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High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Space Station

High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Space Station. Shuang-Nan Zhang ( 张双南 ) zhangsn@ihep.ac.cn Center for Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences. HERD: H igh E nergy cosmic- R adiation D etector.

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High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Space Station

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  1. High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Space Station Shuang-Nan Zhang (张双南) zhangsn@ihep.ac.cn Center for Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences

  2. HERD: High Energycosmic-Radiation Detector Secondary science: γ-ray astronomy  monitoring of GRBs, microquasars, Blazars and other transients  down to 100 MeV for γ -rays  plastic scintillator shields for γ -ray selection *complementary to high altitude cosmic-ray observations

  3. HERD Cosmic Ray Capability Requirement P (<A>~ 1) He (<A>~ 4) L (<A>~ 8) M (<A>~ 14) H (<A>~ 25) VH (<A>~ 35) Fe (<A>~ 56) Model 2 Heavy Model Model 1 Light model PeV PeV Except for L, up to PeV spectra feasible with GF~2-3 in ~years: discriminate between models. Detection limit: N = 10 events PeV PeV N(E>E0; 2 yr) HERD HERD TeV TeV

  4. Characteristics of all components

  5. Expected performance of HERD Acceptance & H-energy > n10X all others

  6. Other detectors: Top down  “small” FoV DAMPE 2015 ISS-AMS: 2011 ISS-CALET: 2015 ISS-CREAM: 2017?

  7. HERD Design：3D Calo & 5-Side Sensitive n10X acceptance than others, but weight 2.3 T ~1/3 AMS STK(W+SSD) Charge gamma-ray direction CR back scatter 3D CALO e/G/CR energy e/p discrimination STK(W+SSD)

  8. Simulation results: energy resolutions Protons Electrons Electron < 1%; Proton: ~20% Essential for spectral features!

  9. Energy Resolution for gamma-rays 500 MeV-100 GeV result

  10. HERD Eff. Geometrical Factor: CALO All five sides All five sides

  11. Expected HERD Proton and He Spectra Horandelmodel as HERD input Only statistical error Protons He

  12. Expected HERD Spectra of C and Fe C Fe

  13. Gamma-ray Sky Survey Sensitivity Narrow FoV

  14. HERD sensitivity to gamma-ray line HERD 1 yr PAMELA: 2006-2016 CALET: 2015-2020; AMS: 2011-2021; DAMPE: 2015-2020; Fermi:2008-2018; HERD: 2020-2021

  15. DM annihilation line of HERD

  16. Sensitivity of Dark Matter Search in MW 90 41 180 16

  17. 95% upper limits on photon fluxes ~ energy Five year sky survey

  18. Comparison of DM sensitivity from γ-line HERD R16

  19. 95% upper limits on decay lifetime of DM

  20. Comparison with DM models γγ γZ

  21. CALO readout Trigger Optical Coupling Fast Frame CCD Image Intensifier

  22. Proof of principle 2×2×6 CsI crystal array ICCD image of cosmic ray events

  23. HERD progress – ICCD development

  24. Scintillator signal readouts • LYSO scintillator  WLSF • Fiber to ICCDsystem Optical fiber winding Crystal packing Image intensifier ICCDsystem Taper

  25. Fiber Image on CCD Signal: 3000 pe; gain of image intensifier: 4000

  26. Fiber Image on CCD Signal: 3000 pe; gain of image intensifier: 50000

  27. CERN Beam Test in Nov 10-20, 2015

  28. Requirements on the prototype • Requirement on dynamic range: ~6000 • Starting from 1/3 MIPs=10 MeV • Ending at max. energy deposition: 60 GeV • Requirement on frame rate of ICCD: > 500 fps • Since the electrons arrive randomly in time

  29. Requirements on the prototype • Scale of the prototype：5×5×10, 3×3×3 cm3 • Larger than envelope of 280 GeV e- shower • 36% of the total energy for protons Along the beam 1/40 size of HERD Transverse direction

  30. LYSO light output for 3cm×3cm×3cm cubic LYSO, but signal << 30 MeV MIP

  31. LYSO performance Variation of LYSO light output: (Max-Min)/Mean ≈25% Energy resolution (σ/E) for 662keV γ peak: < 5%

  32. Realization of two readout ranges H Low T Low H T

  33. Signal ratios ~ 50:1

  34. Fiber winding development Fiber insert hole Slot instead of hole

  35. Fiber winding development

  36. Fiber winding development

  37. Fiber winding development

  38. Fiber winding development

  39. Making ESR wrapping

  40. Assembly and lab test of the prototype

  41. @CERN: beam test starts on Nov. 10, 2015 Packing @ IHEP Oct 28 @ CERN Final test @ IHEP

  42. HERD beam test @ SPS H4 • Purposes • To verify the WLSF+ICCD design • To verify the design specifications of energy resolution, angular resolution (by only CALO), and particle discrimination. • Requirements • Large dynamic range, ~ 6000 • Frame rate, > 300 fps • 1 LYSO array • 5*5*10 crystals • 2 ICCD systems • 2 PMT systems • Envelope • 560*580*240 mm3

  43. Beam runs & counts • Triggered events • ~5 M events during e & p runs • ~1 M events during Pb runs till this morning

  44. Beam - calibration Stable hadron beam!

  45. 250 GeV electron shower CCD camera 3D shower

  46. 20 GeV electron shower CCD camera 3D shower

  47. Preliminary result – PMT readout PMT spectrum @ 100 GeV

  48. Preliminary result – ICCD low range readout Sigma ~ 5%@10 GeV without correction

  49. 1st HERD workshop, Oct.17-18, 2012, IHEP, Beijing

  50. 2nd HERD Workshop @IHEP 2013/12/2-3

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