NAOJ) Astronomy has been at the forefront for data conservation and distribution, and also for information networking, thanks to early definition of de facto disciplinary standards, availability of observatory archives, and collaboration between archive providers, data centres and journals. The current astronomy information network already allows scien-

tists to surf from observations to results published in journals, and includes value-added information services. CDS in Strasbourg and NAOJ/ADAC have been collaborating for many years in this domain, in particular for preparation and distribution of cata-logue data. In recent years, the Virtual Observatory vision has developed very rapidly, with the aim of going further in the inte-gration of heterogeneous, distributed information, tools and computational resources. To date, there are fifteen VO projects worldwide, who coordinate their efforts through the International Virtual Observatory Alliance (IVOA). The aims of IVOA, and the current developments of the French VO (OV France) and the Japanese VO will be explained. IVOA: http://www.ivoa.net; OV France: http://www.france-vo.org/; Japanese VO: http://jvo.nao.ac.jp/; CDS: http://cdsweb.u-strasbg.fr/; NAOJ: http://www.nao.ac.jp/

Francoise Genova Observatoire de Strasbourg 11 rue de l'Universite 67000 Strasbourg genova@astro.u-strasbg.fr

Old stars in the Galaxy: a tool to understand the formation of the elements in the Universe Very old stars of our galaxy contain mostly primordial matter (mainly Hydrogen and Helium). but they also contain some traces of heavier elements (like Carbon, Iron, Ura-nium). The interest of these very old stars is that they have been polluted by few gen-erations of supernovae, there are a very powerful tool to understand how the elements are synthetized in stars. Our collaboration is focussed on the synthesis of the most heavy elements (heavier than Iron) which are built during the late stages of evolution of the stars through a process called "r-process".

Patrick Francois Observatoire de Paris 61 Av. de l'Observatoire 75014 Paris Patrick.Francois@obspm.fr

Gyro-resonant surfing acceleration of ions in front of quasiparallel shocks and in-jection problem. Kuramitsu Y. and Krasnoselskikh V. We discuss a acceleration mechanism of charged particles around magnetohydrody-namic (MHD) structures, uch as shocks and short-large amplitude magnetic structures (SLAMS). In the presence of electromagnetic waves and a electrostatic electric field, particles are

accelerated efficiently in the perpendicular direction owing to the combination of two effects, one is the trapping of particles by the wave and another is the dragging by the electrostatic field to keep the resonance condition. This allows particles to propagate downstream even when they have smaller kinetic energy than the potential. We show fundamental properties of this mechanism that is referred to as gyro-resonant surfing.

Vladimir Krasnoselskikh LPCE 3a Av. de la recherche scientifique 45071 Orleans Cedex 2 vkrasnos@cnrs-orleans.fr

Abstract to be announced Hideki Ozawa LAOG Observatoire de Grenoble 414 rue de la Piscine BP 53 38041 Grenoble Cedex 9 hideki@obs.ujf-grenoble.fr

20

Statistical Study of Dust Emission in Molecular Clouds Y. Fukui(1), A. Kawamura(1), A. Mizuno(1), N. Mizuno(1), T. Onishi(1), H. Sasago (1), H. Shibai(1), K. Dobashi (2), J.P. Bernard(3), C. Joblin (3), C. Meny (3), R. Paladini (3), D. Paradis(3), I Ristorcelli (3), A. Abergel(4), F. Boulanger(4), G. Lagache(4), N. Bot (5), L. Cambresy(5), A. Coulais(6) (1) Nagoya University, Nagoya, Japan; (2) Tokyo Gakugei University, Tokyo, Japan; (3) CESR, Toulouse, France; (4) IAS, Orsay, France; (5) Obs. Strasbourg, Strasbourg, France; (6) LERMA, Paris, France

Dust grains of the Inter Stellar Medium (ISM) play a major role in the chemistry and the structuration of the ISM. In particular, the most abundant molecules in the gas phase of the ISM, like molecular Hydrogen (H2), are formed at the surface of grains. The dust also partially controls the thermal behavior of the gas through photo-electric effect and cooling. This poster will present the goals of an ongoing collaboration effort between France and Japan to perform a statistical study of the dust properties in the most nearby molecular clouds in our galaxy. This study will make use of the large molecular survey undertaken by the Nagoya group using the NANTEN telescope in Chile, will use the IR data currently being obtained by the American satellite Spitzer and the large scale extinction maps generated by the Strasbourg and Tokyo research teams.

Deborah Paradis CESR 9 Av. du Colonel Roche BP 4346 31028 Toulouse Cedex Deborah.Paradis@cesr.fr

The nutation of the Earth: state of the art of theories and observations The nutation of the Earth, discovered by Bradley in 1749, stands for the periodic oscilla-tions of the axis of rotation as well as the axis of figure of the Earth with respect to iner-tial space, due in large part to the effects of the Sun, the Moon and also the planets on the Earth’s flattening. Thanks to the spectacular improvements of modern observational techniques as VLBI (Very Long Baseline Interferometry) it is now possible to determine the motion above with an exceptional precision, at the order of a few 10 �as

(microsarcseconds of arc). At the same time, a lot of efforts have been made in the last decade to ameliorate the theoretical mod-els of nutation in order to match up to the quality of observations. This lead to a conventional model of nutation MHB2000 adopted by the IAU. We describe in detail how this model is built and the numerous effects it includes.

Jean Souchay Observatoire de Paris 61 Av. de l'Observatoire 75014 Paris Jean.Souchay@obspm.fr

Abstract to be announced Laurent Wiesenfeld LAOG Observatoire de Grenoble 414 rue de la Piscine BP 53 38041 Grenoble Cedex 9 Laurent.Wiesenfeld@ obs.ujf-grenoble.fr

21

“Presentation of JSPS Alumni Association” "The Association des anciens boursiers francophones de la JSPS" has been founded in 2004. This main objectives of this association are: 1. to advise and help the french-speaking students and young researchers who want to

join a japanese laboratory for their research and also the other way round: to help Japanese students and young researchers to find a host laboratory in french-speaking countries,

2. to assist the students and young researchers for the preparation of their stay in Japan or in France and in french-speaking countries,

3. to diffuse largely in France and in french-speaking countries information about the fellowships, in particular JSPS fellowships,

4. to be an efficient partner for the French JSPS Office. Association board:

Honorary President: Jean-Marie Lehn, ULP, Strasbourg President: Marie-Claire Lett, ULP, Strasbourg Secretary: Jacques Streith, UHA, Mulhouse Vice-Presidents: Alain Milon, UPS, Toulouse Eric Oswald, INRA, Toulouse Treasurer : Robert Pansu, ENS-Cachan Deputy Treasurer : Reiko Oda, CNRS, Bordeaux

Contact address: Prof. Marie-Claire LETT Université Louis Pasteur President of JSPS Alumni Association Institut de Botanique, 28, rue Goethe F-67000 Strasbourg - France http://assoc-jsps.u-strasbg.fr/ lett@gem.u-strasbg.fr

22

NOTE

23

NOTE

24

NOTE

1

2

Société Japonaise pour la Promotion de la Science JSPS Strasbourg Office

Maison universitaire France-Japon

42a, avenue de la Forêt-noire 67000 Strasbourg, France

Tél : +33(0)3 90 24 20 17 Fax : +33(0)3 90 24 20 14

jsps@japon.u-strasbg.fr http://jsps.u-strasbg.fr/