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Astro-E2 and Japanese future space programs for high energy astrophysics

Astro-E2 and Japanese future space programs for high energy astrophysics. Tadayasu Dotani (ISAS). Astro-E2 NeXT XEUS Small satellite programs. Astro-E2.

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Astro-E2 and Japanese future space programs for high energy astrophysics

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  1. Astro-E2 and Japanese future space programs for high energy astrophysics Tadayasu Dotani (ISAS) Astro-E2 NeXT XEUS Small satellite programs

  2. Astro-E2 A powerful X-ray observatory developed under Japan-US collaboration. It is a recovery mission of Astro-E, which was failed in February, 2000. • High spectral resolution (DE~10 eV) with a micro-calorimeter. • Very large, simultaneous bandwidth (0.5–600 keV). • Large collecting area with high sensitivity. • Launch: 2005/1-2

  3. Scientific Instruments on-board Astro-E2 XRT Pre-collimator (Astro-E2) HXD

  4. Scientific Instruments on-board Astro-E2 XRS XIS Mechanical Cooler(Astro-E2)

  5. Astro-E2: Effective Areas Non-imaging Detector XRT+FPD

  6. Resolving power of the micro-calorimeter (XRS)

  7. Effective Area of XRS

  8. Simulated Spectra: A2199 (higher energy part) BeppoSAX observations indicated the presence of a hard tail. ASCA GIS Hard tail can be clearly detected. Astro-E2: 100 ks

  9. Simulated Spectra: A2199 (lower energy part) Z=0.03 Good statistics of XIS and high resolution of XRS work complementary. XIS XRS Triplet lines from He-like iron are easily resolved. Astro-E2: 100 ks

  10. Comparison of the 3 X-ray observatories Astro-E2 Chandra XMM-Newton

  11. NeXT(Next X-ray telescope) A next generation X-ray observatory following Astro-E2 • X-ray supermirror capable of focusing up to ~80 keV. • Hybrid detector covering 0.1–80 keV. • Large format TES calorimeter for high-resolution imaging spectroscopy. • Soft g-ray detector with high sensitivity. • Launch: ~2010?

  12. Key Technology: supermirror Bragg reflection Soft X-rays Model calculation Hard X-rays Pt C • Incident angle = 0.169 deg • 15 blocks • 95 layers • Periodic length = 3–12 nm

  13. Effective Area of the Supermirror 12 cm Focal length = 12m 60 cm 40 cm 8 m 6 m Number of nest = 272

  14. Balloon Experiment of the Supermirror InFOCmS • Collaboration between Nagoya Univ. & NASA/GSFC • First imaging observation in 20-40 keV with the supermirror. • Launched on July 5, 2001, from Texas, USA. • Succeeded to observe Cyg X-1

  15. CdTe VA2TA(IDE) Development of Detectors for NeXT (2) Hybrid detector (1) TES micro-calorimeter Upper stage: Thinned CCD (<10 keV) Lower stage: Pixel detector (>10 keV) CdTe, etc. 3-side buttable CCD developed by HPK CdTe pixel detector with analog VLSI Superconducting magnet Heat switch Salt pill

  16. XEUSX-ray Evolving Universe Spectroscopy mission • Effective area 30 m2 (@1keV) with a focal length of 50 m. • Formation flight between the mirror satellite (MSC) and the detector satellite (DSC). • Mirror satellite evolves from XEUS1 (6 m2) to XEUS2 (30 m2) using ISS. • Concept design are being made under ESA/Japan collaboration. • Launch: 2013 or later.

  17. Optical baffle Mirror satellite (MSC1) Formation Flight Docking port 50 m Optical bench Mirror Detector satellite Thermal baffles, launch support structure • Mirror satellite takes a Kepler orbit. • Detector satellite takes a non-Kepler orbit to follow the mirror satellite. • Alignment accuracy of the two satellites should be better than 1mm.

  18. Upgrading the mirror satellite: MSC1→MSC2

  19. XEUS - Sensitivity Comparison • A limiting sensitivity of 4×10-18 erg cm-2 s-1 – about 250 times deeper than XMM-Newton. • The sensitivity of XEUS is well matched to that of the new generation of observatories working in other wavebands.

  20. Small Satellite Programs • Small satellites: 10 kg – a few hundreds kg. • Appropriate launch system (including vehicles) needs to be established. • Small satellite programs include following possibilities: • XMAS - X-ray milli-Arcsecond Satellite • DELUXS - Diffuse Emission from Large-scale Universe X-ray Spectrometer • Solid-state Compton telescope to detect polarization in GRB • Large area CCD satellite • Wide-field, hard X-ray survey satellite • Wide-field, imaging survey satellite with soft X-ray telescope • X-ray polarization detector

  21. Summary of the future programs 2015 2010 2005 Astro-E2 Tests Fabrication Launch NeXT Tests Design Fabrication Launch Basic research Tests Design Fabrication XEUS1 XEUS2 Small satellite programs

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