High-Energy Astrophyiscs and Fundamental Physis missions in

Tadayuki Takahashi ISAS/JAXA

1. ISAS/JAXA 2. X-ray 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

X-ray Astronomy

Infrared Astronomy

Lunar Science Space VLBI

Geo- Primitive body exploration Planetary Atmosphere

Akatsuki JAXA’s future activities of Space Science

Near Future pre-Phase A -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 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 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 -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. 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 ASCA 1000 kg M5 M3SII Weight 2.7 t 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 AO PathFinder mission

Single and small satellite in low- orbit Laser Local Sensor Payload :~1m3 , Total weight: 350kg Altitude 500km, 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 Observatory) - Space gravitational-wave antenna (launch ~2027) - Observation band around 0.1 Hz

* Baseline length: 1000 km Arm cavity

1000km Fabry-Perot Interferometers Arm cavity

Laser Mirror * 3 S/C formation flight Photo- detector Drag-free S/C and Drag-free control LiteBIRD Working Group Activity for Future Proposal to JAXA Small Satellite AO

primordial Cosmic Microwave Background gravitational (CMB) polarization Studies of B-mode Polarization and waves Inflation from Cosmic Background Radiation Detection B-mode 10−38 sec 380000 yrs now n Scientific objectives n Stringent tests of cosmic inflation Superconducting ~450kg n Tests of quantum gravity theories Focal plane LEO (500km) n Observations (100mK) (L2 as an n Full-sky CMB polarization survey option) at a degree scale n Detecting primordial gravitational waves imprinted in CMB polarization map δr = 0.001 Conlusions

} The ASTRO-H international X-ray observatory is now under construction for the launch of 2014. ASTRO-H will play an important role for the studies of CR acceleration in the Universe. } CALET (@JEM-EF/ISS) will be launched in 2014. } Science missions in Japan are implemented by the bottom- up process. Several space-based astroparticle physics projects are proposed to form working groups. } ISAS/JAXA is planning to issue AOs of MOO and Medium class missions in near future. We would like to have proposals with high scientific level and with high TRLs (Techinical Readiness Level).

26 What X-ray missions have bought to us Extreme Environments - Particle Accelerator - RX J1713.7-3946 Most filaments (spatially extended) are variable in time!!

Timescale ~ 1 year

− . Decaying B 1 5 ! −0.5 tsync ∼ 1.5 year !mG" #keV $ X-ray spectra: a power law with photon index ~2 B ∼ 1 mG η ∼ 1 Brightening and Decaying −1.5 0.5 −2 ∼ B " Vs Chandra (color) tacc 1 η −1 years !mG" #keV $ !3000 km s " HESS (contours) Uchiyama, T.T et al. (2007) Search for Synchrotron Emission from secondary electrons

F. Aharonian 4. Power of ASTRO-H : Cluster dynamics: Non-thermal emission

HXI

radio synchrotron emission (contours)

A3667 z=0.05 SXS

XMM (color) Finoguenov+10 Markevitch, Akamatsu, and the ASTRO-H Cluster STF 4. Power of ASTRO-H : Cluster dynamics: Non-thermal emission

HXI

radio synchrotron emission (contours)

A3667 z=0.05 SXS

Line broadening due to turbulent gas XMM (color) motion Finoguenov+10 Markevitch, Akamatsu, and the ASTRO-H Cluster STF 4. Power of ASTRO-H : Cluster dynamics: Non-thermal emission

HXI

radio synchrotron emission (contours)

Non-thermal hard X-ray emission from relativistic particles

A3667 z=0.05 SXS

Line broadening due to turbulent gas XMM (color) motion Finoguenov+10 Markevitch, Akamatsu, and the ASTRO-H Cluster STF Selection Process ISAS Advisory Council for Research and Selection and operation of Management Space Science Missions MDR/SRR/SDR AO PDR/CDR Recommendation Evaluation with Committee Steering Committees Members from Space Science Space Engineering Universities

Support to Mission Planning, Front-loading studies, Technology for Future missions.

Working Groups Working Groups Working Groups

Scientists in Universities, Research Institutes including ISAS/JAXA Phase of research Steering ISAS committees organization

Research based on interests of individual researchers Individual researchers Research Div.

Group of researchers

Space programs WG selection Project preparation WG Project working group

Development Phase up eval. Project team of project Project team Spacecraft operation Annual eval. Data reduction Research Div. 31 Data users Science Output Astroparticle Physics Int'l Forum October 17, 2012