ASTRO-H ASTRO-H and future missions in JAXA program. Tadayuki Takahashi PI/Project Manager on behalf of the ASTRO-H team
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1 ASTRO-H ASTRO-H and future missions in JAXA program Tadayuki Takahashi PI/Project Manager on behalf of the ASTRO-H team 1
2 Status The ASTRO-H Project is in Phase B, since 2008 Oct. (JAXA) 2009/Jan-Feb : Science Working Group members (science advisors) selected by NASA(8), ESA(3) and JAXA(2), Chair: A. Fabian 2009/Feb : 1st Collaboration Meeting (Science Meeting/3rd Design Meeting) 2009/June 4-5 : 4th Design Meeting (with two days splinter meeting) 2009/June 16: NASA entered Phase B International Sep-Jan: Sub System Level Review Feb-Mar: System Level PDR Nov-2011 April : MTM - TTM Feb-Mar: CDR ASTRO-H Feb-Oct: Integration Test Jan-Feb.: Launch (Planned) 2
3 From Suzaku to ASTRO-H XRT for CCD Hard XRT XRTs Micro Cal. & CCD Softγ Hard XRT XRT for Calorimeter 14 m Hard Xray Imagers 6.5 m Suzaku 3 ASTRO-H
4 ASTRO-H Features... Spectroscopy (for diffuse source) ASTRO-H Energy Coverage Chandra Area for SoftX-rays Suzaku Angular Resolution XMM Area for Hard X-rays
5 Design Parameters of Instruments Hard X-ray Imaging System (HXT+HXI) 5-80 kev Soft X-ray Spectrometer System (SXT-S+SXS) kev Soft X-ray Imaging System (SXT-I+SXI) kev Soft γ-ray detector (SGD) kev Specifications Effective area : 300 cm 2 (@30 kev) Spatial resolution : 1.7 arcmin (HPD) Energy resolution : 2 kev Field of view : 9 arcmin kev Energy resolution : 7 ev Spatial resolution : 1.7 arcmin (HPD) Effective area : 210 cm 2 (@6 kev) Field of view : 3 arcmin kev Spatial resolution : 1.7 arcmin (HPD) Effective area : 360 cm kev Energy resolution : 150 ev Field of view : 38 arcmin kev Effective area : 100cm kev Energy resolution : 2 kev (Requirement) Astrometric accuracy : <0.6 arcdeg (E<150 kev)
6 1. Soft X-ray Imager (SXI) AstroH SXI vs Suzaku XIS on A1795 Large FOV CCD (F.L. 5.6m) Energy resolution : 150 ev Field of view : 38 kev Astro-H SXI 4CCD chips/62x62mm 2 Spatial resolution : 1.7 arcmin (HPD) (requirement) R 200 Suzaku XIS Chandra ACIS XMM Hamamatsu Photonics
7 2. Soft X-ray Spectrometer (SXS) Hg 1-x Cd x Te, Si - High Resolution Spectroscopyby a micro calorimeter array Effective area : 210 cm 2 (@6 kev) Field of view : 3 arcmin kev Requirements (/Goal) Energy resolution Energy range Background rate Field of view 7 ev (FWHM) (4 ev(fwhm) Goal) kev 1.5 x 10-3 cts/s/kev 2.9 x 2.9 arcmin Detector array 6 x 6 Absorber size 800 µm Angular resolution Effective area Lifetime Maximum count rate Energy scale accuracy 1.7 arcmin HPD 160 / 210 cm 2 (at 1 / 6 kev) 3 years / 5 years 150 cts/s 2 ev with much more robust cooling system than that of Suzaku 7
8 - Improved Resolution for ASTRO-H - 8 Mitsuda
9 High Resolution X-ray Spectroscopy of 4-6 ev (FWHM) Velocity Structure of X-ray lines SNR Merging Cluster A2256 (z = 0.058) 1000 km/s 80 ksec x 2 Simple Simulation: 100ks Obs., Tycho SNR :two velocity components, seperated by ±2000km/s (blue and red)
10 High Resolution Spectroscopy by ASTRO-H (~2013) Turbulent motion in A2029 ASTRO-H measures bulk velocity flow as small as 300 km/s in the brightest 30 hot clusters (kt > 5 kev). ASTRO- H will push on X- ray astronomy to a new excigng phase by showing dynamical mogons in all scales in the universe with a micro- calorimeter. (cooled at 50 mk)
11 Line profile from a turbulent gas 100ks SimulaGon baseline, 7eV Perseus cluster (r<2, 100ks) vapec 3T (0.6keV, 2.6keV, 6.1keV)
12 3. Hard X-ray Telescope (HXT) Imaging at Higher Energies New Hard X-ray Telescope with large effective area 300 cm 2 (@30 kev) HXT SXT λ θ λ θ Pt C d Two Telescopes/ F. L. 12 m Mounted on the Fixed Optical Bench 12
13 4. Hard X-ray Imager (HXI) Cutting Edge Technology 1. Well-type BGO Active Shield (APD Readout) 2. Si/CdTe Hybrid Detector (Double Sided) VERY Careful Design to achieve Low Background CdTe Double Side Strip (CdTe: 1Layer) 30mm High Res. CdTe Diode (Cross Strips) 250 micron pitch Double Side Si Strip (Low Activation E< 25 kev) (DSSD: 4Layer) 9x9 arcmin 2
14 Simulation Comparison with INTEGRAL/IBIS image ASTRO-H HXI INTEGRAL IBIS ks/pointing by A.Bamba (Revnivtsev+04)
15 SN1006 with HXI HXI kev (100ks) SN kev pos. difference of cutoff? thermal parameters w. SXS -> acc. efficiency by A.Bamba
16 Obscured blackholes Terashima The origin of the CXB? ASTRO-H should directlyresolve out >30% at peak. 16
17 5. Soft Gamma-ray Detector (SGD) Higher Senstivity above 80 kev Completely New Approach to achieve Low Background Fine collimator Narrow FOV Si/CdTe Compton Detector θ Si Strips Concept E in E 1 APD BGO Compton camera CdTe Pixels cos θ = 1 m e c 2 ( 1 E 2 1 E 1 + E 2 ) 17 Gap ~3mm
18 With Polarization Measurement Capability Experimental Results by SGD prototype 100% polarized beam (SPring-8) 18 Takeda +,09
19 ASTRO-H Sensitivity for Hard Photons (Point Source) Background Sensitivity 19
20 ASTRO-H is the next generation of X-ray observatories ASTRO-H IXO Suzaku ASTRO-H is a jumping board to IXO Chandra XMM/Neton 20
21 Then, we will have a complete set of X-ray missions to work with BIG representatives from other wave length CTA/AGIS HESS/VERITAS/Cangaroo3 (Energy) Fermi Gamma-ray X-ray All-sky survey Gamma-ray satellite ASTRO-H/NuStar/ e-rosita/gems Chandra, XMM-Newton Suzaku Optical & infrared ASTRO-H is the observatory JWST Herschel ALMA Radio High-resolution interferometer in the millimeter band (Year)
22 Summary 1. ASTRO-H is a real mission. It s in Phase B both in Japan&US. 2. Wide-band/Low-background & Micro-Calorimeter Resolution. 3. Large International Collaboration (NASA/SRON/ESA/CSA/DAI/Geneva U. and more) 4. Many reasons to have ASTRO-H (This Conf.). 5. Best Match with BIG observatories in other wavelength Sensitivity (Point Source) Sensitivity (Diffuse Source) 22
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