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Space X-ray Astronomy

Current and Future Space X-ray astronomy Missions in China Chen Zhang represent Prof. Shuang-Nan Zhang Institute of High Energy Physics National Astronomical Observatory Chinese Academy of Sciences zhangchen12@gmail.com zhangsn@ihep.ac.cn. Space X-ray Astronomy. Matter under extreme conditions

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Space X-ray Astronomy

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  1. Current and Future Space X-ray astronomy Missions in ChinaChen Zhangrepresent Prof. Shuang-Nan ZhangInstitute of High Energy PhysicsNational Astronomical Observatory Chinese Academy of Scienceszhangchen12@gmail.comzhangsn@ihep.ac.cn

  2. Space X-ray Astronomy • Matter under extreme conditions • Formation of structure • Life cycle of matter and energy AXRO 2009, Prague

  3. An overview of Space astronomy Missions in China • Still no space astronomy satellite launched up to now • Focusing on high energy astrophysics and solar physics, developing the space optics, radio,  gravitational wave and dark matter detection. • Strengthen international cooperation • Recent scientific programs • “Black Hole Probe” (BHP): HXMT, SVOM, Polar • “Diagnostics of Astro-Oscillations” (DAO): XTP,… • “Portraits of Astrophysical Objects” (PAO), dark matter detection, solar microscope, solar portraits Prof. S.N. Zhang is the coordinator of BHP, DAO and PAO programs. AXRO 2009, Prague

  4. The Hard X-ray Modulation Telescope: planned for launch around 2010-2011 Based on the direct demodulation (DD) method Ready for Phase C/D: 2007: official announcement of selection as China’s first dedicated astronomy; 2008: completion of phase A. Full funding decision not made yet! AXRO 2009, Prague

  5. Main science of HXMT • Broad band (1-250 keV) and large collection area (5000 cm2@100 keV) • Hard X-ray full sky survey • A high precision hard X-ray sky map • About 1000 new hard X-ray sources • Diffuse background and cosmic variance • Discover highly obscured supermassive BHs • Pointed observations of high energy sources • Dynamics and radiation near compact objects: X-ray binaries, AGNs, SGRs • Clusters of galaxies, GRBs, SNRs AXRO 2009, Prague

  6. HXMTfull sky survey • 1 year exposure map AXRO 2009, Prague

  7. HXMT Pointed Observation • Power spectrum • Light curve AXRO 2009, Prague

  8. Low Energy X-ray Instrument (LE) (1-15 keV) SCD, 384 cm2 Detectors onboard High Energy X-ray Instrument (HE) (20-250 keV) NaI(Ti)/CsI(Na) crystal 18 modules, 5000 cm2 Medium Energy X-ray Instrument (ME) (5-30 keV) SiPIN, 952 cm2 AXRO 2009, Prague

  9. HXMT characteristics AXRO 2009, Prague

  10. HXMT HE characteristics 20-250 AXRO 2009, Prague

  11. China-France joint GRB mission: SVOM Main Science GRBs: Diversity and unity, Radiation processes, Early afterglow, GRB-supernova connection, Short GRB progenitors Cosmology and Fundamental Physics : Star formation, Host galaxies, Cosmological parameters, Probing Lorentz invariance… AXRO 2009, Prague

  12. China-France joint GRB mission: SVOM ECLAIRs: Hard X-ray Imager 4-150 keV VT: 45 cm Visible Telescope • Status • phase A has ended • phase B to start soon • reviews completed from both sides • China & France funding approved • Planned launch in 2013-2014 GRM: Gamma-Ray Monitor 30-5000 keV (IHEP) Star sensor XIAO: Soft X-ray Telescope 0.5-2 keV Service platform AXRO 2009, Prague

  13. China-France joint GRB mission: SVOM • Goals (beyond Swift) • Higher redshift GRBs (with ECLAIRs) • Deeper and more uniform sampling of optical afterglows (with XIAO & VT) • Better E_peak measurements (with GRM) AXRO 2009, Prague

  14. Gamma-ray burst polarization experiment onboard China’s Spacelab: POLAR GRB prompt emission polarization: one of the last observables of GRBs • Different GRB models • E-M Model: well defined, moderate Plin ~ 50% • Fireball Model: high values excluded Plin ~ 10-20 % • Cannon ball Model: full range possible Plin = 0 - 100% • Probe quantum gravity (???): • Amelino-Camelia G., 2000, Nature, 408, 661 • Piran T, 2005, Lect. Notes Phys, 669, 351 • Fan, Y-Z; Wei, D-M; Xu, D. 2007, MNRAS, 376, 1857 From M. Lyutikov, 2003 See papers discussing various GRB models: T. Piran, A. Dar, M. Lyutikov, D. Eichler, G. Ghisellini, D. Lazzatti, M. Medvedev, E. Rossi etc. AXRO 2009, Prague 14

  15. Gamma-ray burst polarization experiment onboard China’s Spacelab: POLAR Tian-Gong 天宫 Palace in Heaven • Onboard China’s spacelab TG-2: launch time 2011-12 • A China-led international collaboration (Switzerland, France, Poland) • FOV of POLAR: ~½ sky • Plastic scintillator stacks Instrument concept proposed by N. Produit, et al., NIM (2005) AXRO 2009, Prague

  16. POLAR capability summary • 10 GRBs per year down to 8%, or • 60 GRBs per year down to 30%, or 100 GRBs per year down to 50%polarization, if all POLAR GRBs are localized independently to ~degrees accuracy by other GRB instruments. AXRO 2009, Prague

  17. X-ray Timing and Polarization (XTP) mission • Science • Precise Light curve: Matter under extreme conditions, Neutron Star state equation, BH basic parameters formation and growth … • Polarization of X-ray: Radiation mechanism… • Diffuse X-ray emission, Gas distribution in Galaxy • … • Goal • The most sensitive light curve and polarization observation at 1-30 keV • Effective area • Low energy end, MCP @0.5-2 keV, the same about IXO • High energy end, Multilayer @30 keV, ~ 10 times of IXO AXRO 2009, Prague

  18. X-ray Timing and Polarization (XTP) mission Using a large array of small telescopes to achieve a very large collection area  competitive w.r.t. IXO for temporal and spectral studies of X-ray binaries and bright AGNs. Sacrifice angular resolution (~1’) in exchange for large collection area  technically easier Soft X-ray telescope Hard X-ray telescope Hard X-ray polarization telescope All-sky monitor Soft X-ray polarization telescope AXRO 2009, Prague

  19. HERO concept: High Energy Replicated Optics –Small Aperture, Short Focal Length and Shallow Grazing Incidence Using a small mirror array to achieve a large collection area: technically more feasible than single large mirror. Ramsey et al, SPIE 2000 • Full-shell shallow-graze-angle iridium-coated replicated mirrors • Complex coating procedures avoided • Requirements for mirror surface quality relaxed Shuang-Nan Zhang @ University of Ferrara, Italy

  20. MCP X-ray Optics Pore glass coated with Iridium: extremely light weight, compact and robust (Fraser et al 2009) Shuang-Nan Zhang @ University of Ferrara, Italy

  21. XTPtimeline and funding • 2010 R&D (Phase 0, A) • CAST and IHEP XTP platform: € 50 K • IHEP detector: € 180 K • CAS XTP Phase 0, A: € 500 K • NSFC detector and mirror: € 320 K • NAOC X-ray lab: € 400 K (applied) • 2012-13: Phase B • 2018 launch: before IXO AXRO 2009, Prague

  22. Summarization • “Black Hole Probe” program • HXMT: hard X-ray observation, around 2010-2011 • SVOM: GRB, 2013-2014 • Polar: GRB polarization, 2011-2012 • “Diagnostics of Astro-Oscillations” program • XTP: Light curve and polarization, Phase A • “Portraits of Astrophysical Objects”, dark matter detection, solar microscope, solar portrait AXRO 2009, Prague

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