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 1/51

2. Science goalsMission requirements Dark matter search R1: Better statistical measurements of e/γ between 100 GeV to 10 TeV Origin of Galactic Cosmic rays R2: Better spectral and composition measurements of CRs between 300 GeV to PeV* with a large geometrical factor HERD: High Energy cosmic-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 2/51

3. HERD Cosmic Ray Capability Requirement P ( ~ 1) He ( ~ 4) L ( ~ 8) M ( ~ 14) H ( ~ 25) VH ( ~ 35) Fe ( ~ 56) Except for L, up to PeV spectra feasible with GF~2-3 in ~years: discriminate between models. N(E>E0; 2 yr) PeV Model 1 Light model Model 2 Heavy Model TeV PeV HERD Detection limit: N = 10 events 3/51

4. Characteristics of all components typesizeX0,λunitmain functions tracker (top) Si strips 70 cm × 70 cm 2 X07 x-y (W foils) Charge Early shower Tracks tracker 4 sides Si strips 65 cm × 50 cm 2 X07 x-y (W foils) Charge Early shower Tracks CALO~10K LYSO cubes 63 cm × 63 cm 55 X0 3 λ 3 cm × 3 cm e/γ energy nucleon energy e/p separation 4/51

5. Expected performance of HERD γ/e energy range (CALO)tens of GeV-10TeV nucleon energy range (CALO)up to PeV γ/e angular resol.0.1 o nucleon charge resol.0.1-0.15 c.u γ/e energy resolution (CALO)<1%@200GeV proton energy resolution (CALO)20% e/p separation power (CALO)<10 -5 electron eff. geometrical factor (CALO)3.7 m 2 sr@600 GeV proton eff. geometrical factor (CALO)2.6 m 2 sr@400 TeV Acceptance & H-energy > n10X all others 5/51

6. Other detectors: Top down  “small” FoV ISS-CREAM: 2017? ISS-CALET: 2015 ISS-AMS: 2011 DAMPE 2015 6/51

7. HERD Design ： 3D Calo & 5-Side Sensitive n10X acceptance than others, but weight 2.3 T ~1/3 AMS 3D CALO e/G/CR energy e/p discrimination STK(W+SSD) Charge gamma-ray direction CR back scatter 7/51

8. Simulation results: energy resolutions Electron < 1%; Proton: ~20% Essential for spectral features! Electrons Protons 8/51

9. Energy Resolution for gamma-rays 500 MeV-100 GeV result 9/51

10. HERD Eff. Geometrical Factor: CALO All five sides 10/51

11. Expected HERD Proton and He Spectra Horandel model as HERD input Only statistical error Protons He 11/51

12. Expected HERD Spectra of C and Fe C Fe 12/51

13. Gamma-ray Sky Survey Sensitivity Narrow FoV 13/51

14. PAMELA: 2006-2016 CALET: 2015-2020; AMS: 2011-2021; DAMPE: 2015-2020; Fermi: 2008-2018; HERD: 2020-2021 HERD sensitivity to gamma-ray line HERD 1 yr 14/51

15. DM annihilation line of HERD 15/51

16. Sensitivity of Dark Matter Search in MW 16 41 90 180 16/51

17. 95% upper limits on photon fluxes ~ energy Five year sky survey 17/51

18. Comparison of DM sensitivity from γ-line HERD R16 18/51

19. 95% upper limits on decay lifetime of DM 19/51

20. Comparison with DM models γγγZγZ 20/51

21. CALO readout Trigger Fast Frame CCD Optical Coupling Image Intensifier 21/51

22. Proof of principle 2×2×6 CsI crystal array ICCD image of cosmic ray events 22/51

23. HERD progress – ICCD development 23/51

24. Scintillator signal readouts LYSO scintillator  WLSF Fiber to ICCD system Image intensifier Taper ICCD system Optical fiber windingCrystal packing 24/51

25. Fiber Image on CCD Signal: 3000 pe; gain of image intensifier: 4000 25/51

26. Fiber Image on CCD Signal: 3000 pe; gain of image intensifier: 50000 26/51

27. CERN Beam Test in Nov 10-20, 2015 27/51

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 28/51

29. Requirements on the prototype Scale of the prototype ： 5×5×10, 3×3×3 cm 3 –Larger than envelope of 280 GeV e- shower –36% of the total energy for protons 1/40 size of HERD Along the beam Transverse direction 29/51

30. LYSO light output for 3cm×3cm×3cm cubic LYSO, but signal << 30 MeV MIP 30/51

31. LYSO performance Variation of LYSO light output: (Max-Min)/Mean ≈25% Energy resolution (σ/E) for 662keV γ peak: < 5% 31/51

32. Realization of two readout ranges T H Lo w H T 32/51

33. Signal ratios ~ 50:1 33/51

34. Fiber winding development Slot instead of hole Fiber insert hole 34/51

35. Fiber winding development 35/51

36. Fiber winding development 36/51

37. Fiber winding development 37/51

38. Fiber winding development 38/51

39. Making ESR wrapping 39/51

40. Assembly and lab test of the prototype 40/51

41. @CERN: beam test starts on Nov. 10, 2015 Final test @ IHEP Packing @ IHEP Oct 28 @ CERN 41/51

42. HERD beam test @ SPS H4 1 LYSO array –5*5*10 crystals 2 ICCD systems 2 PMT systems Envelope –560*580*240 mm 3 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 42/51

43. Beam runs & counts Triggered events –~5 M events during e & p runs –~1 M events during Pb runs till this morning TimeBeam Particle Start Time 2015/Nov/ (D/h:m) Stop Time 2015/Nov/ (D/h:m) TypeP (GeV/c) 13/00:3813/04:23pion+50 13/04:4613/09:02e-200 13/09:0213/12:41beam tuning by CCC 13/12:4113/18:40proton400 13/18:4213/20:00pion+50 13/20:0013/23:30no beam 13/23:3914/02:23pion+50 14/02:5014/09:15proton350 14/09:2314/21:43e-150, 100, 50, 40, 10 14/23:1615/03:05pion+50 15/03:1715/13:16e-30,20, 10, 250 15/13:5815/15:27e+100 15/15:2715/16:40no beam 15/16:4315/21:00e-100, 50 15/21:1115/22:10e+50 15/22:3015/23:20e-80GeV 15/23:3016/3:38pion+50 16/03:3816/5:30proton350 16/05:3016/6:00e-200 43/51

44. Beam - calibration Stable hadron beam! 44/51

45. 250 GeV electron shower CCD camera 3D shower 45/51

46. 20 GeV electron shower CCD camera 3D shower 46/51

47. Preliminary result – PMT readout PMT spectrum @ 100 GeV 47/51

48. Preliminary result – ICCD low range readout Sigma ~ 5%@10 GeV without correction 48/51

49. 1st HERD workshop, Oct.17-18, 2012, IHEP, Beijing 49/51

50. 2 nd HERD Workshop @IHEP 2013/12/2-3 50/51

51. The HERD Proto-Collaboration Team Chinese institutions (more welcome!) –Institute of High Energy Physics, Purple Mountain Observatory, Xi’an Institute of Optical and Precision Mechanics, University of Science and Technology of China, Nanjing University, Peking University, Yunnan University, China University of Geosciences, Ningbo University, Guangxi University International institutions (more welcome!) –Switzerland: University of Geneva –Italy: Università di Pisa/INFN, IAPS/INAF, University of Florence/INFN, University of Perugia/INFN, University of Trento/INFN, University of Bari/INFN, University of Salento/INFN-Lecce –Sweden: KTH –USA: MIT/Harvard 51/51