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.

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Presentation transcript:

Lake Louise - February 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

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

J. Bolmont - LPTA Lake Louise - February AMS-02 Launch scheduled in 2008

J. Bolmont - LPTA Lake Louise - February 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  e+e+ e-e-

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

J. Bolmont - LPTA Lake Louise - February 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

J. Bolmont - LPTA Lake Louise - February 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

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

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

J. Bolmont - LPTA Lake Louise - February 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

J. Bolmont - LPTA Lake Louise - February Various  sources Energy range : 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 )

J. Bolmont - LPTA Lake Louise - February 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) J J J Crab J *Vela J C J J One year of operation

J. Bolmont - LPTA Lake Louise - February 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 GeV > 50 GeV

J. Bolmont - LPTA Lake Louise - February 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 !

J. Bolmont - LPTA Lake Louise - February 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, …

J. Bolmont - LPTA Lake Louise - February Predictions for benchmark fluxes Galactic Centre mSUGRA models MC simulation Accelerators & WMAP constraints Various DM halo profiles ModelBGIKL mm m0m tan   relic n  (NFW) n  (NFW cuspy) n  (Moore) One year of operation J. Ellis et al. Eur. Phys. J. C24 (2002) 311

J. Bolmont - LPTA Lake Louise - February 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

J. Bolmont - LPTA Lake Louise - February Summary Using Si-Tracker and EM Calorimeter, AMS-02 will provide new  measurements in the range 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.