High Energy cosmic-Radiation Detection (HERD) Facility onboard Chinas Space Station Shuang-Nan Zhang(张双南) Zhangs@ihep. accn Center for Particle Astrophysics 粒子天体物理中心 Institute of High Energy physics Chinese Academy of Sciences 1/42
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 粒子天体物理中心 Institute of High Energy Physics Chinese Academy of Sciences 1/42
Astroparticle Physics Particle Astrophysics Physics Astronomy Particle Physics Astrophysics Astroparticle Physics Particle Astrophysics ool: Universe Tool: Particle Physics Goal: Particle Physics Goal: Universe The Physical Universe and its Laws 142
Astroparticle Physics & Particle Astrophysics Physics Particle Physics Astroparticle Physics Particle Astrophysics Astronomy Astrophysics Tool: Universe Goal: Particle Physics Tool: Particle Physics Goal: Universe The Physical Universe and Its Laws 2/42
Tibet High Altitude Cosmic-ray Observatory Sea level and YBJ—ASy,ARGo Space Projects Underground Exp. LHAASO AMS CE. HXMT CMS, Daya-Bay POLAR DAMPE SVOM Dark matter search SEMS. XTP HERD 150 students HEP Center 180 fulltime staff postdocs and for Particle scientists and visiting scholars Astrophysics engineers High Energy Cosmic-ray Gravity Cosmology Charged Particles, Compact Objects Neutrinos, Gamma-rays Galaxy, Cluster Explosive Phenomena CMB GRB SN&SNR Bh&NS accretion 2
IHEP Center for Particle Astrophysics High Energy Cosmic-ray Charged Particles, Neutrinos, Gamma-rays Explosive Phenomena GRB,SN&SNR BH&NS accretion Sea Level and Underground Exp. CMS, Daya-Bay Dark Matter Search Gravity & Cosmology Compact Objects Galaxy, Cluster CMB Space Projects AMS, CE, HXMT POLAR, DAMPE, SVOM SEMS, XTP, HERD Tibet High Altitude Cosmic-ray Observatory YBJ－AS, ARGO LHAASO 180 fulltime staff scientists and engineers 150 students, postdocs and visiting scholars 3/42
HERD: High Energy cosmic-Radiation Detector Science goals Mission requirements Dark matter R1: Better statistical measurements search of e/y between 100 GeV to 10 TeV Origin of R2: Better spectral and composition Galactic measurements of crs between Cosmic rays 300 Gev to Pev* with a large geometrical factor Secondary science: Y-ray astronomy> monitoring of grbs microquasars, blazars and other transients> down to 100 Mev for y-rays> plastic scintillator shields for y-ray selection *complementary to high altitude cosmic-ray observations 2
Science goals Mission 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 4/42
HERD Cosmic Ray Capability Requirement P(~1) a.gi3 He(~4) L(~8) M(~14) Model 1 d Model 2 H(~25) 10 Light model Heavy Model ⅦH(~35) Pe∨ Fe(~56) 10 fev Detection limit: N= 10 events I PeV EXcept for L, up -h to PeV spectra w feasible with M 0.36m'Sr PeV Fe GF-2-3 in NouAu years 3sr discriminate HERD HERD between models TeV t03 eV 2
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 PeV Model 1 Light model Model 2 Heavy Model TeV TeV PeV PeV HERD HERD Detection limit: N = 10 events 5/42
Characteristics of all components itype size X0, A unit main functions tracker Si70cm×2×07 X-y Charge (top) strips 70 cm (W foils)Early shower Tracks tracker Si 65 cm X 2 X0 7 X-y Charge 4 sides strips 50 cm (W foils)Early shower Tracks CALO 10K63cm×553cm× e/y energy LYSO63cm×X0 3cm× nucleon energy cubes 63 cm 3 a 3 cm e/p separation 42
Characteristics of all components type size X0,λ unit main functions tracker (top) Si strips 70 cm × 70 cm 2 X0 7 x-y (W foils) Charge Early shower Tracks tracker 4 sides Si strips 65 cm × 50 cm 2 X0 7 x-y (W foils) Charge Early shower Tracks CALO ~10K LYSO cubes 63 cm × 63 cm × 63 cm 55 X0 3 λ 3 cm × 3 cm × 3 cm e/γ energy nucleon energy e/p separation 6/42
Expected performance of HERD y/e energy range(CALO) tens of Gev-10TeV nucleon energy range(CALO) up to PeV ye angular resol 0. nucleon charge resol 0.10.15cu yle energy resolution(CALO) n10X all others 7142
Expected performance of HERD γ/e energy range (CALO) tens of GeV-10TeV nucleon energy range (CALO) up to PeV γ/e angular resol. 0.1o nucleon charge resol. 0.1-0.15 c.u γ/e energy resolution (CALO) n10X all others 7/42
Other detectors: Top down÷“ small"Fo∨ Plastic Scintillator Detector Silicon- Tungsten Tracke BGO Calorimeter 64P DAMPE 2015 Neutron Detector ISS-AMS W converter thick calorimeter (total 33 X) precise tracking charge measurement 2011 high energy y-ray, electron and CR telescope TCD ISS-CALET: 2015 Event inside TCD-CAL acceptance SCD. CAL ISS-CREAM 2017? 3E8 arbon targe S3 hodoscope BASE PANEL 2
Other detectors: Top down → “small” FoV ISS-CREAM: 2017? ISS-CALET: 2015 ISS-AMS: 2011 DAMPE 2015 8/42
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 STK(W+SSD) e/G/CR energy e/p discrimination 42
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) STK(W+SSD) Charge gamma-ray direction CR back scatter 9/42
Simulation results: energy resolutions 25 09 ·Npe.:10/MP 24 08 23 0.7 edep Protons 0.6 2 05 20 04 Electrons 19 0.3 18 0.2 17 0.1 16 15 2004006008001000 Eo(Gev 10 Proton Energy (TeV) Electron 1%: Proton -20% Essential for spectral features 42
Simulation results: energy resolutions Electron < 1%; Proton: ~20% Essential for spectral features! Electrons Protons 10/42