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S pace Multi-band V ariable O bjects M onitor -----A Chinese-French Mission for GRBs

S pace Multi-band V ariable O bjects M onitor -----A Chinese-French Mission for GRBs. WEI Jianyan NAOC, Beijing Jacques PAUL IRFU-SAp, Saclay and APC, Paris ZHANG Shuangnan IHEP, Beijing Stephane BASA LAM, Marseille

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S pace Multi-band V ariable O bjects M onitor -----A Chinese-French Mission for GRBs

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  1. Space Multi-bandVariableObjectsMonitor -----A Chinese-French Mission for GRBs WEI Jianyan NAOC, Beijing Jacques PAUL IRFU-SAp, Saclay and APC, Paris ZHANG Shuangnan IHEP, Beijing Stephane BASA LAM, Marseille On behalf of the joint SVOM team Liverpool, June 18, 2012

  2. GRB phenomenon GRB phenomenon Diversity and unity of GRBs Diversity and unity of GRBs GRB physics GRB physics Acceleration and nature of the relativistic jet Acceleration and nature of the relativistic jet Radiation processes Radiation processes The early afterglow and the reverse shock The early afterglow and the reverse shock GRB progenitors GRB progenitors The GRB-supernova connection The GRB-supernova connection Short GRB progenitors Short GRB progenitors Cosmology Cosmology Cosmological lighthouses (absorption systems) Cosmological lighthouses (absorption systems) Host galaxies Host galaxies Tracing star formation Tracing star formation Re-ionization of the universe Re-ionization of the universe Cosmological parameters Cosmological parameters Fundamental Fundamental Origin of high-energy cosmic rays Origin of high-energy cosmic rays physics physics Probing Lorentz invariance Probing Lorentz invariance Short GRBs and gravitational waves Short GRBs and gravitational waves Scientific rationale of a new GRB mission

  3. Scientific requirements on SVOM Permit the detection of all know types of GRBs (>200), with a special care on high-z GRBs and low-z sub-luminous GRBs Provide fast, reliable and accurate GRB positions Measure the broadband spectral shape of the prompt emission (from visible to MeV) Measure the temporal properties of the prompt emission Quickly identify the afterglows of detected GRBs, including those that are highly redshifted (z>6) Quickly provide (sub-) arcsec positions of detected afterglows Quickly provide redshift indicators of detected GRBs

  4. Proposed scientific instruments ECLAIRs, the X-ray and soft gamma-ray trigger camera 4-250KeV 2sr (90*90 deg) GRM, the gamma-ray spectro-photometer 50KeV-5MeV 2sr MXT, the micro-channel soft X-ray telescope 0.3-5KeV 65’65’ VT, the visible telescope 400-650nm, 650-950nm 26’26’ GWAC, an array of ground wide angle cameras 450-900nm 2sr C-GFT, the Chinese ground follow-up telescope 400-1000nm? 25’25’ F-GFT, the French ground follow-up telescope 400-1700nm 30’30’

  5. GRM VT GWAC GFTs MXT ECLAIRS

  6. Eclairs: the trigger 2-D coded mask (30% transparency) Passive shield to block X-ray background 200 modules of 32 CdTe detectors (4 mm × 4 mm) Useful area: 1024 cm2 Field of view: 2 sr Spectral domain: 4 keV to 300 keV

  7. 300 3.5 keV 200 Counts 100 0 10 20 30 40 50 60 Energy (keV) ECLAIRs: the trigger camera Main design objective A low energy threshold in the X-ray domain Simulated sensitivity ECLAIRs expected to be more sensitive than SWIFT (BAT) for GRBs whose peak energy is < 20 keV

  8. 100 SWIFT (bright) SWIFT 80 ECLAIRs 60 Fraction > z (%) 40 DATA (SWIFT) 20 0 0 2 4 6 8 10 Redshift z ECLAIRs – Anticipated performances Simulated redshift distribution of long GRBs to be detected by ECLAIRs Nearly 10-20% of ECLAIRs GRBs could be situated at high redshift (z > 6)

  9. 2 modules GRM: the Gamma-Ray Monitor Scintillation (phoswich) detector NaI (10 mm thick) + CsI (40 mm thick) FoV： 2 sr Useful area： 280 cm2 per module Spectral Domain：50 keV to 5 MeV Measurement ofEpeak（up to ~ 500 keV）

  10. ECLAIRs + GRM: Epeak ~ 10-500keV

  11. MXT: to provide the accurate positioning Micro-Channel optics CCD camera passively cooled Field of view: 65 arc min× 65 arc min Spectral domain: 0.3 keV to 5 keV Useful area: 52 cm2 at 1 keV Detected GRBs to be localized with an error ~ 30 arc sec

  12. Sensitivity: Comparison with Swift/XRT MXT can detect ~90% of the afterglows

  13. VT：the Visible Telescope Modified R-C optical design Aperture size :450 mm Focal length：3600mm Field of View： 26 arc min × 26 arc min Bands：400-650 nm &650-950 nm Afterglow emission detection down to MV ~ 23 (300 s exposure)

  14. 1.0 0.8 0.6 Cumulative probability 0.4 0.2 0.0 12 14 24 16 18 20 22 Magnitude at 1000 seconds VT: the visible telescope VT-SVOM UVOT-SWIFT Akerlof & Swan, ApJ 671, 1868, 2007 The intrinsic cumulative GRB apparent optical afterglow distribution To detect ~ 80% of the observed GRBs

  15. Space instruments performances

  16. Parameters of GWAC • Cameras： 72 • Diameter： 180mm • Focal Length： 213mm • Wavelength： 450－900nm • Total FoV： 9000Sq.deg • Limiting Mag： 16.5V（5，10sec） Prompt optical emission detection down to MV ~ 16.5 (10 s exposure)

  17. Combined optical light curve Kann et al 2010 GWAC GFT T-t0=30 sec VT

  18. Sun Night side Sun Night side Sun Night side Pointing strategy: anti solar SVOM orbit (i ~ 30°) About 75% of the GRBs detected by SVOM to be well above the horizon of large ground based telescopes all located at tropical latitudes

  19. Prompt dissemination of the GRB parameters VHF Network

  20. T0 + 5 min VT (V & R band photometry) MXT (Soft X-ray photometry) T0 +1 min GWAC GFTs(g, r, i, J, H) 1-2 m robotic telescopes Multi messenger follow-up GRB observation strategy Space GRB trigger provided by ECLAIRs at time T0 Ground

  21. 1022 Space GRM 1020 ECLAIRs MXT Frequency (Hz) 1018 1016 VT Slew 1014 Ground 1015 GWAC C-GFT Frequency (Hz) F-GFT 1014 -5 0 1 10 102 103 104 105 Time (s) Log. scale Time (m) Lin. scale Multi-wavelength capabilities of SVOM

  22. SVOM compared with Swift • Prompt emission measurement • More sensitive below 20keV (to 4keV) • Better Epeak measurement capability • Prompt optical emission • Afterglow emission measurement • 10 times more sensitive in the visible, additional 650-950 nm band • Ground follow-up observation • Two dedicated 1meter telescopes with NIR dectector • GRBs more easily scrutinized by the largest telescopes

  23. Hunting for high-z GRBs • SVOM is going to provide redshift indicators to GCN • Eclairs + GRM: pseudo redshift • VT: redshift indicator: z<4.2, 4<z<6.0, z>6.0 or “dark” • GFTs: photometric redshift • Ground near Infrared telescopes are encouraged to point promptly to the GRBs which are detected by MXT in X-ray, but not by VT ! (~10 per year)

  24. Status of the SVOM mission 2005 Sino-French discussions (CNES-CNSA) on a mini satellite mission Scientific discussions on theSVOM mission for GRB studies 2006 SVOM Phase 0 kick-off meeting (March, Toulouse) SVOM phase 0 review(Sept., Shanghai) – No critical issue CNSA/CNES MoU signed during the President visit (Oct., Beijing) 2007 SVOM Phase A kick-off meeting (March, Xi’an) SVOM mission approved by CNES SPC(April, Paris) 2008 SVOM Phase A review meeting (Oct., Beijing) 2009 SVOM proved by CNES France 2010 SVOM funded by CNSA China 2016 SVOM launch at Kulu, the only mission to deliver GRB localization (?)

  25. 谢 谢！

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