1 / 35

Astroparticle Physics with AMS-02

Astroparticle Physics with AMS-02. Dr. C.Sbarra INFN-Bologna, Italy On behalf of the AMS collaboration 12th Lomonosov Conference, Moscow 2005. Outlook. The AMS experiment and its forthcoming operation on International Space Station (ISS)

breck
Download Presentation

Astroparticle Physics with AMS-02

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. Astroparticle Physics with AMS-02 Dr. C.Sbarra INFN-Bologna, Italy On behalf of the AMS collaboration 12th Lomonosov Conference, Moscow 2005

  2. Outlook • The AMS experiment and its forthcoming operation on International Space Station (ISS) • The antimatter discovery potential of AMS-02 and the Baryogenesis scenarios investigated • The e+ , p , ddetection and subsequent impact on the various models of exotic physics Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  3. The Test Experiment: AMS-01 Onboard the shuttle Discovery (1998) • Results: • Environmental studies • Background studies • Fulfill the constraints from space • Antimatter/matter limit • (<1.1x10-6 at 95% C.L. PR 366/6, 2002) Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  4. The AMS-02 experiment The Anti Matter Spectrometer The knowledge obtained in the precursor 10 days flight AMS-01 (1998) was used to redesign the spectrometer for the ISS: • Long exposure: > 3 years • Superconducting magnet (BL2 0.86 T, 1m3 fill volume) • Large acceptance: 0.5 m2 sr • Many repeated measurements of particle velocity, momentum and charge Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  5. The AMS-02 experiment PID : The subdetectors • Huge statistics of all type of Cosmic rays in the energy range 1 GeV – 1 TeV (/nucl) • For low rates high redundancy and precise detector measurements

  6. The AMS-02 experiment PID : The subdetectors • 20 layers of TRD for e+/h sep. (1.5 -300 GeV) • 4 layers of TOF for trigger, time (150 ps), βand |Q| meas. • 8 layers of double sided Silicon tracker for p (10/30 μm res. b./non b.) and ±Q meas. • VETO Counters • RICH for β (Δβ/β~0.1%) and |Q| • 3D sampling ECAL (17X0of plastic fibers) for e+e-/h sep. (1.5 GeV-500GeV) Super conducting Solenoid (0.86 T) He vessels Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  7. The AMS-02 experiment Spectrometer Resolution (P.R. 366/6) Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  8. The AMS discovery potential Antimatter in our universe • The physical laws at microscopic level are symmetric between baryons and anti-baryons • The physical Universe seems to be asymmetric (there seems to be only matter) - How can evolve an asymmetric universe (totally or even only locally) from a primordial big-bang and with symmetric laws? baryogenesis ? Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  9. Andrei Shakarov put the necessary conditions for baryogenesis [JETP Lett. 91B,24 (1967)] : Baryon number B non conservation C and CP non conservation Out of equilibrium decay - The inflation is a natural scenario where a baryogenesis can take place: it allows the out of equilibrium condition and it can avoid the a-prori hypothesis of initial symmetric conditions [L.F. Abbott et Al.,Physics Lett.117B(1982)] Antimatter in our universe: Baryogenesis Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  10. Antimatter in our universe: Baryogenesis Is the Universe globally or only locally asymmetric? • In a totally symmetric universe, high energy CRs could escape from an antimatter domain and get to our galaxy • On the basis of γ-rays observations our matter dominated region has at least the size of cluster of galaxies Is there place for antimatter in a totally asymmetric Universe as seem to be ours? Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  11. Antimatter in our universe: Baryogenesis [M. Y. Khlopov, S.G.Rubin and Al.S.Sakharov hep-ph/0210012 ] • In the matter dominated universe there is also the possibility of small insertions of antimatter regions : Quantum fluctuations of a complex, baryonic charged scalar field caused by inflation can generate antimatter regions that can survive annihilation • There can exist antistar global clusters in our galaxy • The expected signature of such scenario is a flux of 3He and 4He accessible to AMS-02 Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  12. Pamela Antimatter in our universe: Experimental searches An anti-nucleus can be found in Cosmic Rays, with a spectrometer on top of the atmosphere (balloons) or on a satellite (Pamela, AMS-02) Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  13. Antimatter in our universe: Antinuclei, antiparticles • The antiparticles are “secondaries” produced by CR interactions with ISM through inelastic collisions – “spallation” Flux 4He O(10-12), D O(10-8), p O(10-4), e+ O(10-3) • But some antiparticles can be “primaries” from exotic sources of antimatter or DM annihilation (an He would be evidence of antistars) Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  14. Antimatter in our universe: antiparticles - Positrons Edsjö et al • Ratio e+/(e++e-) can reveal neutralino annihilations [Phys.Rev.D 65/6] HEAT data show possible excess around ~10GeV Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  15. Antimatter in our universe: antiparticles - Positrons AMS can measure 106positrons up to 300 GeV and can confirm or not the bump • Flux ratio : p/e+ ~ 103 Strong p/e+ rejection - TRD : Rej~103/102 in 3-300 GeV - ECAL: Rej~104 for E~500 GeV (TRD + ECAL together Rej ≥ 105) Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  16. Antimatter in our universe: Antideuterons • Antideuteron is to be observed in CRs D limit from Bess < 1.9x10-4 (m2 ·s·sr·GeV/n)[28th ICRC 2003] The neutralino (the lightest supersymmetric particle) would be left as relic by large amount of sparticles decayed • AMS-02 can observe O(10) low momentum D from neutralino annihilation [F.Donato et Al.1999] Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  17. Antimatter in our universe: Antideuterons • The known ratio of D/p is ~ 10-5in the observed universe • AMS-02 can detect D from antimatter domains : D/p ~ 10-5(AMS-01 observed ~100 p, thus D was unobservable) The ratio of primordial He to D is ~ 104 and in CR it is about 10 thus any D from antimatter domain would be accompaigned by He or p Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  18. Antimatter in our universe: Antiprotons • Antiproton flux O(10-4) at E~1 GeV (e-/p ~ 103 at E ~ 1 GeV strong e-/p rejection at this energy) • Antiprotons in CRs have been detected up to O(10 GeV) and all seem to be compatible with secondary production Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  19. Antimatter in our universe: Antiprotons • Simulation of three years of high statistics measurements of antiproton spectrum • AMS-02 will be able to detect antiprotons up to 400GeV [V.Choutko,Nucl.Phys.B Proc.Suppl.113-2002] Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  20. Antimatter in our universe: Antiprotons • Proton rejection: good control of charge confusion, interaction with the detector and misreconstructed tracks • Electron rejection: use TOF + RICH beta measurements at low energies, TRD and ECAL rejection capability at high energy Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  21. Wolfendale & Stecker hypothesis[19th ICRC proc. p.354]: We know that the mean lifetime of a CR in the galaxy falls with energy as E-δ with δ~0.7 If antiprotons are produced and accelerated in an antimatter domain as the protons are in our galaxy The antiproton/proton ratio , at high energies, would go~ Eδ with δ~ 0.7 , the antiprotons being mainly extragalactic and the protons galactic Antimatter in our universe: Antiprotons Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  22. Antimatter in our universe: Antiprotons [data from Golden, Buffington, Bogolmolov] • Primary hypothesis: p/p E0.7 From Stecker & Wolfendale, 19th ICRC (La Jolla) 1985, OG6.1-8, p354 • At energy E>100GeV the experimental data could discriminate between primary and secondary hypothesis Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  23. AMS-01 [V.Choutko] Antimatter in our universe: Antiprotons • Most recent data on p/p [by Picozza and Morselli J.Phys.G: Nucl.Part.Phys.29 (2003)] • Superimposed extragalactic hypothesis, black hole evaporation model, secondary production • More data could discriminate between the various models for E >10GeV Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  24. Antimatter in our universe: Antiprotons • As other antiparticles, antiprotons at lower energy could reveal neutralino annihilation: • χχ WW,.. e+, p, D, γ… ( Indirect search in several channels ) • Flux of products depends on neutralino density, CRs propagation terms,.. Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  25. Signal : 1) M=964 GeV (4200) 2) M=777 GeV (1200) Antimatter in our universe: Antiprotons Ullio (1999) • Antiprotons are particularly sensitive to the physics details of CR propagation (controlled by B/C ratio), particularly at low momentum Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  26. Conclusion • The AMS-02 spectrometer will measure CRs fluxes with high precision for more than three years • AMS-02 will be sensitive to antinuclei up to 100 Mpc of distance • AMS-02 can discriminate between a totally symmetric or an antisymmetric universe also through antiprotons at E >100GeV • AMS-02 will have the sensitivity to detect the products of DM annihilation in our galaxy through positrons, antideuterons and antiprotons at O(GeV) energy Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  27. SLIDES EXTRA

  28. The AMS-02 experiment Operation in Space constraints • Thermal range (day/night ΔT~1000 ) • Vibration (6.8 G RMS) and G-Forces (17 G, 9 G take off) • Weight limitation (7000 kg) • Power limitation (2000 W) • Vacuum: < 10-10 Torr • Radiation ionizing flux ~1000 cm-2s-1 • Orbital debris and micrometeorites • Must operate without human intervention (Redunduncy) Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005

  29. AMS-01 p/pbar all recent + Ams01

  30. p/pbar – all recent data

  31. Energy resolution (from Palomares) (E)/E ~ 3% for 100 GeV electrons

  32. The AMS-02 experiment AMS –γ :2 modes detection Converted  : Detection of the e+e- pair in the tracker Calorimeter : Standalone trigger

  33. The AMS-02 experiment Energy Resolution ….

  34. The AMS-02 experiment Angular Resolution (tracker)

More Related