1 / 35

Toward Stronger Sino-French cooperation on Particle Physics

Toward Stronger Sino-French cooperation on Particle Physics. Hesheng Chen Institute of High Energy Physics Beijing100049 China. Sino-French Cooperation. Chinese and French physicists worked closely in many international collaborations: L3, ALEPH, AMS…

lakia
Download Presentation

Toward Stronger Sino-French cooperation on Particle Physics

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Toward Stronger Sino-French cooperation on Particle Physics Hesheng Chen Institute of High Energy Physics Beijing100049 China

  2. Sino-French Cooperation • Chinese and French physicists worked closely in many international collaborations: L3, ALEPH, AMS… • Until recently the level and the scale of the bilateral cooperation were rather lower. • Bilateral workshop of Astroparticle physics and cosmology at CPPM Sept. 2005. • Discussion with Roy Alekson by phone Oct. 2005 • Chen of IHEP and Spiro of IN2P3 signed the cooperation agreement on LCG at IN2P3 Feb, 2006. • Representative of IN2P3 in Beijing since Aug. 2006: Dr. Lydia Roos.

  3. Sino-French Cooperation • Many exchanges and workshop between IHEP and CPPM, IPNL, CC-IN2P3/CEA • Workshop Dec. 2006 at IHEP Beijing started large scale and national wide bilateral cooperation: beginning of FCPPL. F. Le Diberder. • Visit Prof. Zinn-Justin of CEA/Scaley • During the visit of CAS president LU April 2007, CAS and CNRS/CEA signed generl agreement and the agreement of FCPPL • A leap in the bilateral cooperation • President of CNRS, Catherine Brechignac,visited China last Nov.. Big reception in IHEP 27 Nov. 2007.

  4. Wide Scope of FCPPL • Physics at LHC experiments: Atlas, CMS, LHCb, Alice • ILC: R&D and physics studies • Physics at BES • Astrophysics and Astroparticles: SVOM, Polar, UHE Radio Detection • Theory • Related technologies and applications: • W-LCG, • ASIC, • SC Technology, • Medical Applications…

  5. 1. LHC experiments and W-LCG • ATLAS collaboration: IHEP, SDU and CPPM, CEA/Saclay, LPNHE • CMS: IHEP and IPNL • LHCb: Tsinghua and • WLCG: IHEP and CC-IN2P3/CEA • …….

  6. Beijing-LCG • Core Servers (SRM-dCache, CE, TOP-BDII, RB, LFC, Myproxy, MON, VOBOX ) • IBM-X3650 • Dual-CPU Intel 5130 • 2x2GB RAM • 2x73GB SAS/10k Disk Raid1 • 1Gb network. • Worknodes (CPUs/cores will be upgraded to 232 next month) • Dual-CPU Intel 5345 • 2x8GB RAM • 1Gb network • Storage • Old SE with 1.1 TB and one server • New SE with 10 TB and five servers

  7. Sino-French Collaboration on W-LCG • A lot of interactions. • People from IHEP visited CC-IN2P3 • CC-IN2P3 helped IHEP on the Tier-2 operation.

  8. Networking – ORIENT/TEIN2 2.5Gbps Improved the bandwidth Between Europe and China significantly.

  9. Network Performance

  10. Cumulative Transfer Volume from CC-IN2P3 to IHEP last year

  11. AMS 2. AMS Physics Goals • Measurement of charged particles, nuclei and gammas: • charged particle rigidity: 0.5 GV to ~ TV • g energy : 1 GeV to ~ TeV • Astrophysics:High-Energy g (AGNs, GRBs, SNRs) • Search for Nuclear Antimatter:  anti-He @ 10-9 sensitivity  anti-C @ 10-6 sensitivity • Search for Dark Matter inp, e+ and gamma spectra

  12. Calorimeter for AMS-02: ECAL • Used in AMS as: • Particle ID • Energy measurement (e+,e+,) • Trigger on non interacting photons • Anti-veto: for electrons and positrons that deposit energy anti coincidence system ECAL: last subdetector crossed by particles from outer space

  13. AMS ECAL: IHEP Beijing, LAPP Annecy INFN Pisa Bilateral Cooperation of LAPP and IHEP • “CALIBRATION AND INTEGRATION OF AMS CALORIMETER” (2006-2008) supported by “Programme International de cooperation scientifique(PICS) FRANCE ” and “IHEP CAS” • Setup the FPCCL project of “AMS ECAL Characterization and Integration” in 2007

  14. Scientific Exchange between LAPP and IHEP Scientists and PHD students from IHEP cooperate in LAPP, working on “AMS ECAL PMT Test” ,“AMS ECAL Front End Electronics Test” and “AMS ECAL Front End Electronics and PMT Thermal vacuum test” “AMS ECAL beam test”,etc. 10 person*times total 25 person*months. Scientists and Engineers from LAPP work on ECAL assembling and Space Qualification test in Beijing. 9 person*times.

  15. Chinese Scientist work with LAPP colleague on test beam

  16. LAPP scientist and engineer join the assembling of the ECAL flight structure in Beijing

  17. AMS Beijing Group with AMS colleagues from France ,Italyand US after space qualification test with success

  18. 3. SVOM--A multi-λGRB project VT(China): 45 cm diameter GRM(China): 20 keV-5 MeV • Scientific instruments : • GRMs ( gamma-ray monitors) • CXG (hard X-ray camera) • SXT(Soft X-ray Telescope ) • VT ( visible telescope) CXG(France): 4-150 keV SXT(France): 0.3-2 keV Launch 2011-2012 Phase A: 2007 Phase A review:Mar. 2008 China-France collaboration

  19. GRM • SVOM should have some capability that SWIFT does not have. • SVOM will observe all GRB events before and after T0 in the X-ray band (1‑10 keV) and in the hard X-ray and soft gamma-ray band (20 keV to 5 MeV), in order to determine as accurately as possible the GRB peak energy. • Swift’s capability to determine the peak energy of GRBs is weak, because of the narrow energy range of SWIFT/BAT (15-100 keV) .

  20. It is difficult to study the GRB cosmology (SVOM mission scientific goals) via SWIFT GRBs, because, currently the methods to study the GRB cosmology is to use GRB’s redshift and peak energy. • GRM will provide the spectral observation on GRBs from ~20 keV to ~5000 keV • GRM will determine the GRBs’ peak energy in hard X and soft gamma ray band. • GRM will enhance sensitivity of the Main Instrument (CXG).

  21. GRM description GRM is composed of 2 Gamma-ray detector units (under the limit of mass budget), one charged particle monitor and one electronic unit.

  22. note Detector 15 mm NaI(Tl) + 35 mm CsI(Na) 2 units, geometry area per unit is 280 cm^2 Energy range ～0.02-5 MeV FOV ～90°×90° Energy res. ～19%@60 keV Power cons. ～20 W One detector: ~1 W，total 2 W; electronic system: 17W; particle monitor: 1 W Mass ～40 kg Trigger sensitivity 0.23 phcm−2s−1 When Incident angle = 0 ° Burst detection ~80 GRBs per year Date rate ~80 Mbytes/day(TBC) dimension Detector module: 220mm*220mm*400mm Particle monitor: 65mm*50mm*69mm Electronics case: 252mm*180mm*172mm Not include mounting architecture in the dimension of detector module. The main technical characteristics

  23. GRM prototype---GRD 0.75 mm 6 mm 15 mm 35 mm Front-end circuit Phoswich box Collimator: 1mm thick, 40mm high Mounting bracket PMT 2014/8/28 23

  24. Status What have been done: • GRM design almost done • GRM prototype done • Preliminary test of GRD Next: • preparation for phase A review in Mar. 2008 • Optimization • phoswich, mechanical design, thermal requirement • Engineering model • Quality, lifetime, reliability, etc. 2014/8/28 SVOM progress meeting 24

  25. 4. GRB Polarization Instrument aboard China’s Spacelab: POLAR • China IHEP/Tsinghua: S.N. Zhang (PI) • China IHEP: H.Y. Wang, B.B. Wu, etc. • France LAPP: G. Lamanna, J-P Vialle • France CPPM: Ch. Tao • France LAM: tbd • Suisse ISDC: N. Produit (Co-PI), D. Haas • Suisse PSI: W. Hajdas, A. Mchedlishvili • Suisse DPNC: E. Suarez, M. Pohl, C. Leluc, D. Rapin • Poland IPJ: R. Marcinkowski, M. Gierlik China 50% + others 50%

  26. POLAR mission status POLAR Tian-Gong 天宫 Palace in Heaven • Instrument conception proposed by N. Produit, et al., NIM (2005) • On board China’s spacelab TG-2: launch time 2011-12 (Phase 2 of China manned spacecraft program, to be confirmed by China government this year.) • FOV of POLAR: ~½ sky • MDP is 10%: >10 GRBs per year down to 10% polarization;

  27. GRB prompt emission polarization: one of the last observables of GRBs • Different GRB models • E-M Model: well defined, moderate Plin ~ 50% • Fireball Model: high values excluded Plin ~ 10-20 % • Cannon ball Model: full range possible Plin = 0 - 100% • Probe quantum gravity (???): • Amelino-Camelia G., 2000, Nature, 408, 661 • Amelino-Camelia G., et al., 1998, Nature, 393, 763 • Piran T, 2005, Lect. Notes Phys, 669, 351 • Fan, Y-Z; Wei, D-M; Xu, D. 2007, MNRAS, 376, 1857 From M. Lyutikov, 2003 See papers discussing various GRB models: T. Piran, A. Dar, M. Lyutikov, D. Eichler, G. Ghisellini, D. Lazzatti, M. Medvedev, E. Rossi etc.

  28. 5. 21CMA Experiment: Xinjiang, China S N W 1 pod (= 127 antennas) 21CMA Layout 81 pods along two perpendicular arms (East-West: 6 km + North-South: 4 km) Control room E

  29. Yangbajing CR Observatory: Tibet, China 270 m Tibet AS ARGO-YBJ 420 m

  30. 21CMA Experiment Site: 4256’N, 8641’E Altitude: 2600 m a.s.l. Effective area: ~2.5 km2 (assume radio signal detected upto 250 m away from shower core) Number of events: ~5000/yr (E0>1017eV, 50% duty cycle) No particle detector array available, no trigger source. Radio background: small Infrastructure: poor YBJ CR Observatory Site: 3006’N, 9031’E Altitude: 4300 m a.s.l. Effective area: ~0.1km2(shower core inside detector array) Number of events: ~2700/yr (E0>5x1016eV, 100% duty cycle) Radio antenna array to be built LOPES style study: EAS parameters are known well. Radio background: some Infrastructure: good Possible cooperation item:UHE Radio Detection

  31. 6. Telescope at Dome A • Chinese Government is going to set up the third south pole scientific station at Dome A. • Dome A : >4000m a.s.l. , +: Dark, Dry, Cold, Quiet, Good weather, no rain or snow. lowest temperature, driest atmosphere, lowest snow fall. Continuous dark time for about 4 months Space quality images -: temp. as low as -80c; transportation difficult. Oxygen similar to 6000 a.s.l. Remote control most of time. • The Chinese South Pole Expedition reached Dome A last weekend, will install a small telescope to check if it works.

  32. Dome C Dome A Lawrence et al. 2004, Nature, 431, 278 Agabi et al. PASP, 118, 840, 344

  33. AST3: Three 0.5 meter wide field Schmidttelescopes @ Antarctica - 3 wide field telescopes of field of view of 10 square degrees (can image an area 13 times the size of the sun), each of 50 cm in diameter. - Can operate in a mode with no mechanical moving parts - Can track the bulge of the Milky Way and discover thousands of extrasolar planets. - Can discover over 2000 Type Ia supernovae to probe the nature of dark energy in the Universe - Can study quasi-stellar objects, AGN,GRB

  34. 4 meter wide field Telescope • Supernovae • Galaxies (BAO, Weak Lensing) • Galaxy Polarimetry

  35. Summary • FCPPL opened new page in the particle physics cooperation between China and France. • Collaborations in LHC experiments and W-LCG are progressing well. • Great potential in the particle astrophysics experiments • CAS and President Lu push hard for the cooperation between CAS and CNRS/CEA

More Related