High-Energy Astrophyiscs and Fundamental Physis missions in Japan Tadayuki Takahashi ISAS/JAXA 1. ISAS/JAXA 2. X-ray Satellites to study Cosmic Rays 3. Astroparticle/Fundamental Physics Missions Space Science Program in ISAS With variety of vehicles Scientific satellites Sounding Rocket - Small/Medium/Large - 150mø handling area Scientific available for balloon launch 30mW×83mL×35mH hanger Balloon with 30mW×28.5mH door 2 JAXA’s current activities of Space Science Suzaku Akari Hinode X-ray Astronomy Infrared Astronomy Solar Physics Lunar Science Space VLBI Geo-magnetosphere Primitive body exploration GEOTAIL Akebono Hayabusa Planetary Atmosphere Akatsuki JAXA’s future activities of Space Science Near Future pre-Phase A ASTRO-H “Project” SPRINT-A (X-ray Astronomy) SCOPE 2014 (Finished MDR) Hayabusa-2 Many more missions are in Working-Group activities (including CR experiments) 2014 “preProject” SPICA (IR) ERG SELENE-2 Bepi Colombo (MMO) (Mercury Exploration) Phase A/Risk Mittigation Phase Phase A 4 50 Years after Sco X-1 Discovery (1962) in X-rays Only possible by a rocket (Giacconi+62) N E S W N M. Oda (right) and his modulation collimator X-ray position determination with mod. collimators (Gursky+66) Optical ID, first in Japan, then at Palomar; 5 (Sandage+66) 50 Years after Sco X-1 Discovery (1962) in X-rays Only possible by a rocket (Giacconi+62) N E S W N M. Oda (right) and his modulation collimator “Inspection of the two plates, taken X-ray position determination with mod. with the Tokyo Obser-vatory’s 74-inch collimators (Gursky+66) reflector, revealed an intense ultraviolet Optical ID, first in Japan, then at Palomar; object within 1’ of one of the two X-ray 5 (Sandage+66) source positions...” X-ray Universe = Hot Universe X-ray observations using space telescopes revealed that the Universe is full of high-temperature phenomena reaching 10 to 100 million degrees, which nobody had imagined before the advent of the X-ray astronomy. 80-90 % of matter in the universe can be accesible to us, is only seen via X-rays (Fukugita & Peebles 2004, Read & Trentham 2005) Science topics of the next genation of X-ray observatory NGC5044 6 X-ray Universe = Hot Universe X-ray observations using space telescopes revealed that the Universe is full of high-temperature phenomena reaching 10 to 100 million degrees, which nobody had imagined before the advent of the X-ray astronomy. 80-90 % of matter in the universe can be accesible to us, is only seen via X-rays (Fukugita & Peebles 2004, Read & Trentham 2005) Science topics of the next genation of X-ray observatory •Gravitational deformation of space at extreme proximity of black holes NGC5044 • Super massive black holes and their role in the galaxy evolution •Dynamical evolution of galaxy clusters •Particle acceleration in the Universe (SNRs, SMBH, galaxy clusters) 6 7 Signature from particle accelerators - Super Nova Remnants • X-ray observation is very sensitive to the existence of the distribution of high energy electrons (particle accelerators) ASCA (Koyama et al. 1995) • X-ray Synchrotron 2 hν synch = 5.3 E100TeVB10µG [keV] 100 TeV energy electrons IC sync. € π0 thermal dF/DE 2 proton E electron X-ray gamma-ray Energy 2012 Milano 8 Signature from particle accelerators - Super Nova Remnants • X-ray observation is very sensitive to the existence of the distribution of high energy electrons (particle accelerators) Similar morphology ASCA (Koyama et al. 1995) X-ray (color: Suzaku) and TeV (contour:H.E.S.S.) Cooling time of X-ray emitting electrons RXJ1713.3-7946 is2012 much Milano shorter than radio ones X-ray Study of Emax synchrotron X-rays have cut-off electron distribution Sync. Emission Γ From Power-law electrons Γ-1 2 exp. N(E) E Emax emission emission from an e ν Ecut-off 2 ~ Emax B Sync. Sync. emission ν E2B Cooling time of X-ray emitting electrons is much shorter than radio ones 4. Blazar (From T. Takahashi). Signature from particle accelerators - Jets from SMBH X-ray Emission from Blazar (Super Massive Blackholes) Blazar MW spectra erg/s Simultaneous flare in light curves are often observed in X-ray/TeV gamma-ray (Due to the change of the high energy end of electron ditribution?_ 10 19 Signature from particle accelerators - Merging Clusters The Biggest Event, should release some fraction of 10^63 erg 1E0657-56 at z=0.30 (Bullet cluster) Cosmic Ray Acceleration at the shock? Color: X-ray (collisional gas) Contours: weak lensing Mach number ～ 3.0 Vpreshock ～4700 km/s Vpostshock～1600 km/s 1’=270 kpc (Clowe; Mastropietro & Burkert 08) Studies of the total energy content (including that of non-thermal particles) require observations by 1) A spectrometer capable of measuring the bulk plasma velocities and/or turbulence with the resolution corresponding to the speed of a few × 100 km/s 2) An arc-min imaging system in the hard X-ray band to study Non-thermal hard X-ray emission from relativistic particles ASTRO-H: International X-ray Observatory 1970 1980 1990 2000 2010 2700 X-ray ASTRO-H Astoronomy Started 2000 kg 2014 1700 H2A Suzaku Ginga ASCA 1000 kg M5 M3SII Weight 2.7 t Tenma Height 14 m Hakucho 430kg 420kg 220kg 90kg Together with the development of new rockets 12 ASTRO-H: Instruments CCD 1. High Resolution Spectroscopy by a micro-calorimeter array ASTRO-H is the first mission to carry out high XRT Si/CdTe Compton Camera resolution spectroscopy of extended objects at Fe-K 2. Wide Band /High Sensitivity Observation 0.3 keV - 600 keV : Four Instruments including Hard X-ray Focusing optics SXS+SXT: Micro Calorimeter SXI+SXT: X-ray CCD HXI (two sets)+HXT: Si and CdTe Hybrid SGD(two sets): Micro Calorimeter Si/CdTe Imager Si/CdTe Compton Camera 13 ASTRO-H Micro Calorimeter System (SXS) Thermal(Detec,on(of(X1Rays( Ion-implanted Si thermometer HgTe absorber (~ 8 microns thick) Pixel size: 824 x 824 microns 50 mK (30 x 30 arcsec) Laboratory X-ray • Above 2 keV, SXS spectrum has higher obtained with the sensitivity and SXS Engineering better energy Model resolution compared with grating spectrometers 4 keV 6 keV 8 keV NASA/GSFC 14 ASTRO-H Features --- Wide Band Observation--- •Pt/C depth-graded multilayer Vast Improvements of the sensitivity Hard X-ray telescope + Imager in the energy window from 10 keV to 600 keV •Si/CdTe Compton Camera (upto 0.6 MeV) 15 Power of ASTRO-H : SNR Supernova Remnants SN1006 10-40 keV (100ks) The combination of ASTRO-H's hard X- ray imaging capability and high spectral resolution will provide information to understand crucial aspects of shock acceleration in SNRs such as the maximum energy of the accelerated by A.Bamba particles. Site of Particle Acceleration to map electon distribution with E=Emax SN1006 RXJ1713 by ASTRO-H Suzaku at 40 keV ASTRO-H at 40 keV -39d30m -40d00m 17h16m 17h14m 17h12m by T. Tanaka 2011//06/30 The X-ray Universe 2011, Berlin 16 Power of ASTRO-H : Cluster dynamics: Gas bulk motion •With high-resolution spectroscopy, the velocity of matter can be derived from the energy shift and width of emission lines A2256 A2256 Δv = 1000 km/s SXS 80 ksec x 2 \ SXS spectra of a merging cluster A2256 assuming 1000 km/s difference in the line-of-sight velocity System TTM (Thermal Test Model) test (Aug-Sep, 2012) ASTRO-H in JAXA’s 13 m thermal-vacuum chamber Astro Particle/Fundamental Physics experiments in Japan } In 1990s, Balloon-borne astroparticle physics experiments were conducted by particle physics and/ or cosmic-ray physics community. ◦BESS and BETS BESS talk by A, Yamamoto on Tuesday } As one of JEM-EF experiments on ISS, CALET is now under construction (2014) } In 2000s, several working groups for space-based astroparticle physics have been formed. 19 CALET Mission to ISS/JEM JEM A Detector Dedicated to Electron Observation in 1GeV-20,000GeV CALET Mission to ISS/JEM Calorimeter (CALET/CAL) • Electrons: 1 GeV – 20,000 GeV • Gamma-rays: 10 GeV – 10,000 GeV (Gamma-ray Bursts: > 1 GeV) • Protons and Heavy Ions: several tens of GeV - 1,000 TeV Gamma-ray Burst Monitor (CGBM) Gamma-ray 10 GeV Electron 1 TeV Proton 10 TeV GAPS (General Anti-Particle Spectrometer) Working Group Activity for Future Proposal to JAXA MOO AO uUS-Japan Collaboration to search for still- undiscovered cosmic antideuterons uThe upper stratosphere over the geomagnetic pole using (ultra-) long balloon flights in late 2010’s. uMeasurements of characteristic X-rays & π/p’s produced by the decay process of exotic atoms for a powerful particle identification capability of D’s from p, p, and other backgrounds. uEngineering flight was successfully carried out in Jun/2012 in Japan using a JAXA’s stratospheric balloon. Primary D Launch of the GAPS engineering “Bkgnd” D balloon flight sub-GeV region is “background- (Japan) free” JEM-EUSO (EUSO on JEM) Working Group Activity for Future Proposal to JAXA JEM-EF AO New window of Astronomy: Origin and acceleration of Extreme Energy Cosmic Rays (EECRs, ～1020 eV), Deployable telescope with Large (2.5m) and Wide FoV (60°) (2 tons) Light Weight Fresnel lenses JEM-EUSO will have an annual exposure of over 4 x 104 km2 sr yr, a factor of 10 above Auger JEM (Japanese Experiment Module, Kibou (Hope) Space GW antenna : DECIGO Working Group Activity for Future Proposal to JAXA Small Satellite AO PathFinder mission Single and small satellite in low-earth orbit Laser Local Sensor Payload :~1m3 , Total weight: 350kg Altitude 500km, sun synchronous 30cm Precise length measurement in space 30cm FP interferometer Actuator Stabilized Yb:YAG laser source Thruster Drag-free control for 6DoF of the satellite motion DECIGO (Deci-hertz interferometer Gravitational wave