astroparticle physics with ams-02
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Astroparticle Physics with AMS-02
Dr. C.SbarraINFN-Bologna, Italy
On behalf of the AMS collaboration
12th Lomonosov Conference, Moscow 2005
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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 , d detection and subsequent impact on the various models of exotic physics
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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The Test Experiment: AMS-01
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
Results: • Environmental studies• Background studies• Fulfill the constraints from space• Antimatter/matter limit (<1.1x10-6 at 95% C.L. PR 366/6, 2002)
Onboard the shuttle Discovery Onboard the shuttle Discovery (1998)(1998)
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The AMS-02 experiment
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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
The Anti Matter The Anti Matter SpectrometerSpectrometer
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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
The AMS-02 experimentPID : The PID : The subdetectorssubdetectors
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The AMS-02 experiment
20 layers of TRD for e+/h sep. (1.5 -300 GeV)
4 layers of TOF for trigger, time (150 ps), β and |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)
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
PID : The PID : The subdetectorssubdetectors
Super conducting Solenoid (0.86 T)
He vessels
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The AMS-02 experimentSpectrometer Resolution (P.R. Spectrometer Resolution (P.R. 366/6)366/6)
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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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 ? baryogenesis ?
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
The AMS discovery potential Antimatter in our Antimatter in our universeuniverse
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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: Antimatter in our universe: BaryogenesisBaryogenesis
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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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?
Antimatter in our universe: Antimatter in our universe: BaryogenesisBaryogenesis
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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[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
Antimatter in our universe: Antimatter in our universe: BaryogenesisBaryogenesis
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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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)
Antimatter in our universe: Antimatter in our universe: Experimental searchesExperimental searches
Pamela
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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Antimatter in our universe: Antimatter in our universe: Antinuclei, antiparticlesAntinuclei, 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
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Ratio e+/(e++e-) can reveal neutralino annihilations [Phys.Rev.D 65/6]
HEAT data HEAT data show possible show possible excess around excess around ~~10GeV 10GeV
Antimatter in our universe: Antimatter in our universe: antiparticles - Positronsantiparticles - Positrons
Edsjö et al
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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AMS can measure 101066 positrons up to 300 GeV and can confirm or not the bump
Flux ratio : p/e+ ~ 103
Strong p/e+ rejectionStrong p/e+ rejection - TRD : Rej TRD : Rej~10~1033/10/1022 in 3-300 GeV in 3-300 GeV
- ECAL: RejECAL: Rej~~101044 for E for E~~500 GeV500 GeV (TRD + ECAL together Rej (TRD + ECAL together Rej ≥ ≥ 101055))
Antimatter in our universe: Antimatter in our universe: antiparticles - Positronsantiparticles - Positrons
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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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 The neutralino (the lightest supersymmetric
particle) would be left as relic by large particle) would be left as relic by large amount of sparticles decayedamount of sparticles decayed
AMS-02 can observe O(10) low momentum D from neutralino annihilation [F.Donato et Al.1999]
Antimatter in our universe: Antimatter in our universe: AntideuteronsAntideuterons
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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The known ratio of D/p is ~ 10-5 in 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 ~ The ratio of primordial He to D is ~ 10104 4 and in CR it is about 10 thus any and in CR it is about 10 thus any D from antimatter domain would be D from antimatter domain would be accompaigned by He or paccompaigned by He or p
Antimatter in our universe: Antimatter in our universe: AntideuteronsAntideuterons
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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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
Antimatter in our universe: Antimatter in our universe: AntiprotonsAntiprotons
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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Antimatter in our universe: Antimatter in our universe: AntiprotonsAntiprotons
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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 [V.Choutko,Nucl.Phys.B Proc.Suppl.113-2002]Proc.Suppl.113-2002]
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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
Antimatter in our universe: Antimatter in our universe: AntiprotonsAntiprotons
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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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: Antimatter in our universe: AntiprotonsAntiprotons
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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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
Antimatter in our universe: Antimatter in our universe: AntiprotonsAntiprotons
[data from Golden, Buffington, Bogolmolov]
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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
Antimatter in our universe: Antimatter in our universe: AntiprotonsAntiprotons
AMS-01 [V.Choutko]
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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,..
Antimatter in our universe: Antimatter in our universe: AntiprotonsAntiprotons
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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Antimatter in our universe: Antimatter in our universe: AntiprotonsAntiprotons
Signal :
1) M=964 GeV (4200)
2) M=777 GeV (1200)
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
Ullio (1999)
Antiprotons are particularly sensitive to the physics details of CR propagation (controlled by B/C ratio), particularly at low momentum
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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
ConclusionConclusion
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
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SLIDES EXTRA
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The AMS-02 experiment
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)(Redunduncy)
Dr.C.Sbarra, INFN-Bologna, Italy 12th Lomonosov Conference, Moscow 2005
Operation in Space Operation in Space constraintsconstraints
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p/pbar all recent + Ams01
AMS-01
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p/pbar – all recent data
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Energy resolution (from Palomares)
(E)/E ~ 3% for 100 GeV electrons
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The AMS-02 experimentAMS –AMS –γγ : : 2 modes 2 modes detectiondetection
Converted :Detection of the e+e- pair in the
tracker
Calorimeter :Standalone trigger
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The AMS-02 experimentEnergy Resolution ….Energy Resolution ….
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The AMS-02 experimentAngular Resolution (tracker) Angular Resolution (tracker)
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