Toward Stronger Sino-French Toward Stronger Sino-French cooperation on Particle Physicscooperation on Particle Physics

Hesheng Chen Institute of High Energy Physics

Beijing100049 China

Sino-French Cooperation• Chinese and French physicists worked closel

y 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.

Sino-French Cooperation• Many exchanges and workshop between IHE

P and CPPM, IPNL, CC-IN2P3/CEA • Workshop Dec. 2006 at IHEP Beijing started l

arge 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 20

07, CAS and CNRS/CEA signed generl agreement and the agreement of FCPPL

• A leap in the bilateral cooperation • President of CNRS, Catherine Brechignac, vi

sited China last Nov.. Big reception in IHEP 27 Nov. 2007.

Wide Scope of FCPPL1. Physics at LHC experiments: Atlas, CMS, LH

Cb, Alice 2. ILC: R&D and physics studies3. Physics at BES4. Astrophysics and Astroparticles: SVOM, Pola

r, UHE Radio Detection 5. Theory6. Related technologies and applications:

– W-LCG, – ASIC, – SC Technology, – Medical Applications…

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• …….

Beijing-LCG Core Servers (SRM-dCache, CE, TOP-BDII, RB, LFC, My

proxy, 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

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.

2.5Gbps

Improved the bandwidth Between Europe and China significantly.

Networking – ORIENT/TEIN2

Network PerformanceGri df tp Test Resul t Between I HEP to I N2P3

0

5

10

15

20

25

1 2 4 8 16 32 64 80Streams

Thro

ughp

ut(M

B/s)

I HEP->I N2P3 Average I HEP->I N2P3 I nstantI N2P3N->I HEP Average I N2P3->I HEP I nstant

Cumulative Transfer Volume from CC-IN2P3 to IHEP last year

2. AMS Physics Goals

Measurement of charged particles, nuclei and gammas:

• charged particle rigidity: 0.5 GV to ~ TV

• energy : 1 GeV to ~ TeV

Astrophysics:High-Energy (AGNs, GRBs, SNRs) Search for Nuclear Antimatter: anti-He @ 10-9 sensitivity anti-C @ 10-6 sensitivity Search for Dark Matter inp, e+ and gamma spectra

AMS

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

AMS ECAL: IHEP Beijing, LAPP Annecy

INFN Pisa

Bilateral Cooperation of LAPP and IHEPBilateral Cooperation of LAPP and IHEP• “CALIBRATION AND INTEGRATION OF AMS CA

LORIMETER” (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

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.

Chinese Scientist work with LAPP colleague on test beam

LAPP scientist and engineer join the assembling

of the ECAL flight structure in Beijing

AMS Beijing Group with AMS colleagues from France ,Italy and US after space qualification test with success

3. SVOM--A multi-λGRB projectGRM(China): 20 keV-5 MeV

VT(China): 45 cm diameter

CXG(France): 4-150 keV

SXT(France): 0.3-2 keV

China-France collaborationChina-France collaboration

Launch 2011-2012Phase A: 2007Phase A review:Mar. 2008

Scientific instrumentsScientific instruments :GRMs ( gamma-ray monitors)CXG (hard X-ray camera)SXT(Soft X-ray Telescope )VT ( visible telescope)

GRM SVOM should have some capability that SWIFT do

es not have. SVOM will observe all GRB events before and afte

r 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) .

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).

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

GRM description

    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 ph cm−2s−1 When Incident angle = 0 °

Burst detection

~80 GRBs per year  

Date rate   ~80 Mbytes/day(TBC)

dimension

Detector module:220mm*220mm*400mmParticle monitor:65mm*50mm*69mmElectronics case:252mm*180mm*172mm

Not include mounting architecture in the dimension of detector module.

The

mai

n te

chni

cal c

hara

cter

istic

s

GRM prototype---GRD

23/5/5 23

Front-end circuit

PMTMounting bracket

Phoswich box

0.75 mm 6 mm15 mm35 mm

Collimator: 1mm thick, 40mm high

StatusWhat 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.

23/5/5 24SVOM progress meeting

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% China 50% + others 50%

POLAR mission status Instrument conception pro

posed 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 skyMDP is 10%: >10 GRBs per

year down to 10% polarization;

Tian-GongTian-Gong天宫天宫

Palace in Palace in HeavenHeaven

POLARPOLAR

GRB prompt emission polarization: one of the last observables of GRBs

Different GRB models• E-M Model: well defined, mod

erate Plin ~ 50%• Fireball Model: high values e

xcluded 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

See papers discussing various GRB models: T. Piran, A. Dar, M. Lyutikov, D. Eichler, G. Ghisellini, D. Lazzatti, M. Medvedev, E. Rossi etc.

From M. Lyutikov, 2003

E

W

S N

Control room

21CMA Layout 81 pods along two perpendicular arms (East-West: 6 km + North-South: 4 km)

1 pod (= 127 antennas)

5. 21CMA Experiment: Xinjiang, China

420 m

270 m

Tibet AS ARGO-YBJ

Yangbajing CR Observatory: Tibet, China

Possible cooperation item: UHE Radio Detection

• 21CMA Experiment– Site: 4256’N, 8641’E– Altitude: 2600 m a.s.l.– Effective area: ~2.5 km2 (ass

ume 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: 3006’N, 9031’E– Altitude: 4300 m a.s.l.– Effective area: ~0.1km2(shower c

ore inside detector array)– Number of events: ~2700/yr (E0>

5x1016eV, 100% duty cycle)– Radio antenna array to be built– LOPES style study: EAS paramet

ers are known well.– Radio background: some– Infrastructure: good

6. Telescope at Dome A• Chinese Government is going to set up the thi

rd 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.

Dome C Dome A

Lawrence et al. 2004, Nature, 431, 278

Agabi et al. PASP, 118, 840, 344

AST3: Three 0.5 meter wide field Schmidt telescopes @ 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

4 meter wide field Telescope

• Supernovae• Galaxies (BAO, Wea

k Lensing)• Galaxy Polarimetry

Summary• FCPPL opened new page in the particle physi

cs cooperation between China and France.• Collaborations in LHC experiments and W-LC

G are progressing well. • Great potential in the particle astrophysics ex

periments• CAS and President Lu push hard for the coop

eration between CAS and CNRS/CEA