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Fundamental Physics in Space in Japan

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Fundamental Physics in Space in Japan JAXA’s Long Term Vision for science Fundamental Physics in Space in Japan Tadayuki Takahashi Institute of Space and Astronautical Science (ISAS) Japan Aerospace Exploration Agency (JAXA) Outline • Agency Organization • Brief History of ISAS and Recent Achievements • Fundamental Science in Space Japan’s approach • High Energy Astronomy • JAXA’s Long Term Vision - JAXA 2015 - from Space Particle point of view JAXA Three Japanese organizations were merged as the Japan Aerospace Exploration Agency(JAXA) on October, 2003. Through the merger of ISAS, NAL, and NASDA, JAXA now promotes all space development, from basic research to development and utilization. Academic Research ISAS Graduate School Education NAL Aerospace Technology Rockets/Satellites NASDA following Japanese Policy • Space Science/Exploration • Earth-observation • Space Environment Utilization Space Flight • Launch Vehicles and • Space Technology Operation H-II A • Education Institute of Space and Space Application Astronautical Science Institute of Aviation Space and Program Aerospace Group Technology Universities (Communities) ISAS Feb. 1970 The L-4S rocket launched Mu Series : Solid Rocket Japan's first satellite, OHSUMI. scientific satellites Feb. 1997 The M-V-1 launched the world's first space VLBI satellite, HALCA. Sep. 2005 HAYABUSA arrived asteroid ITOKAWA for the first sample return from asteroid HAYABUSA（隼） PICTURES OF ITOKAWA TAKEN BY HAYABUSA Mother Spacecraft Sampling Mechanism Hopping Rover Target Marker Hakucho (1979) Strategy Step-by-step but challengingly progressive strategy Tenma (1983) Example: X-ray astronomy satellites Small but beautiful Aiming at new results with unique, original mission instruments Ginga (1987) International Collaboration ASCA (1993) ISA Hakucho (1979) Strategy Step-by-step but challengingly progressive strategy Tenma (1983) Example: X-ray astronomy satellites Small but beautiful Aiming at new results with unique, original mission instruments 1,600 Ginga (1987) InternationalASC CollaborationA - International Mission - 1,400 Paper in Refereed Journal (>1400) PhD (>110) 1,200 1,000 ASCA (1993) 800 600 400 200 ISA 0 1994 1995 1996 1997 1998 1999 2000 2001 2002 2003 2004 Particle and Fundamental Physics in Space Japan’s Approach To understand the universe - From the Big Bang to Ourselves - 8 To understand the universe - From the Big Bang to Ourselves - To understand the universe - From the Big Bang to Ourselves - Neutrino Astronomy/Neutrino Mass Super-KAMIOKANDDE To understand the universe - From the Big Bang to Ourselves - Neutrino Astronomy/Neutrino Mass Super-KAMIOKANDDE KAMLAND To understand the universe B-factory - From the Big Bang to Ourselves - CP Violation Neutrino Astronomy/Neutrino Mass Super-KAMIOKANDDE KAMLAND To understand the universe B-factory - From the Big Bang to Ourselves - CP Violation Neutrino Astronomy/Neutrino Mass Super-KAMIOKANDDE TAMA30 Gravitational Wave KAMLAND To understand the universe - From the Big Bang to Ourselves - To understand the universe - From the Big Bang to Ourselves - ATLAS at LHC (E/J/US) To understand the universe - From the Big Bang to Ourselves - ATLAS at LHC (E/J/US) Cangaroo (J/ To understand the universe - From the Big Bang to Ourselves - ATLAS at LHC ALMA (J/US/ (E/J/US) Cangaroo (J/ To understand the universe - From the Big Bang to Ourselves - ATLAS at LHC ALMA (J/US/ (E/J/US) Cangaroo (J/ To understand the universe - From the Big Bang to Ourselves - ATLAS at LHC ALMA (J/US/ (E/J/US) Cangaroo (J/ Telescope To understand the universe - From the Big Bang to Ourselves - SDSS(US/J/ ATLAS at LHC ALMA (J/US/ (E/J/US) Cangaroo (J/ Telescope Subar To understand the universe - From the Big Bang to Ourselves - SDSS(US/J/ ATLAS at LHC ALMA (J/US/ (E/J/US) Cangaroo (J/ Telescope To understand the universe Balloon Experiments - From the Big Bang to Ourselves - •Evaporation of Search for Anti-Particle Primordial Black Holes Primordial Antiparticles •Annihilation of Particle in Cosmic Rays super-symmetric particles (Particle Detectors) BESS(J/US) BH To understand the universe Feb.22/2006 - From the Big Bang to Ourselves - Birth & Evolution of Galaxies (Infrared : Low Temperature, Less Extinction, High Redshift) AKARI (Astro-F) , the second space mission for infrared astronomy in Japan. It aims for an all-sky survey with much better sensitivity, spatial resolution and wider wavelength coverage than IRAS. AKARI (Astro-F) Survey Mission/ 2006 To understand the universe - From the Big Bang to Ourselves - To understand the universe - From the Big Bang to Ourselves - To understand the universe - From the Big Bang to Ourselves - Solar Wind To understand the universe - From the Big Bang to Ourselves - SCOPE Solar Wind (planned) To understand the universe - From the Big Bang to Ourselves - The best way is to be there. SCOPE Solar Wind (planned) To understand the universe - From the Big Bang to Ourselves - The best way is to be there. • Venus Climate Orbiter (2008) And also Bepi-Colombo(2011?) SCOPE Solar Wind (planned) To understand the universe - From the Big Bang to Ourselves - The best way is to be there. • Venus Climate Orbiter (2008) And also Bepi-Colombo(2011?) • Solar Sail Mission to Jupitor (approved as “High Priority Mission”) SCOPE Solar Wind (planned) To understand the universe Optical (Green) vs - From the Big Bang to Ourselves - Radio (Red) High resolution imaging by Space VLBI (relativistic jets) Synchrotron Radio VSOP -> Trace Distibution of High Energy Electrons M87 Jet by Hubble Telescope 360 µ arcsec@5GHz VSOP２ではこの中を VSOP Image （１．６GHｚ、１mas） さらに分解する VSOP2 Angular Resolution 40 micro arcsec (10 times better than VSOP) Ground Network VSOP-2 (selected as the 26’th 15 scientific satellite) VSOPにも参加4 VSOP-2で新規参加 VSOP2 Angular Resolution 40 micro arcsec (10 times better than VSOP) Ground Network VSOP-2 (selected as the 26’th 15 scientific satellite) VSOPにも参加4 VSOP-2で新規参加 To understand the universe - From the Big Bang to Ourselves - Suzaku(朱雀） X-ray/Gamma-ray Best probe to study Extreme Universe. Can be done only in space X-ray emission from close to the event July 10, 2005 horizon provides a powerful probe Broad Iron line interpreted as due to gravitational redshift toward the blackhole (First discovered by ASCA) Power of Suzaku XIS (X-ray CCD) Wide band observation of non- HXD thermal sources Connection between THERMAL and non-THERMAL Cen A Observation Narrow Fe K line 100 PIN Diodes GSO/BGO Absorption due to interstellar gas phoswich surrounding the black counters hole 10 X-ray CCD Camera Intensity of Radiation 1 Hard X-ray Detector preliminary Suzaku Team From the edge of a black hole to the collision of largest celestial objects Study of the structure of the universe: Cluster of galaxies : Largest celestial object (self gravitating energy 10^64 erg, hundreds of galaxies) Cluster merging (optical) Cluster merging (X-ray) T.Takahashi, Heidelberg γ2004 W.S Energy contents of non-thermal emission? A2256 (Fusco-Femiano et al. 2000) Recent Radio/X-ray observation ー> Non-thermal emission from clusters of galaxies Non-Thermal (above 10 keV) Component Non-thermal luminosity kT=7ke (comparable or even larger than Thermal the thermal luminosity Component if p/e ~100.) 2 5 10 20 50 100 keV NeXT (Non-thermal Energy eXploration Telescope) (selected as one of two top priority missions in ISAS) T.Takahashi, Heidelberg γ2004 W.S Energy contents of non-thermal emission? A2256 (Fusco-Femiano et al. 2000) Recent Radio/X-ray observation ー> Non-thermal emission from clusters of galaxies Non-Thermal (above 10 keV) Component Non-thermal luminosity kT=7ke (comparable or even larger than Thermal the thermal luminosity Component if p/e ~100.) 2 5 10 20 50 100 keV The energy we have not yet realized (Non-thermal Energy) NeXT (Non-thermal Energy eXploration Telescope) (selected as one of two top priority missions in ISAS) NeXT Mission • First Hard X-ray Focusing Telescope • Highly sensitive γ-ray detector with capability to measure γ-ray polarization • ΔE=7 eV resolution (TES calorimeter) for soft X-rays NeXT Mission • First Hard X-ray Focusing Telescope • Highly sensitive γ-ray detector with capability to measure γ-ray polarization • ΔE=7 eV resolution (TES calorimeter) for soft X-rays Motion、Turbulence、Shock Wave NeXT Mission • First Hard X-ray Focusing Telescope • Highly sensitive γ-ray detector with capability to measure γ-ray polarization • ΔE=7 eV resolution (TES calorimeter) for soft X-rays Motion、Turbulence、Shock Wave Heating NeXT Mission • First Hard X-ray Focusing Telescope • Highly sensitive γ-ray detector with capability to measure γ-ray polarization • ΔE=7 eV resolution (TES calorimeter) for soft X-rays Motion、Turbulence、Shock Wave Heating Thermal Emission From 0.5 10 NeXT Mission • First Hard X-ray Focusing Telescope • Highly sensitive γ-ray detector with capability to measure γ-ray polarization • ΔE=7 eV resolution (TES calorimeter) for soft X-rays Motion、Turbulence、Shock Wave Heating Acceleration Thermal Emission From 0.5 10 NeXT Mission • First Hard X-ray Focusing Telescope • Highly sensitive γ-ray detector with capability to measure γ-ray polarization • ΔE=7 eV resolution (TES calorimeter) for soft X-rays Motion、Turbulence、Shock Wave Heating Acceleration Thermal Emission From Non-thermal emission From accelerated Particles 0.5 10 80 1Me Strategy of Space Origin of the solarSolar system system Observation Science in Japan HAYABUSA Exploration from Space Infrared HAYABUSA AKARI -2 Technology SPICA X-ray/Gamma-ray Origin & Formation and Technology Structure of Evolution of Moon Exploration the
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