The Alpha Magnetic Spectrometer Experiment AMS AMS Guoming

The Alpha Magnetic Spectrometer Experiment (AMS) AMS Guoming Chen IHEP Beijing

AMS: A Te. V (1012 e. V) Magnetic Spectrometer in Space 3 m x 3 m, 7 t, ~ 0. 5 m 2 sr +y 03 K 193_2 ea

AMS is an international collaboration of 16 countries, 60 institutes and 500 physicists. FINLAND HELSINKI UNIV. OF TURKU DENMARK NETHERLANDS USA UNIV. OF AARHUS CIEMAT - MADRID I. A. C. CANARIAS. MEXICO UNAM PORTUGAL LAB. OF INSTRUM. LISBON I. K. I. ITEP KURCHATOV INST. MOSCOW STATE UNIV. GERMANY ESA-ESTEC NIKHEF NLR FLORIDA A&M UNIV. JOHNS HOPKINS UNIV. MIT - CAMBRIDGE FRANCE NASA GODDARD SPACE FLIGHT CENTER GAM MONTPELLIER NASA JOHNSON SPACE CENTER LAPP ANNECY TEXAS A&M UNIVERSITY LPSC GRENOBLE UNIV. OF MARYLAND-DEPRT OF PHYSICS UNIV. OF MARYLAND-E. W. S. S. CENTER YALE UNIV. - NEW HAVEN SPAIN RUSSIA RWTH-III MAX-PLANK INST. UNIV. OF KARLSRUHE ROMANIA ISS UNIV. OF BUCHAREST SWITZERLAND ETH-ZURICH UNIV. OF GENEVA 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 KOREA EWHA KYUNGPOOK NAT. UNIV. CHINA BISEE (Beijing) IHEP (Beijing) SJTU (Shanghai) SEU (Nanjing) SYSU (Guangzhou) SDU (Jinan) ACAD. SINICA (Taiwan) AIDC (Taiwan) CSIST (Taiwan) NCU (Chung Li) NCKU (Tainan) NCTU (Hsinchu) NSPO (Hsinchu) 95% of the $1. 5 B to build AMS has come from our international partners based on NASA’s commitment to deploy AMS on the ISS.

First flight AMS-01 Approval: April 1995, Assembly: December 1997, Flight: 10 days in June 1998 AMS y 96207_05 b

Unexpected results from first flight: 1 - the existence of two Spectra in proton flux 0. 8< M<0. 9 Expected Spectra due to Earth’s magnetic field . 7 M <0 . 3 M <0 . 5 M 4< 6< 0. <0 0. Flux (m 2 sec sr Me. V)-1 1. 0< M<1. 1 Phys. Lett. B 472 (26 Jan 2000) 215 -226

Unexpected results from first flight: 2 - There are many more positrons (e+) than electrons (e-) Second Spectra Geomagnetic latitude (radians) Phys. Lett. B 484 (27 Jun 2000) 10 -22

Unexpected results from first flight: 3 - He 4 and He 3 isotopes are completely separated in space 80 100 3. 650± 0. 09 Energy/2 He 4 Events 60 10 1 -0. 8 40 -0. 4 0 ΘM 0. 4 0. 8 M 40 20 Events 30 0 5 (Ge. V) 10 20 10 0 1 2 3 4 Mass (Ge. V) 5 6 Phys. Lett. B 494 (2000) 193 -202 These results were not predicted by any cosmic ray model

Construction of the AMS-02 Superconducting magnet Dipole Coils (2 x) Racetrack Coils (2 x 6) 0. 86 T 2, 500 l Superfluid He Duration: 3 -5 years

Transition Radiation Detector: TRD Identify e+, reject P works for 20 y 20 layers

5248 tubes BEAM TEST at CERN Design rejection

Time of Flight (TOF) Measures the time of particles to ~ 100 picoseconds Charge measurement up to Z=26 with de/dx AMS Tracker RICH ECAL He Vessel Superconducting Magnet TOF Coils Cryocooler TRD TOF

Silicon Tracker, 8 planes TRD (5248 channels) 2500 L SF Helium Tracker (200000 channels) Superconducting Magnet TOF RICH (10880 channels ) ECAL (1300 ch. 12

200 000 channels alignment 3 m S side Test results from CERN identify all nuclei simultaneously K side 13

AMS Ring Imaging CHerenkov (RICH) Precise measurement of the velocity & charge Charge Z Velocity Particle Cerenkov Radiator Conical Reflector Photodetectors 10, 880 photodetectors

RICH test beam E=158 Ge. V/n Δv/v = 0. 001 charge measurement up to 30 Z (1 -v/c)/1000 (1 - )/1000 He Li C O Single Event Displays Ca

ECAL: A measurement of the direction & energy of gamma rays and electrons TRD (5248 channels) 2500 L SFHelium Tracker (200000 channels) Superconducting Magnet TOF RICH (10880 channels ) ECAL (1300 ch. Cut-away view of fibers and lead Completed Flight Module e, γ p

ECAL capability Complementary with TRD, ECAL can reject hadron by a factor of 200 at high energy

Accelerator testing of AMS and components Tandem heavy ion Van de Graff, Catania High intensity proton cyclotron, Indiana Heavy ion accelerator, Darmstadt High energy proton and ion accelerator, Geneva

Results from accelerator tests He Number of Events Li B C Be N O Simultaneous measurement of all nuclei Ne Mg F Na Al Si P S Cl Ar Ca K Sc. Ti VCr Mn Fe “Hubble telescope” Co for charged particle Atomic Number 103 Δv/v = 0. 001 1500 Events/20 ps 10 Events 102 Events Δx = 10 µm Δ t = 100 ps 2500 -2 1 y 04 K 513_05 (1 - )/1000 -1 0 1 2 Time of Flight (ns)

Cosmic test early 2008, every piece works well

AMS 02 Cosmic Test

Space qualification Testing in 2008 LARGE SPACE SIMULATOR AT ESA The detector is on schedule to be sent to KSC in early 2009

Search for Antimatter in the Universe AMS in Space Se arc AMS hf se or the ex is ten ce of r Accelerators an ti U niv e rse n igi or f h o e h t c r ea S The Big Bang origin of the Universe requires matter and antimatter to be equally abundant at the very hot beginning o e f th U er v i n

Experimental work on Antimatter in the Universe Direct search AMS-01 Results negative AMS-02 Increase in sensitivity: x 103 – 106 Increase in energy to ~Te. V y 06 K 299 a Baryogenesis conditions Search for new CP BELLE Ba. Bar FNAL KTe. V CERN NA-48 CDF, D 0 LHC-b ATLAS CMS Search for Proton decay LVD, ICARUS, Super K, … Major worldwide efforts with negative results

AMS-02 Antihelium Limits He/He (CL 95%) Current antimatter searches are limited y 06 K 301

2 x 109 nuclei If no antimatter is found => there is no antimatter within ~ 1000 Mpc. Other possible solutions: The existence of a new source of CP Violation The existence of Baryon, Lepton Number Violation Grand Unified Theory Electroweak Theory SUSY the Foundations of Modern Physics These are central research topics for the current and next generation of accelerators world wide

Indirect dark matter search 8 Space avoid contamination from atmospheric secondaries 8 Multichannel analysis

Dark Matter Search Through Positron Assume HEAT excess come from χ

A leading theoretical candidate for Dark Matter A supersymmetric particle with Mχ = 840 Ge. V. 10 -3 P/P Spectra with Dark Matter 10 -4 Normal spectra for anti-proton/proton 10 -5 1 10 100 Kinetic Energy (Ge. V)

Dark Matter Search Through Antiproton

Dark matter search through high energy diffuse gammas g T. Prodanovi´c et al. , astro-ph/0603618 v 1 22 Mar 2006 Space Experiments Ground Experiments EGRET up p e− e+ P− P+ er lim AMS-02 E− E+ Unique constraints P+ = E + = P − = E − The diffuse gamma-ray spectrum of the Galactic plane 40 o < 100 o, |b| < 5 o 1. Pointing precision of 2 arcsec 2. UTC time (from GPS, μsec accuracy) allows to relate AMS measurements with other missions its

Precision study of the properties of Cosmic Rays Composition at different energies (1 Ge. V, 100 Ge. V, 1 Te. V) Charge measurement up to 30 (s-1 m-2 sr-1 Ge. V-1) 104 H 101 He Li Be B C N O 10 -2 F 10 -5 Ne Na 10 -8 Mg Al Si P 10 -11 S Cl Ar K Ca Sc 1 Ti V Cr Mn Fe Co Ni 5 10 Z 15 20 Isotope measurement: D/P, He(3)/He(4), Be(9)/Be(10)… 25 100 10 /n E kin 1000 1 e. V (G 0. 1 )

Proton Flux up to 2 Te. V

Helium Flux up to 1 Te. V/Nuc

Electron Flux up to 1 Te. V

3 He/4 He Ratio Measurement

B/C measurement relative fluxes regardless of the magnetic field AMS will measure the ratio B/C up to and collect after 3 years 105 C with E > 100 Ge. V/A 104 B with E > 100 Ge. V/A

10 Be / 9 Be Measurement C. Mana i) the cosmic ray confinement time in the galaxy, ii) the mean density of interstellar material traversed by cosmic rays. One of the most important measurements in cosmic ray physics y 01 K 22 ge. ppt

Background determination for dark matter search The precise measurement of all the nuclei and their isotopes will provide stringent constraint on cosmic propagation models, which will in turn give precise background prediction for positron, anti-proton and gamma rays

Conclusion • • • AMS 02 has been built and tested, ready to be launched Search for anti-Helium at the sensitivity of 10 -9, will exclude anti-matter within Billion pc Search for dark matter through positron, antiproton and gamma spectrum Precise measurement of nuclei and their isotopes up to z=30 will provide precise prediction of background for dark matter search Global fitting of the positron, anti-proton and gamma rays worldwide may give a hint to the solution of dark matter