The ASTRO-H Mission Tadayuki Takahashi ISAS/JAXA

on behalf of the ASTRO-H Team 1. X-ray 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.

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.

ASTRO-H is a powerful satellite for the next generation of X-ray Astronomy

2011//06/30 The X-ray Universe 2011, Berlin 2 2. ASTRO-H

ASTRO-H is an international X-ray observatory, which is the 6th in the series of the X-ray observatories from Japan. It is currently planned to be launched in 2014 with an H-IIA rocket from the Tanegashima Space Center, Kagoshima, Japan. European Participation SRON & U. of Geneva Filter Wheel for SXS CEA/DSM/IRFU Contribution to BGO Shield/ASICS for HXI ESA SGD (Soft Three Science Advisors from Europe Felix Aharonian Gamma-ray Andy Fabian (Chair: Science Advisor Team) Detector) Jelle Kaastra Contribution to SXS/HXI/SGD/HXT More than 160 scientists from Japan/US/Europe/Canada

SXI (X-ray CCD) SXS (Micro Calorimeter) weight 2.7 t HXI (Hard X-ray Imager)

2011//06/30 The X-ray Universe 2011, Berlin 3 2. ASTRO-H

2011//06/30 The X-ray Universe 2011, Berlin 4 2. ASTRO-H

1. Wide Band /High Sensitivity Observation 0.3 keV - 600 keV : Four Instruments including Hard X-ray Focusing optics

SXT-I SXI (telescope)

SXT-S SXS (telescope)

HXT HXI (telescope)

SGD

2. High Resolution Spectroscopy by a micro-calorimeter array

5 eV (FWHM) @ 6 keV

2011//06/30 The X-ray Universe 2011, Berlin 5 2. ASTRO-H Operation ASTRO-H is in many ways similar to Suzaku in terms of orbit, pointing, and tracking capabilities, ASTRO-H will be launched into a circular orbit with altitude 500–600 km, and inclination 31 degrees or less.

Science operations will be similar to those of Suzaku, with pointed observation of each target until the integrated observing time is accumulated, and then slewing to the next target.

All instruments are co-aligned and will operate simultaneously. Time Allocation (TBC) Phase 0 : !!3 Months !!: !Satellite/Instruments Check out Phase 1 : !!6 Months !!: !SWG 100 % (PV Phase, including Calibration) Phase 2 : !!12 Months : !SWG Carry Over 15 %, GO 75 %, !Observatory 10 % Phase 3 : !!!Rest of the mission : KeyProject 15 % (TBD) , GO 75 %, Observatory 10 % Data policy among J/Europe/US in the GO time, would be similar to the Suzaku case. But we are planning to introduce key-project type and/or early-data-released type observations from early phase of the mission.

2011//06/30 The X-ray Universe 2011, Berlin 6 3. ASTRO-H : Satellite

The entire structure forms a “telescope” In order to minimize thermal distortion, CFRP is used with thermal expansion coefficient of < 2!10-7

Side Panel 3 側面パネル３ Side Panel 2 側面パネル２

Side Panel 1 側面パネル１ Upper Coupliing上部連結金具 Fitting

Side Panel 4 側面パネル４ Total Length 14m

Side Panel 8 側面パネル８

EOB 側面パネル５Side Panel 5 Side Panel 7 側面パネル７ 6.3 m

Side Panel 6 側面パネル格子部Side Panel Lattice 側面パネル６

Base Panel Z ベースパネル Y X

A-HASTRO-H座標系 Coordinate アウトリガーOutrigger Rocketロケット結合リング Connection Ring HXIプレートHXI Plate 2011//06/30 The X-ray Universe 2011, Berlin 7 3. ASTRO-H : Soft X-ray Telscope for SXS & SXI

Soft X-ray Telescope (SXT) will be an ASTRO-H upgraded version of the Suzaku X-ray telescope (XRT). The diameter and focal length is larger, thus number of the nesting shells are increased.

Suzaku

EM quadrant fully illuminated by diverging X-ray beam from the source 100 m away (at GSFC)

HPD < 1.3 arcmin is achieved from the EM quadrant (the requirement is 1.7’)

NASA/GSFC/MSFC/Nagoya/ISAS

2011/03/15 CNR/Rome 8 3. ASTRO-H : Soft X-ray Imager (SXI): X-ray CCD

Large FOV X-ray CCD (F.L. 5.6 m) 4CCD chips/62x62mm2 Energy Resolution ~150 eV Depletion Layer ~200 micron

Field of view : 38 arcmin @6 keV

Flight CCD will be delivered this year (2011).

Coma cluster (ROSTA, S.L. Snowden) Recent Progress EM Model/ Thermal Balance Test (2011/June)

2011//06/30 The X-ray Universe 2011, Berlin 9 3. ASTRO-H : Hard X-ray Telescope (HXT) • Pt/C depth-graded multilayer X-ray telescope • Large photon collecting area above 10 keV. • Careful Calibration using SPring-8 Hard X-ray Beam line is going on

Incident X-ray (λ) Bragg Reflection 2 300 cm (@30 keV) nλ= 2d sinθ θ

Heavy Material (Pt)

Light Material (C)

gap (d)

HXT

SXT

HPD < 1.7 arcmin is the requirement

2011//06/302010/06/30 The SPIE X-ray Meeting, Universe San Diego 2011, Berlin 10 3. ASTRO-H : Hard X-ray Telescope (HXT)

Recent Progress Vibration Test (March 2011)

2011//06/30 The X-ray Universe 2011, Berlin 11 3. ASTRO-H : Hard X-ray Imager (HXI)

Si and CdTe Hybrid Imager ( 5 - 80 keV): Soft X-ray photons below < 20 keV are absorbed in the Si part (DSSD), while hard X-ray photons go through theSi part and are detected by the newly developed CdTe double sided cross-strip detector

Efﬁciency 100 % Double Side! 70 % Si Strip (Low Activation SiE< DSSD 25 keV)! (DSSD: 4Layer)! CdTe DSD CdTe ! 30mm! Double Side Strip! (CdTe: 1Layer)! 80 keV

“Stacked Si/CdTe Detector” and “Well-type BGO shield” 50 kg will reduce background

2011//06/30 The X-ray Universe 2011, Berlin 12 3. ASTRO-H : Hard X-ray Imager (HXI) :

Engineering Model 4 layer of Si DSSD and 1 layer of CdTe DSD CdTe DSD (ISAS)

250 micron pitch strips for both side

100 µm width slit φ3 mm hole bad strips histe2_000 800 µm pitch φ2 mm hole (open) !103 220 22000

200 Si DSSD 20000 CdTe DSD [mm] 180 FWHM 0.9 keV 18000 ~1.6 keV FWHM 160 @14 keV 16000 @ 60 keV 140 14000 120 241 241 Am 12000 Am

100Count 10000 80 8000 60 6000 40 4000 20 2000 0 0 10 20 30 40 50 60 0 10 20 30 40 50 60 70 Energy (keV) [mm] (a) (b) 2011//06/30 The X-ray Universe 2011, Berlin CdTe DSD 13 Power of Hard X-ray Telescope

Suzaku PIN

ASTRO-H SXT/SXI (1.7 arcmin, HPD)

ASTRO-H HXT/HXI 3. ASTRO-H: Performance of HXT + HXI

Imaging with hard X-ray optics will enable us to observe at x100 times higher sensitivity than Suzaku. 30-50% of the cosmic X-ray background will be resolved into hidden super-massive black holes. 30-50% of Hard XRB will be resolved

Ueda+ 03 NeXTNuSTAR/ limit ̃40-50% XRB ASTRO-H

SWIFT

2011//06/30 The X-ray Universe 2011, Berlin 3. ASTRO-H: Soft Gamma-ray Detector

• Si/CdTe Compton Gamma Camera and Well-type shield to achieve ultimately low background. (40 - 600 keV) • The Compton Camera enables us to measure polarization >60 keV. • GRB Monitoring using BGO shield.

During Vibration Test by using a Mass Model Si/CdTe Compton Camera (only select gamma-rays from the FOV)

Compton Kinematics

2 1 1 cos θ =1− mec − !E2 E1 + E2 " BGO Ein = E1 + E2

2011//06/30 The X-ray Universe 2011, Berlin 16 3. ASTRO-H: Wide-band Observation is so important!

0.5 keV 10 keV 300 keV Suzaku Cyg X-1 Spectra (by S. Yamada) " " 20 ks 2 2 í í ($%& ($%& í í !! !! (/ (/ í í 40 ks Observing Time ()*+,-,./(01 ()*+,-,./(01 ' 2009/06/02 14 ks ' "#! "#! $%& 2008/04/18 27 ks $%& 2007/04/30 38 ks 10 keV 100 keV "#"! "#"! !!" !"" 3.%456()$%&2

2010/06/30 SPIE Meeting, San Diego 17 3. ASTRO-H: SGD Performance - Magnetar 4U 0142+61

SGD will be able to measure spectra up to 600 keV with higher quality, and will constrain the nature of the hard component.

SGD simulation (100 ks)

(Simulation by T. Enoto)

2010/06/30 SPIE Meeting, San Diego 18 3. ASTRO-H: Soft X-ray Spectrometer (SXS) Micro calorimeter array Detector to be Filter Wheel Operated at 50 mK

Liq. He+2stageST Cooler＋JT Cooler+ADR

2010/06/30 SPIE Meeting, San Diego 19 3. ASTRO-H: Soft X-ray Spectrometer (SXS) - High Resolution Spectroscopy by a micro calorimeter array

2 210cm @6keV for micro-calorimeter

2011//06/30 The X-ray Universe 2011, Berlin 20 3. ASTRO-H: Soft X-ray Spectrometer (SXS) - High Resolution Spectroscopy by a micro calorimeter array

2 210cm @6keV for micro-calorimeter

2011//06/30 The X-ray Universe 2011, Berlin 21 3. ASTRO-H: Soft X-ray Spectrometer (SXS)

EM Detector System (Detector Assembly + Detector Array + Anti-co Detector)

NASA/GSFC

2011//06/30 The X-ray Universe 2011, Berlin 22 3. ASTRO-H: Soft X-ray Spectrometer (SXS)

EM CSI as of 5/31/2011

NASA/GSFC

2011//06/30 The X-ray Universe 2011, Berlin 23 3. ASTRO-H: Soft X-ray Spectrometer (SXS) Very Recent Results based on the Engineering Model of ASTRO-H

4.1 eV (FWHM)

NASA/GSFC

2011//06/30 The X-ray Universe 2011, Berlin 24 3. ASTRO-H: SXS EM Dewar in progress

ISAS/JAXA & SHI 2011//06/30 The X-ray Universe 2011, Berlin 25 4. ASTRO-H Science : Black Hole GRO J1655-40 The superior resolution of SXS in the Fe K band enables the unambiguous detection of weak and narrow lines from a wind. Chandra ASTRO-H (50ks) Same Model Parameters with the Chandra result

Lines are saturated but not black due to scattering, resolution.

Running out of S/N

(Simulation by J. Miller) ASTRO-H SXS can handle 250 cts/s 2011//06/30 The X-ray Universe 2011, Berlin 26 4. ASTRO-H Science : 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 27 4. ASTRO-H Science : Fe line from AGN