JAXA,NASA,Aoyama Gakuin U.,Cambridge U.,CEA/DSM/IRFU,CfA/Harvard, Chubu U.,Chuo U.,Columbia U.,Dublin Institute for Advanced Studies,Durham U.

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1 JAXA,NASA,Aoyama Gakuin U.,Cambridge U.,CEA/DSM/IRFU,CfA/Harvard, Chubu U.,Chuo U.,Columbia U.,Dublin Institute for Advanced Studies,Durham U.,Ehime U.,ESA, Gunma Astronomical Observatory,Hiroshima U.,Kanazawa U.,Kobe U.,Kogakuin U.,Kyoto U.,Michigan U.,MIT,Miyazaki U.,MPIK,Nagoya U.,Nara Women's U.,Nihon Fukushi U.,Nihon U.,NIMS,Osaka City U.,Osaka U.,RIKEN,Rikkyo U.,Rutgers U.,Saitama U.,Shibaura Inst. Tech.,SRON,Stanford U./KIPAC,STScI,Toho U.,Tokyo Inst. Tech,Tokyo Metropolitan U.,Tokyo Science U.,Tsukuba U.,U. Maryland, U. of Geneva, U. of Tokyo, Waseda U.

2 1. X-ray Universe X-ray observations using space telescopes revealed that the Universe is full of hightemperature phenomena reaching 10 to 100 million degrees, which nobody had imagined before the advent of the X-ray astronomy. Gas at temperatures of million degrees. Remnants of exploded stars Matter falling into black holes and neutron stars Stellar coronae Winds from star-forming galaxies Electrons accelerated in strong magnetic fields (~ Gauss). Electronic transitions in partially ionized atoms of atomic number greater than or equal to 4 (Be). Recent studies show that phenomena observed in X-rays are deeply connected to those observed in other wavelengths. An X-ray mission is indispensable to maximize the scientific yields expected by large radio, infrared, and optical missions.

3 2. ASTRO-H X-ray Astronomy Satellite ASTRO-H is in Phase-C (Detal Design Phase) Launch Year : 2014 Launch site: Tanegashima Space Center, Japan Launch vehicle: JAXA H-IIA rocket Orbit Altitude: 550km Orbit Type: Approximate circular orbit Orbit Inclination: ~31 degrees Orbit Period: 96 minutes Total Length: 14m Mass: <2.6 metric ton Power: <3500 W Telemetry Rate: > 8 Mbps (X-band) Recording Capacity: > 12 Gbits Mission life : > 3 years Suzaku (6m, 1.7t) ASTRO-H 14 m

4 3. ASTRO-H Scientific goals and Objectives Observing the Dynamic Universe and Studying its History with the Ultimate Goal of Understanding the Structure and Evolution of the Universe Scientific objectives : Revealing the large-scale structure and its evolution of the Universe Understanding the extreme conditions in the Universe Exploring the diverse phenomena of non-thermal Universe Elucidating dark matter and dark energy Key features : 1. One of the first imaging and spectroscopic observations with the hard X-ray telescope. 2. The first spectroscopic observations with an extremely high energy resolution of the micro-calorimeter. 3. The most sensitive wideband observation over an energy range from 0.3 to 600 kev. 4

5 4. ASTRO-H Mission Instruments Spectroscopy (for diffuse source) ASTRO-H Energy Energy Coverage Coverage Area for SoftX-rays Chandra Suzaku SXT-S (telescope) SXS Soft X-ray Spectrometer System kev - Large Area Soft X-ray Telescope - X-ray micro calorimeter - super resolution (<7eV at 6 kev) SXT-I (telescope) SXI HXT (telescope) HXI Angular Resolution Hard X-ray Imaging System XMM Area for Hard X-rays - Hard X-ray Telescope (5-80 kev) - Focal Length 12 m - New CdTe Imager (Fine Pitch Cross Strip) Soft X-ray Imaging System kev - Large Area Soft X-ray Telescope - Large FOV 38x38 arcmin 2 - CCD spectroscopy SGD Soft Gamma-ray Detector kev non-imaging - Si/CdTe Compton Camera with Narrow FOV Active Shield - most sensitive gamma-ray detector ever

6 4. ASTRO-H Mission Instruments Sunshades X-rays Hard X-ray Telescopes (HXT) Focal Length = 12m Fixed Optical Bench Soft X-ray Telescopes (SXT-S, SXT-I) Focal Length = 5.6 m SXT-I HXT2 HXT1 Solar power Microcalorimater (SXS) Radiator X-ray CCD (SXI) Hard X-ray Imagers (HXI) SXT-S Deployable Optical Bench Soft γ-ray detectors (SGD) Radiator

7 4. ASTRO-H Mission Instruments Pt/C depth-graded multilayer X-ray telescope, original to Japan. Large photon collecting area above 10 kev. Light-weight design as a heritage of Suzaku. Proven technology by balloon experiments. Bragg Reflection 300 cm 2 (@30 kev) HXT SXT Nagoya/Ehime/ISAS/Kobe/Chuo and more

8 4. ASTRO-H Mission Instruments A High Resolution CdTe imager combined with Si imagers for wide dynamic range CdTe Cross strips 34 mm x 34 mm (9 x 9 arcmin) 0.75 mm thick 250 μm strip pitch kev CdTe Ge Si Thickness (mm) Absorption Efficiency (%) at ISAS High Eff. High E resolution kev ISAS/UT/ Waseda/ Saitama/ Stanford/ Hiroshima/ CEA and more Stacked configuration Newly developed CdTe Cross strip detector ISAS CdTe! Double Side Strip! (CdTe: 1Layer)! 30mm! High Spatial Resolution (250 μm) Double Side! Si Strip (Low Activation E< 25 kev)! (DSSD: 4Layer)! ISAS

9 4. ASTRO-H Mission Instruments X. Soft X-ray Spectrometer (SXS/XCS) Requirements (/Goal) High Resolution Spectroscopyby a micro calorimeter array AS T R O -H/SXS ISAS/Kanazawa/Metro U./ Riken/GSFC/SRON/ Geneva U and more Preliminary Design Review, March 10-12, 2010 Energy resolution 7 ev (FWHM) (4 ev(fwhm) Goal) Energy range kev Field of view 2.9 x 2.9 arcmin Detector array 6x6 Absorber size 800 µm Effective area 160 / 210 cm2 (at 1 / 6 kev) NASA Goddard Space Flight Center 6 エネルギー (電子ボルト) 2010/06/30 SPIE Meeting, San Diego 2010年7月1日木曜日 9

10 4. ASTRO-H Mission Instruments Operating Temperature 50 mk X-rays Liq. He+2stageST Cooler JT Cooler+ADR

11 4. ASTRO-H Mission Instruments Soft X-ray Telescope (SXT) will be an upgraded version of the Suzaku X-ray telescope (XRT). The diameter and focal length is larger, thus number of the nesting shells are increased. (1) thicker aluminum substrate for the larger radii, (2) more forming mandrels for better substrate shaping (3) precise alignment bars (4) glue to fix reflectors on the alignment bars (5) stronger housing. For Both SXS and SXI GSFC/MSFC/ / /ISAS

12 4. ASTRO-H Mission Instruments Large FOV X-ray CCD (F.L. 5.6 m) Osaka/Kyoto/ISAS/Miyazaki/ Kogakuin/RIkkyo and more

13 4. ASTRO-H Mission Instruments New cocepts of Si/CdTe Compton Camera and Well-type shield to achieve ultimately low background. Stanford/ISAS/Hiroshima/ UT/Waseda/Saitama/Aoyama/ Kanazawa and more + Polarization Measurement

14 5. ASTRO-H Mechanical Structure The entire structure forms a telescope In order to minimize thermal distortion, CFRP is used with thermal expansion coefficient of < Side Panel 3 Side Panel 2 Upper Coupliing Fitting Side Panel 1 Side Panel 4 Side Panel 8 Side Panel 5 Side Panel 6 A-H Coordinate Rocket Connection Ring Side Panel 7 Side Panel Lattice Base Panel Outrigger HXI Plate

15 6. ASTRO-H Science Cluster of Galaxies Dynamics Turbulance, Collisions) Non-thermal Emission Cluster Outskirt Site of Sturcture Formation Temperature Map Heavy Metal Distribution Simulation of Centaurus Cluster To the virial radius, and beyond M.R. George et al SXI FOV Astro-H will detect bulk velocity flow as small as 300 km/s in the brightest 30 clusters with T > 60 x 106 K (kt > 5 kev.)

16 6. ASTRO-H Science Merging Cluster A2256 (z = 0.058) Perseus cluster (r<2, 100ks) vapec 3T (0.6keV, 2.6keV, 6.1keV) micro Calorimeter Spectrum 1000 km/s 80 ksec x 2 Wide band Spectrum

17 6. ASTRO-H Science Supernova Remnants SN kev (100ks) The combination of ASTRO-H's hard Xray 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 particles. SN1006 by ASTRO-H by A.Bamba Site of Particle Acceleration to map electon distribution with E=Emax RXJ1713 Suzaku at 40 kev ASTRO-H at 40 kev -39d30m -40d00m 17h16m 17h14m 17h12m by T. Tanaka 2010/06/30 SPIE Meeting, San Diego 2010年7月1日木曜日 17

18 6. ASTRO-H Science Imaging with hard X-ray optics will enable us to observe at x100 times higher sensitivity than Suzaku % of the cosmic X-ray background will be resolved into hidden super-massive black holes. Soft Gamma-ray Spectrum up to several hundred kev by SGD for bright AGN

19 7. ASTRO-H Team -- International Collaboration Aoyama Gakuin U., Chubu U.,Chuo U.,Ehime U.,Gunma Astronomical Observatory,Hiroshima U.,Kanazawa U.,Kobe U.,Kogakuin U.,Kyoto U.,,Miyazaki U.,Nagoya U.,Nara Women's U.,Nihon Fukushi U.,Nihon U.,NIMS,Osaka City U.,Osaka U.,RIKEN,Rikkyo U.Saitama U.,Shibaura Inst. Tech.,Toho U.,Tokyo Inst. Tech,Tokyo Metropolitan U.,Tokyo Science U.,Tsukuba U.,U. of Tokyo, Waseda U. SXS ASTRO-H HXI SGD SXS AMC

20 8. Summary ASTRO-H is a major X-ray OBSERVATORY in 2010 s and is a juming board to future large X-ray satellites, such as IXO. ASTRO-H is now in Phase C. a) The ASTRO-H Project has been authorized to proceed into Phase C/D by SAC (Space Activity Commission) in Japan. SAC confirms that the ASTRO-H project is ready to proceed to the development phase. b) JAXA and NASA PDR have been completed. Next major step is the CDR (crytical design review) in /06/30 SPIE Meeting, San Diego 2010年7月1日木曜日 20

21 Appendix. ASTRO-H Scientific goals and Objectives Revealing the large-scale structure of the Universe and its evolution Observe clusters of galaxies, the largest structure of the Universe, and uncover their entire picture of interplays among thermal energy, kinetic energy of matter, and non-thermal energies, and see dynamic evolutions of clusters of galaxies. Unveil super massive black holes behind thick intervening material in the distant past with a 100 times higher sensitivity than Suzaku, and reveal the role they play in the galaxy evolution and formation. Understanding the extreme conditions in the Universe Measure the motion of matter at extreme proximity of black holes, sense the gravitational deformation of the space, and understand the structure of relativistic space-time. Exploring the diverse phenomena of non-thermal Universe Derive the physical condition of the sites where high energy particles (cosmic rays) gain energy, and elucidate the process in which gravity, collision, and explosions give rise to cosmic rays Studying dark matter and dark energy Obtain the distribution and total mass of dark matter in clusters of galaxies at different distances (ages), and study the roles of dark matter and dark energy in the evolution of clusters of galaxies 21

22 Appendix. ASTRO-H - Synergy with other BIG missions ASTRO-H will be the only General Observatory in X-ray in 2010 s. There is a world-wide devoid of future X-ray missions around 2013.An X-ray mission is indispensable to maximize the scientific yields expected by large radio, infrared, and optical missions. (Energy) HESS/MAGIC/VERITAS/Cangaroo3 CTA/AGIS Gamma-ray X-ray Fermi AGILE All-sky survey Gamma-ray satellite INTEGRAL Chandra, XMM-Newton Suzaku MAXI Optical & infrared Herschel JWST Radio High-resolution interferometer in the millimeter band. ALMA (Year)