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A Large High Altitude Air Shower Observatory LHAASO Project

A Large High Altitude Air Shower Observatory LHAASO Project. Zhen Cao Institute of High Energy Physics, China, Beijing 100049 TeVPA, SLAC ,2009. Yangbajing Valley in Tibet. YBJ, Tibet 4300m a.s.l. Outline. Scientific Perspectives Tentative design of a detector array Performance

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A Large High Altitude Air Shower Observatory LHAASO Project

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  1. A Large High Altitude Air Shower Observatory LHAASO Project Zhen Cao Institute of High Energy Physics, China, Beijing 100049 TeVPA, SLAC,2009

  2. Yangbajing Valley in Tibet

  3. YBJ, Tibet 4300m a.s.l.

  4. Outline • Scientific Perspectives • Tentative design of a detector array • Performance • Prototyping • Conclusion

  5. Leptonic model ？ Hadronic model Scientific Problems and Possible Solutions • TeVγray observation has an opportunity of finding CR origin: 80+ sources discovered • 50+ galactic sources: γat high energy (>30TeV) is crucial (high sensitivity and high energy resolution) • All-sky survey forγsource population is necessary (full duty cycle, wide FOV and sufficient sensitivity) • PeV CR spectra of individual composition • Bridge between space/balloon borne measurements and ground based UHECR measurements • Searching for Dark Matter galactic sub-structures

  6. A Tentative Design of A Complex Detector Array Three major components • 1km2 complex array forγrays and CRs >30TeV • 1 km2scintillation detector array • 40k m2μdetector array • 28 C-telescopes • 1k m2 burst detector • 90k m2 water Cerenkov detector for γ>100GeV • Two MagicII telescopes

  7. Charge Particle Array μdetector Array Water C Array Wide FOV C-Telescope Array & Core Detector Array LHAASO Project: γastronomy and origin of CR Large High Altitude Air Shower Observatory

  8. Contribution of Magic Coll.

  9. Water Cherenkov Detector

  10. μdetector

  11. 1.2m 250mm 250mm 1m 20mm Ground Charge Particle Detector Thick Iron Case 2.3cm scintillatorPMTWS fiber

  12. Wide FOVCherenkovtelescopes

  13. YAC detector Pb(7r.l.) Fe(1cm) Plastic　scinti. Shower Core Detector

  14. Cost Free high energy (1EeV)extension Re-Configuration Tower CT: 16 μ : 100x400m2 Side Trigger CT: 2x4

  15. Performance • 1km2 array for γdetection >50TeV • MagicII @ Tibet site • WCDA for source survey • CR (30TeV ~ 1EeV): both knees & absolute energy scale

  16. ？ Forγastronomy ARGO

  17. Proton Iron For Proton and Helium: • 1.5 m spacing • Nb>100 , any 5 (> 30 GeV) For Iron: • 3.75m spacing • Nb>100 , any 21 ( > 30 GeV) Resolution for light and heavy compositionμ-content, Xmax and HE (>30TeV) shower particles

  18. The keys are to lower threshold, making connections with direct measurements & measure spectra up to 100PeV

  19. A bridge between balloon measurements and ground base UHECR experimentcovering both “knees” with absolute energy scale

  20. Dark Matter g-rays from the sub-halos ARGOsensitivity LHAASO sensitivity Reed et al, MNRAS357,82(2004) source y g-rays from smooth bkg sun GC

  21. Prototyping • R/D budget: ~$1M • Detector unit prototype @ IHEP

  22. ARGO Hall On Site Prototype Exp. • 1% of the final configuration of LHAASO

  23. 预先研究进展 • 1%规模实验计划

  24. CR Energy Spectrum (160k events) resolution < 10% With bias<3% Core resolution <1m From S. P. SWORDY, Space Science Reviews 99: 85–94, 2001.

  25. Conclusion • a ground based large and complexγ/CR observatory at high altitude (4300m a.s.l.) within 5~10 years • Complementary to CTA in γastronomy • Unique for CR measurements at Knees • Perhaps useful for DM detection

  26. Perspectives on γAstronomy • Survey the whole sky for γsources above 100GeV (>90% of area is never surveyed at a sensitivity of 0.03ICrab) • Investigate detailed energy spectra for galactic sources above 30TeV, cosmic ray sources are expected to be identified • Detailed morphologic investigation of discovered sources for acceleration mechanism. (>30GeV)

  27. Domestic Collaboration(13 inst.) • ARGO collaboration: • APC of IHEP (detector design, project organization) • Tibet Univ. （FPM） • SW Jiaotong Univ.（FPM: construction at high altitude) • Yunnan Univ. (PMT calib., optics) • Shandong Univ. (PMT calib.. Computing & Simulation) • Hebei Normal Univ. (Simulation) • New collaborators • EPC of IHEP (KM2A electronics, DAQ) • USTC (WCDA electronics, trigger and PMT calib.) • PKU (computing, UHE CRs) • IAP (high Altitude Atmospheric Phys. ) • CSSAR (Space weather monitoring and prediction) • NSMC (Space weather monitoring and prediction) • IMP (Biophys. & Environment ) • Communication Members (potential collaborators): • Tsinghua Univ. • Shanghai Jiaotong Univ. • Eastern Institute of Science and Technology • Nanking Univ.

  28. International Collaboration • ARGO collaboration: • Rome II Univ. （RPC, Simulation, Slow Control） • Lecce Univ.（CRs, electronics) • Napeli Univ. (DAQ) • Torino Univ. (ECAL, GRBs) • ….. • Magic collaboration: • Max Planck Institute (Germany) (electr., Simulation, analysis) • Padova Univ. (Italy) (Telescope, optics) • IFAE (Spain) (Telescope, analysis) • ….. • Heidelberg Univ. (phys. Analysis) • Communication Members (future collaborators): • HAWC Coll.(WCDA)

  29. You are invited to Lhaaso at Lhasa! Large High Altitude Air Shower Observatory

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