The High Resolution X-ray Spectrometer, SXS, on the Astro-H mission
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1 The High Resolution X-ray Spectrometer, SXS, on the Astro-H mission K. Mitsuda Institute of Space and Astronautical Science (ISAS) Japan Aerospace Exploration Agency (JAXA) High resolution X-ray spectroscopy: towards IXO, MSSL, March 18-19, 2009
2 Hard X-ray imaging Spectroscopy (2-80 kev) Soft X-ray high-resolution Spectroscopy (FWHM 7eV) Evolution of super massive black holes Evolution of clusters of galaxies Accelerations in clusters and SNRs Vicinity of black holes Present status: phase B. Present expected launch date: JFY 2013.
3 Astro-H Science Payloads Soft X-ray Telescope for CCD (5.6m focal length) Hard X-ray Telescopes (12 m focal length units) SXS Telescope Thin foil mirror 45cm diameter, 5.6m focal length, 1 resolution Soft X-ray Imager (CCD) Soft Gamma-ray Detectors (2 units) Hard X-ray Imagers (2 units) 12 m SXS-XCS (Soft X-ray Spectrometer - X-ray Calorimeter System) 8x8 µ-calorimeter array FWHM < 7 ev resolution 4 x4 FOV
4 Soft X-ray Spectrometer, SXS High resolution X-ray spectrometer using a microcalorimeter array High Energy resolution (FWHM<7eV) and modest imaging (6x6 or 8x8) capabilities SXS XRT (SXT-S) Thin foil mirror 45cm diameter, 5.6m focal length, 1 resolution Microcalorimeters High quantum efficiency Imaging capability 50 mk SXS-XSC Dewar Soft X-ray Spectrometer - X-ray Calorimeter System 8x8 µ-calorimeter array 7 ev resolution 4 x4 FOV
5 Astro-H SXS collaboration X-ray Calorimeter System (SXS-XCS) ISAS/JAXA ARD/JAXA Tokyo Metropolitan University Kanazawa University Riken Rikkyo University Saitama University National Inst. Material Science Tsukuba University NASA/GSFC University of Wisconsin Yale University NASA/AMES Telescope (SXS-XRT) ISAS/JAXA Nagoya University Tokyo Metropolitan University Ehime University NASA/GSFC SRON University of Geneva Participation to be decided. High resolution X-ray spectroscopy: towards IXO, MSSL, March 18-19, 2009
6 SXS requirements and goal Baseline Goal XRS Pixel size 814µm 624µm Array format 6 x 6 (32 pixel readout) 8 x 8 (64 pixel readout) 6 x 6 (32 pixel readout) (FOV) Effective area@1kev Effective area@7kev Energy Resolution Lifetime 3.0 x x x cm cm cm cm 2 7 ev 4 ev (12 ev) 7 ev 3 years > 5 years (>2 years) whole the SXS system is designed to handle 8x8 array High resolution X-ray spectroscopy: towards IXO, MSSL, March 18-19, 2009
7 Field of View Telescope HPD ~ calibration pixels Pixel gap is not in scale. Filling factor > 95%
8 Astro-H SXS thin filter Astro-H SXS baseline filter Suzaku 100 XMM-Newton Chandra 0 Effective Area (cm-2) 400 Effective area Energy (kev) 5 10 High resolution X-ray spectroscopy: towards IXO, MSSL, March 18-19, 2009
9 Energy resolution improvement Suzaku XRS flight data (Kelley+ 2007) 7 ev Improvement in energy resolution at laboratory level (Kelley+ 2008) Lower operating temperature (60mk 50mK) Lower Heat Capacity (~factor 4) Hg 1-x Cd x Te, x = 0.16, µm MnKα 1,2 profile 50 mk heat sink 4.2 ev XRS Array (HgTe) XRS (HgTe) 1/4 HgTe HgCdTe
10 Energy resolution Chandra LETG Chandra HETG-HEG Chandra HETG-MEG (10 7 K) 100 km/s 100 km/s /!100 XMM RGS Astro-H (4eV) Suzaku XRS Astro-H (7eV) Compton CCD X-ray Energy kev High resolution X-ray spectroscopy: towards IXO, MSSL, March 18-19, 2009
11 SXS system Op;cs: NASA/GSFC Contribution Soft X-ray Telescope Filter Wheel + Cal sources Gate Valve Aperture Cylinder + Optical Blocking FIlters Refrigera;on & Electronics: Calorimeter Electronics: Detector Assembly Amplification & Digitization ISAS/JAXA Contribution SRON (& Geneva) Contribution Digital signals Analog signals Power ADRC Pulse Shape Processor SCD Shield Coolers Helium Cryostat ADR Xbox PSP Science Data JT Cooler + Pre-coolers Dewar JTD PCD PSU DIST Instrument Digital Control (IDC) & SpaceWire Router (SWR) S/C Bus High resolution X-ray spectroscopy: towards IXO, MSSL, March 18-19, 2009
12 Cooling Requirements Requirement Goal interface Stability Lifetime 47 mk 47 mk 1µK rms in 20s -10mim 0.5 µk rms 3 years 5 years Heat load from detector (FEA) (He)* (IVCS) FEA = detector Front-End Assembly * Dependent on IVCS temperature High resolution X-ray spectroscopy: towards IXO, MSSL, March 18-19, 2009
13 Cooling system: Cooling chain 290 K 100K 100K shield 2ST 20K shield H/Ps 2ST Redundant 2ST 2ST 15K Redundant 20K 1.8K 3 He JT Redundant 1.3K(1.8K) LHe (30L) He ballast ADR (GLF) 120g, 2 T 0.5K 2K shield in He tank ADR (CPA) 240g, 2T 50mK 0.4 µw H/Ps Astro-H EM 3 He JT cooler Radiators 270 K
14 Cooling system: LHe expected life Case Cooler Power (W) Heat load to He tank (mw) Lifetime of LHe (years) 1 Normal Shield cooler 50x2 Precooler 50x2 JT (0.3 from FEA) Failure of one shield cooler Shield cooler 90x1 Precooler 50x2 JT (0.6 from FEA) Failure of JT compressor Shield cooler 90x2 Precooler 50x2 JT (0.1 from FEA) Failure of one JT precooler Shield cooler 90x2 Precooler 90x1 JT (0.1 from FEA) + Observation continues as far as 3 He JT cooler works High resolution X-ray spectroscopy: towards IXO, MSSL, March 18-19,
15 Science with the SXS Ask people in this room
16 Main scientific objectives of the SXS Energy budget of clusters of galaxies and SNRs Thermal energy, bulk motion/turbulence energy, [and non-thermal energy by HXI] Gravitational potential and spin of black holes Broad/narrow emission/absorption lines Chemical enrichment of ICM and IGM; when, where, how elements are created and dispersed? N-Ni abundances of galaxies and clusters, resolving K and L lines Constraints on cosmological parameters from clusters Precise determination of mass of 30 nearby clusters, by measuring temperature, pressure, and bulk motion/turbulence.
17 A simulated Asto-H observation Chandra T map Sun et al. (2002) Cluster merger, A2256 HXT-HXI image E>10 kev Imaging observation A2256 is crucial to discriminate out the AGN contribution. SAX spectrum Fusco-Femiano et al. (2000) Spectrum by SXI-HXI-SGD Spectrum by Micro-calorimeter (SXS) 6.30 kev 6.35 kev SXI 1keV HXI SGD 1MeV
18 Summary Astro-H is presently in phase-b, and expected to be launched in JFY 2013 (2012 summer or 2013 winter). The Soft X-ray Spectrometer (SXS) consists of a focusing X-ray telescope and a microcalorimeter-array, and is developed by Japan-US collaboration with European participation. Effective area = 225cm 7 kev Energy resolution (FWHM) 7 ev Field of view = 4. 1 x 4. 1 with 8x8 pixels Operation life 3 years Main scientific objectives of the SXS Energy budget of clusters and SNRs Gravitational potential and spin of black holes Chemical enrichment of ICM and IGM Cosmological parameters from cluster mass
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