The AMS detector: a particle physics experiment in space
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1 The AMS detector: a particle physics experiment in space Roberto Battiston University and INFN of Perugia International Workshop on Energy Budget in the High Energy Universe ICRR Tokyo February 21 st f/1
2 The universe is the ultimate laboratory to study fundamental physics. AMS, LISA/BBO WMAP, Planck Hubble XMM, Swift, Chandra, LISA 264 2f/2
3 264 2f/3.reaching energies which cannot be studied at accelerators AMS LISA/BBO LHC LEP
4 Messengers are photons, charged/neutral particles, gravitational waves f/4
5 18 Orders of magnitude in Energy 264 2f/5 Cosmic Ray Origin & Direct Measurements 50 Orders of magnitude in flux Intensity Log Intensity / m 2 sr sec GeV 15 orders of magnitude in flux Intensity 7 orders of magnitude in Energy
6 264 2f/6 The purpose of the AMS experiment is to perform accurate, high statistics, long duration measurements in space of energetic (0.1 GV few TV) charged CR energetic (>1 GeV) gamma rays.
7 264 2f/7 Cosmic rays Nobel Prizes, (1) Pulsar, (2) Microwave, (3) Binary Pulsars, (4) Solar neutrino X Ray sources
8 Alpha Magnetic Spectrometer - AMS-01 First flight, STS-91, 2 June 1998 (10 days) TOF Tracker Magnet TOF Cerenkov Counter y99163_04c.ppt 264 2f/8
9 264 2f/9
10 Magnetosphere effects 264 2f/10
11 264 2f/11
12 264 2f/12 February 2006 AMS
13 264 2f/13 AMS is an International Collaboration NASA provides: Three shuttle flights and Mission Management at JSCJ S. C.C. Ting - Spokesperson USA A&M FLORIDA UNIV. JOHNS HOPKINS UNIV. MIT - CAMBRIDGE NASA GODDARD SPACE FLIGHT CENTER NASA JOHNSON SPACE CENTER UNIV. OF MARYLAND-DEPT OF PHYSICS UNIV. OF MARYLAND-E.W.S. S.CENTER YALE UNIV. - NEW HAVEN MEXICO UNAM DENMARK UNIV. OF AARHUS FINLAND HELSINKI UNIV. UNIV. OF TURKU FRANCE GAM MONTPELLIER LAPP ANNECY LPSC GRENOBLE GERMANY RWTH-I RWTH-III MAX-PLANK INST. UNIV. OF KARLSRUHE ITALY ASI CARSO TRIESTE IROE FLORENCE INFN & UNIV. OF BOLOGNA INFN & UNIV. OF MILANO INFN & UNIV. OF PERUGIA INFN & UNIV. OF PISA INFN & UNIV. OF ROMA INFN & UNIV. OF SIENA NETHERLANDS ESA-ESTEC NIKHEF NLR PORTUGAL LAB. OF INSTRUM. LISBON ROMANIA ISS UNIV. OF BUCHAREST RUSSIA I.K.I. ITEP KURCHATOV INST. MOSCOW STATE UNIV. SPAIN CIEMAT - MADRID I.A.C. CANARIAS. SWITZERLAND ETH-ZURICH UNIV. OF GENEVA CHINA BISEE (Beijing) IEE (Beijing) IHEP (Beijing) SJTU (Shanghai) SEU (Nanjing) SYSU (Guangzhou) SDU (Jinan) ACAD. SINICA (Taiwan) CSIST (Taiwan) NCU (Chung Li) NCKU (Tainan) NCTU (Hsinchu) NSPO (Hsinchu) KOREA EWHA KYUNGPOOK NAT.UNIV.
14 G.F cm 2 sr Exposure > 3 yrs dp/p 2 ~ MDR = 2.5 TV, h/e = 10-6 (ECAL +TRD) 264 2f/14
15 264 2f/15
16 264 2f/16 AMS-02 spectrometer Acceptance for charged CR: 0.5 m 2 sr Exposure: at least 3 years (from 2008) Charge: Z determination up to Z = 26 charge confusion < Z=1 & < Z>10 Rigidity (R=p/Z): σ(r)/r = 10 GV, Max Detectable Rigidity > 2-3 TV Velocity (β): TOF: σ(β)/β = 3.5% (protons) RICH: σ(β)/β = 0.1% (protons)
17 264 2f/17
18 264 2f/18 AMS-02 goals and capabilities Cosmic rays spectra and chemical composition up to 1 TeV Search for Antimatter in Space Search for Dark Matter AMS will identify and measure the fluxes for: p for E < 1 TeV with unprecedented precision e+ for E < 300 GeV and e for E < 1 TeV (unprecedented precision) Light Isotopes for E < 10 GeV/n Individual elements up to Z = 26 for E < 1 TeV/n Absolute fluxes and spectrum shapes of protons and helium are important for calculation of atmospheric neutrino fluxes Composition and spectra are important to constraint propagation, confinement, ISM density
19 264 2f/19 Protons and helium AMS will measure H & He fluxes for E < 1 TeV after 3 years will collect 10 8 H with E > 100 GeV and 10 7 He with E > 100 GeV/n 6 hours 3 days
20 264 2f/20 Electrons and positrons Energetic e+/e cannot diffuse more than few kpc: they are sensitive probes of the Local Bubble and its neighbourhood.
21 264 2f/21 Heavier nuclei AMS will measure the flux of Z 26 for E < 1 TeV/n The secondary to primary ratio B/C is used to fit the CR diffusion parameters After 3 years will collect 10 5 Carbon with E > 100 GeV/n and 10 4 Boron with E > 100 GeV/n 6 months
22 264 2f/22 Nuclei separation Charge measurement: TOF, Tracker and RICH He Li Be Test Results from Tracker detector C O N Si Verified by heavy ion beam tests at CERN & GSI. TOF
23 264 2f/23 Light isotopes Hydrogen and helium isotopes (deuterium and 3 He) are important tests of Big Bang nucleosynthesis which is their main source. AMS-02 will identify D and 3 He up to 10 GeV/n 1 day 6 hours After 3 years AMS-02 will collect about 10 8 D and 3 He
24 264 2f/24 10 Be/ 9 Be radioactive clock 10 Be (t 1/2 = 1.51 Myr) is the lightest β-radioactive secondary isotope having a half-life comparable with the CR confinement time in the Galaxy. In diffusion models, the ratio 10 Be/ 9 Be is sensitive to the size of the halo and to the properties of the local interstellar medium AMS will separate 10 Be from 9 Be for 0.15 GeV/n < E < 10 GeV/n after 3 years will collect Be 1 year
25 264 2f/25
26 264 2f/26 Search for antimatter at the 10-9 level of sensitivity with AMS-02 on the ISS BESS flights Bess Polar (20 days) Pamela ( ) AMS on ISS ( )
27 Dark matter There are many theoretical suggestions that SUSY particles (χ) are at least part of the Dark matter. J. Ellis et al., Phys. Lett. B, 214, 3, 1988 and M. Turner and F. Wilczek, Phys. Rv. D, 42, 4, 1990 E.A. Baltz, J. Edsjo, P.R. D59, 23511, 1999 y97089_1p.ppt 264 2f/27
28 Non baryonic Dark Matter 264 2f/28 Baltz and Edsjo (1998) Indirect search with annihilation of DM candidates into standard model particles neutralino χ 0 from msugra (SuSy) χ o χ o qq, W + W -, HZ o, γγ, νν,.. p, p, e +, e -, γ e + example stable particles from Kaluza-Klein (KK photon in UED: B 1 ) Feng (2004) B 1 B 1 ff, HH p, p, e +, e - e + example AMS-02 can measure simultaneously indirect DM signal : e +, p, D and γ.
29 264 2f/29
30 Positron search 264 2f/30 Possible excess seen at 8 GeV by HEAT in cosmic positron fraction. S. Coutu et al. (ICRC 2001) Expected background DM interpretation. AMS-02 accuracy with e + from KK photon B 1 (UED) annihilation, χ 0 (msugra) annihilation. Ratio e + /(e + +e - ) Expected statistic for LKP of 300 GeV in AMS-02 AMS-02 accuracy with boost =1700 AMS-02 accuracy with boost =60 KK photon B 1 (UED) Signal fitted on HEAT data Expected statistic for benchmark E in AMS-02 χ 0 (msugra) 3 years 3 years Ratio e + /(e + +e - ) e m χ =124 GeV + background (e + signal * Boost) + back. AMS-02 accuracy Signal fitted on HEAT data
31 264 2f/31
32 AMS sensitivity to anti D 264 2f/32 AMS-02
![AMS-02 acceptances 264 2f/33 Antiproton acceptance 0.16 m 2.sr for [0.5-16] GeV 0.033 m 2.sr for [16-300] GeV tracker mode γ calorimeter mode γ Positron acceptance 0.042 m 2.sr for E e+ >4 GeV 0.](/docs-images/86/94285379/images/33-0.jpg "3 X 0 Gamma acceptance tracker mode: γ e + e - in the upper sub-detector 0.05 m 2.sr for [5-300] GeV calorimeter mode: no γ conversion until ECAL 0.08 m 2.")
33 AMS-02 acceptances 264 2f/33 Antiproton acceptance 0.16 m 2.sr for [0.5-16] GeV m 2.sr for [16-300] GeV tracker mode γ calorimeter mode γ Positron acceptance m 2.sr for E e+ >4 GeV 0.3 X 0 Gamma acceptance tracker mode: γ e + e - in the upper sub-detector 0.05 m 2.sr for [5-300] GeV calorimeter mode: no γ conversion until ECAL 0.08 m 2.sr for [10-300] GeV e + e - ~350 γ from galactic center during 1 year
34 264 2f/34 Unique Feature of AMS Combining searches in different channels could give (much) higher sensitiviy to SUSY DM signals
35 ORBITER SILL TRUNNIONS 264 2f/35
36 TRD In Assembly Upper TOF GPS Star Tracker Cryomagnet ACC Tracker Lower TOF In Assembly In Design In Assembly In Assembly In Assembly In Design, Manufacturing & Assembly In Assembly RICH In Manufacturing & Assembly ECAL In Testing
37 264 2f/37
38 264 2f/38
39 264 2f/39 TRD Performances 20 layer prototype tested with e -, μ -, π +, p + Proton rejection >10 2 reached up to 250GeV with 90% electron efficiency
40 Silicon Tracker All 8 planes, 300,000 channels have been produced Coordinator: R.Battiston Tracker on large 3D measuring machine 264 2f/40
41 AMS-02 Silicon Spectrometer Rigidity Resolution/ 264 2f/41 σ(1/r) = MDR = 2.5 TV Rigidity (GV)
42 264 2f/42
43 264 2f/43
44 264 2f/44
45 264 2f/45 Conclusions Cosmic Rays carry important informations about the non thermal universe AMS-02 has been designed to measure with ppb accuracy primary CR composition up the TeV region These accurate measurements will allow to undertand propagation and confinement mechanisms in our Galaxy The study of the rare components would allow to search for new phenomena (Dark Matter, strangelets) or to better constrain fundamental issues like the existence of primordial antimatter
46 Addressing fundamental questions aiming for a breakthrough Accelerator Original purpose Discovery AGS Brookhaven (1960) π N interactions 2 kinds of neutrinos, Breakdown of time reversal symmetry, 4-th Quark FNAL Batavia (1970) neutrino physics 5-th Quark, 6-th Quark SLAC Spear (1970) ep, QED Partons, 4-th Quark, 3rd electron PETRA Hamburg (1980) 6-th Quark Gluons Super Kamiokande (2000) Proton Decay Neutrino Oscillation Hubble Space Telescope AMS on ISS Galactic Survey Dark Matter Antimatter Curvature of the universe? y96402nac.ppt 264 2f/46
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