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EM counterparts of GW s : Observation Strategy of SVOM Mission

Learn about the observation strategy of SVOM Mission and its GW counterparts. This includes the status of the mission, proposed instruments, and multi-wavelength capabilities.

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EM counterparts of GW s : Observation Strategy of SVOM Mission

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  1. EM counterparts of GWs: Observation Strategy of SVOM Mission WEI Jianyan@SVOM Team NAOC, Beijing 7th Jan. 2019, Xiamen

  2. Outlines A short introduction about SVOM GW EM counterparts observation strategy

  3. Status of the SVOM mission 2001 SVOM proposed by Chinese side,Eclairs by French side 2006 Phase 0 kick-off meeting (March, Toulouse) Phase 0 review(Sept., Shanghai) CNSA/CNES MoUsigned during the President visit (Oct., Beijing) 2007 Phase A kick-off meeting (March, Xi’an) Phase A review meeting (Oct., Beijing) 2008 2010 SVOM funded by CNSA China 2014 SVOM funded by CNES France 2014 Phase B kick-off meeting (Sept., Shanghai) 2016 Phase B review meeting (July 4-8, Yantai) 2017 Phase C kick-off meeting, and SIR review 2021 SVOM launch at Xichang（西昌）, China

  4. 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

  5. ～13.8Byrs Evolution after the big bang Now 1 + z The first stars and the baby Universe 105 1010 109 108 107 106 Re-Iron. Big Bang Sun Dark Age last diffusion limit Pop III 3 10 30 100 300 1000 3000

  6. Proposed scientific instruments ECLAIRs, the X-ray and soft gamma-ray trigger camera 4-250KeV 2sr (~8000 Sq.deg) GRM, the gamma-ray spectro-photometer 15KeV-5MeV 60 Deg MXT, the micro-channel soft X-ray telescope 0.3-6KeV 65’65’ VT, the visible telescope 400-650nm, 650-950nm 26’26’ GWAC, an array of ground wide angle cameras 500-800nm ~ 5000 Sq.deg. C-GFT, the Chinese ground follow-up telescope 400-1700nm? 25’25’ F-GFT, the French ground follow-up telescope 400-1700nm 30’30’

  7. SVOM scientific instrument arrangement ( SVOM white paper)

  8. ECLAIRs: the trigger camera Main characteristics Coded mask telescope Wide FOV : 2 Sr 6400 CdTe - 1024 cm2 4 keV – 150 keV Anticipated performances Loc. accuracy < 10arcmin 3 arcmin for bright burst 70 GRBs / year

  9. GRM – The Gamma Ray Monitor Main characteristics NaI detectors FOV : 60 Deg. 10 keV – 5 MeV Anticipated performances Loc. accuracy ~ 2° 100 GRBs / year

  10. MXT – The Multi-channel X-ray Telescope Main characteristics MCP X-ray optic FOV ~ 1 deg2 256 x256 PN CCD 0.3 keV – 6 keV Anticipated performances Loc. accuracy < 1 arcmin 20 arcsec for bright GRB 5x10-12 erg cm-2 s-1 in 1000s

  11. VT – The Visible Telescope Main characteristics Ritchey Chretien Ф=40cm FOV : 26 x 26 arcmin2 2 X 2048x2048 CCD 400 - 650 / 650 - 950 nm Anticipated performances Loc. accuracy ~1 arcsec Mv = 22.5 in 300s

  12. Parameters of the GWAC at China Prompt optical emission detection down to MV ~ 16.0 (10 s exposure) • Cameras： 40 • Diameter： 180mm • Focal Length： 220mm • Wavelength： 500－800nm • Total FoV： ~6000Sq.deg • Limiting Mag： 16.0V（5，10sec） • Self Trigger: ~13*5sec

  13. Space instruments performances

  14. 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

  15. Prompt dissemination of the GRB parameters VHF Network

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

  17. SVOM repartition: useful observing time

  18. 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 SVOM: also a powerful multi-band observatory for transcients! GWs will be followed within 12 hours.

  19. The strategy for SVOM to observe GW bursts 2015 2019 2022 Error box: ~600 Sq.Deg ~<10 Sq.Deg. GRM Eclairs MXT VT GWAC

  20. GW 170817 / GRB 170817A  Would this GRB Have been detected by SVOM? ECLAIRs • Up to 35°: ECLAIRs detects and localizes the GRB • ECLAIRs sends an and a slew reques • to the satellite •  Up to 50°: GRM sends an alert (coarse location) SVOM JSC – December 6th - Paris GRM

  21. GW 170817 / GRB 170817A ToO-MM The associated kilonova would have been easily detected by the VT and the GFTs From T0 + 2 hours and for 10 days SVOM JSC – December 6th - Paris

  22. Status: GWAC • 2013-2016: Mini-GWAC for developing Pipelines V1.0; • 2014-2015: two 60cm, one 30cm telescopes from GXU and . • 2015-2016: the first 18-GWAC system (10 telescopes from NJU); • 2017-2018: the 16-GWAC in testing; 22-GWAC waiting for check

  23. An example：2015年12月18日发现---耀星

  24. GRB （Wang et al. 2013） Flare star （Mini-GWAC 2015） ----------------------------------- -------------------------- GWAC 600秒 T-T0=30 sec T0

  25. 2.16-M follow a flare star：2015年12月18日发现的耀星

  26. So far more than ~60 flare stars were triggeredby GWAC/Mini-GWAC

  27. SVOM Follow-up testing system 2017 -2018 SVOM Mini-GWAC，GWACs, F-60A,B CFHT Obs. time SVOM Scheduler Database Server Scientific expertise Xinglong 2.16M Lijiang 2.4M

  28. 7 GWs followed during O2

  29. O1: • GW151226 O2: • GW170104 • 6 other events • 10 GCN circulars (其中2个使用2.16m 和2.4m )

  30. SVOM Follow-up testing system 2019 -2020: O3 SVOM GWACs, C-GFT CFHT Obs. time GRANDMA Lite Database Server of pointings OT sc. products SVOM Pointinggenerator Database Xinglong 2M ZADKO TAROT LCOGT Lijiang 2.4M SVOM testing system Follow the strategy of SVOM 2017-2018 Smoothly evolve to SVOM 2021

  31. 2021 SVOM Follow-up System SVOM ECLAIRs, VT,MXT,GRM GWACs, C-GFT, F-GFT Scientific expertise SVOM Scheduler Database Server Voluntaried Facilities Guaranted time Time to buy Time to Apply TAROT LCOGT 1m LCOGT 2m CFHT XXX Obs Lijiang 2.4M UKIRT VLT XXX Obs XXX Obs XXX Obs XXX Obs Organization of the SVOM Follow-up system, operational in 2021? and based on the attractiveness of SVOM The exchanges between SVOM and its various partners are (will be) defined in the updated SVOM Science Management Plan

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