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From INTEGRAL to SIMBOL-X

From INTEGRAL to SIMBOL-X. F. Lebrun CEA-Saclay SAp/APC. INTEGRAL: a European gamma-ray observatory. IBIS – The gamma-ray Imager onboard the INTEGRAL satellite. Excellent Imaging, good spectra. Launch: October 2002. ISGRI – the IBIS low energy camera (CdTe).

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From INTEGRAL to SIMBOL-X

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  1. From INTEGRAL to SIMBOL-X F. Lebrun CEA-Saclay SAp/APC High Energy Astrophysics in the Next Decade

  2. INTEGRAL: a European gamma-ray observatory IBIS – The gamma-ray Imager onboard the INTEGRAL satellite. Excellent Imaging, good spectra Launch: October 2002 ISGRI – the IBIS low energy camera (CdTe) Perigee: 10,000 km, Apogee: 150,000 km SPI – The gamma-ray Spectrometer of INTEGRAL. Excellent spectra, good images Operations funded till end 2008 High Energy Astrophysics in the Next Decade

  3. GALACTIC DIFFUSE EMISSION 511 keV bulge ~ 8° (Knödlseder et al., 2005) 1043 e+/s ! Light dark matter ? Point sources > 85% (Lebrun et al., 2004, Strong et al., 2005, Bouchet et al., 2005) 26Al (Diehl et al., 2006) Positronium ~ 92% (Jean et al., 2005 Weidenspointner et al., 2006) 60Fe (Harris et al., 2005) High Energy Astrophysics in the Next Decade

  4. POINT SOURCES • More than 200 sources detected with ISGRI (Bird et al., 2005) • 55 sources are new and heavily absorbed (NH~ 1023 cm-2). • HMXB population doubled (mostly pulsar+supergiant companion) • IGR J17456-290:A steady non-thermal source near the GC • IGR J00291+5934:Fastest ms pulsar (P=1.67 ms), pulsed fraction increases with energy • 44Ti linesdetected in the Cas A spectrum • Magnetars: very hard spectrum High Energy Astrophysics in the Next Decade

  5. Conclusions about ISGRI/CdTe • No failure in 44 months of flight operations • Noisy detectors: only 3% • Performances • Sensitivity: milliCrab (3σ, tobs= 1 day, ΔE=E) • Actual lower threshold: 15 keV • Spectral performance is nominal • 9% at 60 keV • 5% at 511 keV • Spectral performance degradation: • ~ 2.6 % / year (factor 2 in 20 years) • 0.7 % after the November 2003 giant solar flare CdTe/CdZnTe is confirmed as the X/gamma-ray detector for tomorrow space astrophysics High Energy Astrophysics in the Next Decade

  6. CNES calls for proposals Selected for a phase A study (on-going) • Micro satellites:ECLAIRs devoted to GRB study launch: 2011 • Formation flight:SIMBOL-X Focusing hard X-rays launch: 2013 Final selection next year High Energy Astrophysics in the Next Decade

  7. ECLAIRs France-China SVOM payload Gamma-ray telescope X-ray telescope Optical telescope Multiwavelength study of Gamma-Ray Burst prompt emission High Energy Astrophysics in the Next Decade

  8. 52 cm 40 cm 38 cm ECLAIRS: The X and Gamma Camera (CXG) Wide field of view (~2 sr) coded mask telescope encircled by a graded shield collimator to reduce the cosmic diffuse induced background XRDPIX modules Useful area 1024 cm2 100 GRB/year Array of CdTe detectors Spectral band 4.0 to 250 keV Detection plane (DPIX) made of 200 XRDPIX modules developed in the framework of CNES/CESR and CNES/CEA R&D programs High Energy Astrophysics in the Next Decade

  9. Crab Nebula 300 3.5 keV 5h 200 Counts 100 20° 0 10 20 30 40 50 60 Energy (keV) 10 INTEGRAL GRB 030227 Sensitivity (ph cm-2 s-1) SWIFT ECLAIRs 1 10 100 1000 Peak energy (keV) CXG Anticipated Performances The position on the sky of all GRBs detected with a signal to noise ratio greater than 5.5 will be given with an accuracy ~10′ High Energy Astrophysics in the Next Decade

  10. 0.1–10 keV 15 keV-10 MeV SIMBOL-X 0.5 – 80 keV Focusing hard X-rays using formation flight technology High Energy Astrophysics in the Next Decade

  11. Participating laboratories F : CEA/Saclay, CESR/Toulouse, APC/Paris, LAOG/Grenoble, Obs.Paris/Meudon It : (INAF :) O.A.Brera, Roma, Palermo, IASF Milano, Bologna D : MPE Garching, I.A.A.Tübingen Short history • End ‘01 : First ideas & discussions CEA/Saclay & O.A.Brera • End ‘03 : CNES call for ideas for formation flight… • Mid ‘04 : Selection of 4 missions for an assessment phase • End ‘05 : Only Simbol-X is recommended for a phase A study High Energy Astrophysics in the Next Decade

  12. Simbol-X basics Have the XMM angular resolution and sensitivity in the INTEGRAL/ISGRI energy range Focusing optics Coded mask optics INTEGRAL > 15 keV XMM < 10 keV 30 degrees 30 arcmin High Energy Astrophysics in the Next Decade

  13. Major science goals Particle acceleration Mechanisms ? Maximum energy ? Accreting Black Holes Physics in single objects Census in Universe High Energy Astrophysics in the Next Decade

  14. Accreting Black Holes Census of Super Massive Black Holes About 50 % resolved in sources in the 7–10 keV band But less than a few % resolved beyond 10 keV, at the emission peak ! • Record of Super Massive Black Holes accretion activity • • Constraints to models for the formation and evolution of structures in the Universe CXB models : major contribution from obscured AGNs, but parametres are not constrained (evolution, energy cut-off, absorption) Need : resolve > 50 % of CXB in the [20-40] keV band -> sensitivity, angular resolution, field of view High Energy Astrophysics in the Next Decade

  15. Simbol-X : understand SgrA* and its environment Simbol-X 3 s, 1 hour INTEGRAL/IBIS/ISGRI Simbol–X, 300 ks, > 10 keV 10x10 arcmin2 XMM-Newton High Energy Astrophysics in the Next Decade

  16. Acceleration : link with HESS sources protons in SNRs shocks ? G347.3-0.5 - HESS @ TeV SX With Simbol-X : • mapping of the synchrotron emission, • determination of spectral break with X-ray alone • correlation with GeV and TeV emissions SN 1006 Simbol-X : E > 10 keV 100 ks 10’x15’ High Energy Astrophysics in the Next Decade

  17. Nucleosynthesis : measure 44Ti yield 10 arcmin Simbol–X 44Ti map Spectrum 1 arcmin2 100 ks Map Cas A emission Measure velocity Measure 1987A yield 44Ti : explosive nucleosynthesis product Period of 85 years Lines (44Sc) at 68 and 78 keV Detected only in CasA (so far), by BeppoSAX and INTEGRAL High Energy Astrophysics in the Next Decade

  18. And a lot more… • Quiescence : physical processes at low accretion rate, « ADAF », jets ? • Difference between accreting neutron stars and black holes ? • Follow and characterize the change of states on their evolutionary times • Local group population ? • Absolute luminosity, localisation • hard X-ray spectrum : population characterization, comparison with Milky Way • Intermediate Mass Black Holes: ULXs characterization, spectrum and QPOs ( BH mass measurement) • Cyclotron lines • Non thermal cluster emission • Young Stellar Objects • Gamma-ray bursts follow up High Energy Astrophysics in the Next Decade

  19. Simbol-X scientific requirements Energy band : ~ 0.5 to > 80 keV ΔE : < 150 eV @ 6 keV (Fe Ka) < 1.3 keV @ 68 keV (44Ti) Δq : < 20 arcsec HPD FOV : > 9 arcmin Attitude reconst. : ± 2 arcsec Δt : < 100 microsecondes Duration : 3 years Over 1000 targets possible Sensitivity [1 Ms, 3 ] : 10-8 ph/cm2/s/keV up to ~ 80 keV 10-14 erg/cm2/s [20-40 keV] (1 mCrab) • Large effective area, excellent angular resolution, very low background High Energy Astrophysics in the Next Decade

  20. Optics Grazing incidence : Emax  1/θ Focal Length • Heritage from XMM–Newton : nickel shells obtained by electroforming replication method; low mass obtained via a reduced thickness of shells • Coating : multi-layer Pt/C needed for requirement on large F.O.V. and on sensitivity up to > 80 keV Mirror parameters to be optimized in phase A Focal length :20 - 30 m Shell diameters :max 70 cm Shell thickness : 0.1 - 0.3 mm Number of shells : ~ 100 High Energy Astrophysics in the Next Decade

  21. The focal detector assembly Low energy detector (450 mm Silicon) (see L. Strüder talk on Friday) High energy detector (2 mm Cd(Zn)Te) Active anticoincidence shield Required parameters • Spectro-imaging system 0.5-100 keV • Pixel size ~ 500 mm (PSF oversampling) • Full size : 8x8 cm2, 128x128 pixels • “Room temperature” operations (~ -30°C) • Fast reading (used in anticoincidence) High Energy Astrophysics in the Next Decade

  22. Phase 0 result (CNES) : orbit pointing & stabilization ecliptic plane Sun sky area visible at any moment  35% 4,5 months 360° 20° Orbit constraints : - have formation flight feasible (> ~ 20,000 km) - minimize background (science > 75,000 km) orbital period correction Increase of perigee Transfer orbit High elliptical orbit : 44,000 - 256,000 km at launch Pointing : XMM / INTEGRAL type fixed solar panels simplified thermal control Formation flight requirements : ± 10 cm along telescope axis ± 1 cm perpendicular, knowldege @ ± 0.5 mm High Energy Astrophysics in the Next Decade

  23. Phase 0 study (CNES) : detector spacecraft Detection payload ISL antennas COLLIMATOR detection radiator and associated heat pipe fine SST towards -X lateral sensor ISL back antenna High Energy Astrophysics in the Next Decade

  24. Phase 0 study (CNES) : mirror spacecraft Wolter-I Mirror sun baffle ISL back antenna thermal baffle D=3m sky screen High Energy Astrophysics in the Next Decade

  25. Phase 0 study (CNES) : launch configuration Launched as a composite under Soyuz fairing Launcher capability : 2.2 tons (5 deg incl.) Masses Detector S/C : ~ 600 kg Mirror S/C : ~ 1300 kg Adapter : ~ 150 kg High Energy Astrophysics in the Next Decade

  26. Status - schedule • Simbol-X in phase A, conducted jointly by CNES & ASI, with the participation of MPE-IAAT • Other partners are possible • • End of phase A review : 2nd quarter 2007 • • Launch date : mid 2013 • Operations for three years (2 years of science observations) • Observation program will be composed of : - a “core program”, with main priority science targets - and a guest observer program open to the community High Energy Astrophysics in the Next Decade

  27. Detector/Electronics requirements • SIMBOL-X requirements: • Spatial resolution: 500 μ  small pixels • Spectral resolution: 1.3 keV @ 68 keV  small pixels • Energy range: 10 – 100 keV • ECLAIRS CXG requirements: • Spatial resolution: 4 mm • Energy range: 4 – 250 keV Front-end electronics : • - multi-channels ASIC / DC coupling • - Ultra low noise (< 40 e- RMS for stand alone chip) • - self triggered • - Multiple event capabilities • - Low power, radiation tolerant, … as usual ! High Energy Astrophysics in the Next Decade

  28. High Energy Detector Arrays of Cd(Zn)Te with integrated ASICs 256 pixels CZT array 6 mm thick (eV-Products) 256 pixels Schottky array 0.5 mm thick (ACRORAD) Tests of pixellated Cd(Zn)Te matrices ASICs development (IDeF-X Vx.x) Hybridization High Energy Astrophysics in the Next Decade

  29. « Flat » prototype / CZT + IDeF-X V1.0 High Energy Astrophysics in the Next Decade

  30. From ISGRI … 2001 to 2005 ISGRI : CdTe Pt/Pt : 4x4x2 mm3 / 120V / 0°C ECLAIRS IDeF-X V1.0: CdTe In/Pt 4x4x1 mm3 / 600V / 24°C R&T IDeF-X V1.0 : CdTe In/Pt 2x2x0.5 mm3 / 340V / 24°C 5.6 keV FWHM 2001 1.8 keV FWHM 2005 1.1 keV FWHM (0.9 keV right side) 2005 0.73 keV FWHM at 13.9 keV High Energy Astrophysics in the Next Decade

  31. Conclusions • Current Results: • New low noise electronics under development for high resolution spectro-imaging • 35 e- RMS achieved without detector • 66 e- RMS achieved with a detector (330V, RT, dark current < 10 pA) • « Flat » prototypes of 64 pixels 900µm, 1mm pitch used for evaluation and characterization of detector arrays • CZT, CdTe and CdTe Schottky • 0.5, 1 and 2 mm thick detectors are studied • 4 keV Low threshold value accessible with 4x4x1 Schottky detectors (600V / -20°C) for the ECLAIRs Mission • 1 keV FWHM at 60 keV accessible goal for SIMBOL-X mission (small pixels) • Current and next development steps : • New ASICs • Hybridization of ASICs and pixel arrays in progress • Space environment and Space qualification constraints studied simultaneously in the R&D program High Energy Astrophysics in the Next Decade

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