1. Lake Louise - February 20-26 2005 1 1 Detection & Measurement of gamma rays in the AMS-02 Detector J. Bolmont - LPTA - IN2P3/CNRS Montpellier - France On behalf of AMS collaboration J. Bolmont - LPTA - IN2P3/CNRS Montpellier - France On behalf of AMS collaboration

2. J. Bolmont - LPTA Lake Louise - February 20-26 2005 2 Outline Detecting  with AMS-02 -Conversion Mode -Single Photons Cosmic Ray Fluxes Various  sources -Pulsars, GRBs -Cold Dark Matter

3. J. Bolmont - LPTA Lake Louise - February 20-26 2005 3 AMS-02 Launch scheduled in 2008

4. J. Bolmont - LPTA Lake Louise - February 20-26 2005 4 Detecting  with AMS Two complementary modes -Tracker mode :   e + e - conversion in TRD -ECAL mode : single  no hit in TOF & Tracker Completeness of AMS-02 : overall proton to gamma supression factor 10 4 - 10 5  e+e+ e-e-

5. J. Bolmont - LPTA Lake Louise - February 20-26 2005 5 Detecting  with AMS :   e + e - The Si Tracker : charged track reconstruction & identification -8 layers -Double sided silicon strips -Total area : 7 m 2 -200000 channels A layer completely equipped

6. J. Bolmont - LPTA Lake Louise - February 20-26 2005 6 Tracker Resolutions Beam test results Angular resolution ~0.02° when E > 100 GeV. Energy resolution at high energy affected by the leptons trajectory reconstruction errors. Energy ResolutionAngular Resolution

7. J. Bolmont - LPTA Lake Louise - February 20-26 2005 7 Detecting  with AMS : single  showers The Electromagnetic Calorimeter -SPACAL calorimeter (Pb + Scintillating fibers) -9 superlayers (~16 X 0 ), X-Y sampling -324 PMTs with 4 pixels  1296 channels high granularity 3 Superlayers

8. J. Bolmont - LPTA Lake Louise - February 20-26 2005 8 EM Calorimeter Resolutions Energy ResolutionAngular Resolution Beam test results

9. J. Bolmont - LPTA Lake Louise - February 20-26 2005 9 Acceptance / Effective Area Monte Carlo simulations + Preliminary analysis Cos(incident angle)

10. J. Bolmont - LPTA Lake Louise - February 20-26 2005 10 Cosmic Ray Fluxes Cosmic Rays Composition : -p : 88 % -He nuclei : 9 % -e - : 2 %  : < 1% Standard CR spectra follows a "power law" E -  with  = 2-3 DM signal : exponential cut-off in the spectra

11. J. Bolmont - LPTA Lake Louise - February 20-26 2005 11 Various  sources Energy range : 1-300 GeV Sources in scope of AMS: -Galactic : pulsars, nebulas (VELA, CRAB,…) -Extra-Galactic : GRBs Diffuse  emission : interaction of Charged Rays with galactic medium produce  (  0 )

12. J. Bolmont - LPTA Lake Louise - February 20-26 2005 12 Some Results Of Simulations Using a fast simulation tool with parametrizations of ECAL & Tracker acceptances and resolutions 3EG CatalogOther Name N  (Tracker)N  (ECAL)N  (total) J0210-50550208-51247.013.460.4 J0530+13230528+13418.74.022.7 J0534+2200Crab102.226.6128.8 J0834-4511*Vela491.4203.8695.2 J1255-05493C279138.635.8138.6 J1409-07451406-07631.75.937.6 J1635+38131633+38265.518.383.8 One year of operation

13. J. Bolmont - LPTA Lake Louise - February 20-26 2005 13 Some Results Of Simulations : CRAB nebula+pulsar Results in 5 energy bands for 1 year of operation : 1-2 GeV 2-5 GeV 5-20 GeV 20-50 GeV > 50 GeV

14. J. Bolmont - LPTA Lake Louise - February 20-26 2005 14 Predictions for GRBs GRBs : the most explosive cosmological events after Big Bang : ~5x10 51 erg released in  Taking into acount the most luminous GRBs observed by EGRET & BATSE, we expect a few GRBs per year in AMS detector. Big uncertainties : processes of  production at high energies not known !

15. J. Bolmont - LPTA Lake Louise - February 20-26 2005 15 Cold Dark Matter The matter content of the Universe is 90% dark and non- baryonic. Astrophysical measurements of the star rotation velocities in the galaxies, of the large structures, gravitational arc phenomena confirm the CDM paradigm. Hypotheses : Dark Matter is Cold (CDM) and weakly interacting (WIMPs) Exotic – Supersymmetry (Particle Physics) offers an excellent WIMP candidate – the LSP as neutralino :  0 1 The WIMPs interact in the underground detectors with nucleons and annihilate in the halo of the Dark Matter and produce stable particles : , neutrinos, e+, anti-p, …

16. J. Bolmont - LPTA Lake Louise - February 20-26 2005 16 Predictions for benchmark fluxes Galactic Centre mSUGRA models MC simulation Accelerators & WMAP constraints Various DM halo profiles ModelBGIKL mm 98.3153.6143.0571.5187.2 m0m0 59.0116.0178.0999.0299.0 tan  10.20.35.38.247  relic 0.1220.1240.1220.1160.101 n  (NFW)0.110.070.470.141.17 n  (NFW cuspy)4.82.820.36.050.5 n  (Moore)14.18.259.017.5146.7 One year of operation J. Ellis et al. Eur. Phys. J. C24 (2002) 311

17. J. Bolmont - LPTA Lake Louise - February 20-26 2005 17 Predictions for  fluxes from the Galactic Centre : DarkSUSY + Suspect MC Different Models : -SUSY conventional (MSSM, mSUGRA) -Non thermal (AMSB) -Kaluza-Klein scenario MSSM = Minimal SuperSymetric Model mSUGRA = Minimal SUGRA model SUGRA = SuperGravity grand unified models AMSB = Anomaly Mediated SUSY Breaking

18. J. Bolmont - LPTA Lake Louise - February 20-26 2005 18 Summary Using Si-Tracker and EM Calorimeter, AMS-02 will provide new  measurements in the range 1-300 GeV during 3 to 5 year mission. AMS-02 will study several galactic and extragalactic  sources as Pulsars, GRBs… (At least) constraints in various Cold Dark Models will be provided.