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The Latest Results from The Alpha Magnetic Spectrometer on the International Space Station June 17, 2014 S. Ting AMS: a U.S. DOE led International Collaboration 15 Countries, 44 Institutes and 600 Physicists FINLAND UNIV. OF TURKU RUSSIA ITEP NETHERLANDS KURCHATOV INST. ESA-ESTEC GERMANY NIKHEF RWTH-I. KIT - KARLSRUHE KOREA USA FRANCE EWHA MIT - CAMBRIDGE LUPM MONTPELLIER KYUNGPOOK NAT.UNIV. NASA GODDARD SPACE FLIGHT CENTER LAPP ANNECY CHINA NASA JOHNSON SPACE CENTER LPSC GRENOBLE TURKEY CALT (Beijing) UNIV. OF HAWAII METU, ANKARA IEE (Beijing) UNIV. OF MARYLAND - DEPT OF PHYSICS IHEP (Beijing) YALE UNIVERSITY - NEW HAVEN PORTUGAL SWITZERLAND ETH-ZURICH NLAA (Beijing) LAB. OF INSTRUM. LISBON UNIV. OF GENEVA SJTU (Shanghai) SEU (Nanjing) SPAIN SYSU (Guangzhou) CIEMAT - MADRID SDU (Jinan) I.A.C. CANARIAS. ITALY TAIWAN ASI ACAD. SINICA (Taipei) IROE FLORENCE CSIST (Taipei) MEXICO INFN & UNIV. OF BOLOGNA NCU (Chung Li) INFN & UNIV. OF MILANO-BICOCCA UNAM INFN & UNIV. OF PERUGIA INFN & UNIV. OF PISA INFN & UNIV. OF ROMA INFN & UNIV. OF TRENTO D. Goldin, former NASA Administrator realized the unique potential of ISS for fundamental science and has supported AMS from the beginning May 16, 2011 May 15, 2011 May 09, 1994 NASA support Mr. William Gerstenmaier has visited AMS regularly More than 10 times, at CERN, KSC, ESTEC . Mr. Mike Suffredini and Mr. Rod Jones have also strongly supported AMS. Their support has made it possible for AMS to collect data continuously The construction of AMS was, and AMS operations are, supervised continuously by NASA-JSC team of Trent Martin, Ken Bollweg and many others. 4 Strong support of STS-134 astronauts (Mark Kelly, Gregory H. Johnson, Michael Fincke, Roberto Vittori, Andrew J. Feustel, Gregory Chamitoff) Development of Accelerators 1612 2014 Energy: 0.0001 eV Energy: 7,000,000,000,000 eV = 7 TeV Galileo’s work on Gravity Study fundamental building blocks of nature Largest Accelerator on Earth (LHC) can produce particles of 7 TeV Italy the Alps CERN LHC Accelerator circumference 16 miles However, Cosmic Rays with energies of 100 Million TeV have been observed. The highest energy particles are produced in the cosmos JEM-EUSO (A. OLINTO) Extreme Universe Space Observatory (EUSO) in the Japanese Experiment Module (JEM) •Ultraviolet telescope to study origin + interactions of Extreme Energy Cosmic Rays (EECR) with E ~ 1020 eV 8 •ISS provides10 x more exposure than ground observatories. Study of Extreme Energies Sources and Interactions JEM-EUSO knee ankle 1020 eV In the 21st Century, We enjoy unprecedented advancements in technological development such as in the fields of communication, computers, transportation, medicine, etc … which have had dramatic effects on the quality of life. 203 A/p10 10 Fundamental Research and Advancements in Technology Television Radio Super Aircraft Manned conductivity Space Laser Photography Stations Neon tube Steam engine Skylab Fusion Transistor Steam turbine Prospecting Nuclear Semi conductor Electromagn. Weather Navigation p - beams reactors X rays Time Keeping Isotope techn. Satellites Pulsars in Medecine Solid State Nuclear Fission Big Bang Physics m - Chemstry Optics Stable Black Holes 2 Tides (exotic Matter ?)SU(3) -Symm E = m• c Cosmic Background Quantum Thermo- Symmetry Radiation radiation Radioactivity mechanics dynamics Comets Strangeness Models of Models of the QCD Sun Quasars Radius p, n Atomic Nuclei Atom Mechanics Kopernicus Classical Quarks Particles Nuclei Atoms Physics Planets Stars Galaxies 10-17m 10-16m 10-14m 10-10m 1m 1011m 1017m 1025m CERN Space Station Higgs particle Space Medicine and Biology www Particle Physics 6 15ft x 12ft x 9ft 7.5 tons Fundamental Science on the International Space Station (ISS) There are two kinds of cosmic rays traveling through space 1- Neutral cosmic rays (light rays): have been measured for many years (Hubble, COBE, Planck, WMAP…). Fundamental discoveries have been made. 2- Charged cosmic rays: Using a magnetic spectrometer (AMS) on ISS is a unique way to provide precision long term (10-20 years) measurements of primordial high energy charged cosmic rays. AMS AMS: A TeV precision, multipurpose spectrometer Transition Radiation Detector Identify electrons Particles are defined by their Time of Flight Z, E charge (Z) and energy (E) or momentum (P) 1 Magnet ±Z Silicon Tracker Z, P 2 3-4 5-6 7-8 Tracker Ring Imaging Cherenkov Z, E Electromagnetic Calorimeter 9 E of electrons The Charge and Energy (momentum) are measured independently by many detectors 14 Tests and calibration at CERN AMS in accelerator test beams Feb 4-8 and Aug 8-20, 2010 27 km AMS 7 km p, e+, e-,π 10-400 GeV θ 2000 positions Φ 19 January 2010 15 May 19, 2011: AMS installation completed. In 3 years we have collected 50 billion events. This is much more than all Cosmic Rays collected over last century. Administrator Charles Bolden inaugurated AMS Payload and Science Operations Centers (POCC), June 23, 2011 17 The physics objectives of AMS include: The Origin of Dark Matter ~ 90% of Matter in the Universe is not visible and is called Dark Matter Collision of “ordinary” Cosmic Rays produce e+, ... Collisions of Dark Matter (neutralinos, ) will produce additional e+, … ) - m=800 GeV + e + m=400 GeV /(e + e I. Cholis et al., arXiv:0810.5344 e± energy [GeV] M. Turner and F. Wilczek, Phys. Rev. D42 (1990) 1001 The e+ /(e+ + e-) = positron fraction decreases up to 10 GeV, as expected, but from 10 to ~250 GeV is steadily increasing + − Positron fraction AMS-02 (6.8 million e , e events) 2013 e± energy [GeV] AMS Positron Fraction 2013 Low energy measurements include HEAT, CAPRICE, TS93 … 20 Comparison with theoretical Dark Matter Models AMS-02 data on ISS 6.8 million e± events, PRL 110, 141102 (2013) m=800 GeV m=400 GeV 0.1 ) - + e + /(e + e Dark Matter model based on I. Cholis et al., arXiv:0810.5344 10 102 e± energy [GeV] On the origin of excess positrons If the excess has a particle physics origin, it should be isotropic Galactic coordinates (b,l) Significance ( ) The fluctuations of the positron ratio e+/e− are isotropic. The anisotropy in galactic coordinates: δ ≤ 0.030 at the 95% confidence level 22 From: Matteo Rini [[email protected]] Sent: 02 January 2014 19:09 To: Samuel Ting Subject: your AMS paper as a 2013 Physics Highlights Dear Sam, this is just to let you know that your article the first AMS data has been selected in our 2013 APS Physics Highlights (http://physics.aps.org/articles/v6/139). Congratulation on this work, which has generated a lot attention among our readers, the press and the scientific community. Best regards, One year Matteo -- Matteo Rini, PhD Deputy Editor, Physics [email protected] http://physics.aps.org 25 Positron Fraction compared with Collision of Cosmic Rays plus Dark Matter or Pulsar models Pulsars Positron fraction Positron m=700 GeV e± energy [GeV] 26 Comment: 3 independent methods to search for Dark Matter Annihilation (in Space) e , p, ,... Scattering AMS (Underground Experiments c p, p,e-,e+,g World Wide): LUX DARKSIDE XENON 100 c p, p,e-,e+,g CDMS II … LHC p p Production (in Accelerators) Physics of electrons and protons Annihilation e e p, p,e,e , SPEAR, PEP, PETRA, LEP, … Ψ, τ - + e p, p,e ,e ,g , electroweak - + Scattering partons e p, p,e ,e ,g SLAC … SLAC BNL, FNAL, LHC …CP, J, Υ, T, Z, W, h0 ... e e p p Production Latest AMS Results and Future Plans Cosmic rays Dark Matter Future Plans Proton spectrum Positron Fraction Positron Fraction Helium spectrum Anisotropy Anisotropy Electron Spectrum Positron Flux Antiproton Ratio Boron Spectrum Antiproton Ratio Photons Carbon Spectrum Antimatter Search Boron/Carbon ratio Strangelets Search Oxygen AMS Data Analysis Centers FZJ – Juelich (2300 cores) AMS@CERN – GENEVA (4000 cores) IN2P3 – LYON (400 cores) CNAF – INFN BOLOGNA (1300 cores) NLAA – BEIJING (1024 cores) CIEMAT – MADRID (200 cores) SEU – NANJING (2016 cores) ACAD. SINICA – TAIPEI (3000 cores) New Results on Positron Fraction 1. At much higher energy (up to 500 GeV) AMS 2014 • Positron fraction Positron e± energy [GeV] 2. With much higher statistics AMS 2014 • 11 million positron-electron events AMS 2013 • Positron fraction Positron PAMELA Δ Fermi 6.8 million positron-electron events e± energy [GeV] 3. Above 206 GeV, Positron Fraction is independent of e ± energy In the energy region 206 – 500 GeV, we fit the Positron Fraction with a straight line equation: positron fraction = a+b·E then b = -(2.6 ± 18.4) 10-5 AMS 2014 • Positron fraction Positron e± energy [GeV] New Positron Fraction results compared with models AMS 2014 • Pulsars Positron fractionPositron e± energy [GeV] 33 New Position Fraction Results compared with Minimal Model −e+ −s -E/Es AMS Fe+ = Ce+ E + CsE e −e- −s -E/Es Minimal Model Fe- = Ce- E + CsE e -1 1/Es = 1.48 ± 0.59 TeV Positron fraction Positron e± energy [GeV] Positron Flux Data (before AMS) Fermi data above 126 GeV are off scale. New AMS Results: Measurement of Positron Flux. The Positron Flux exhibits 3 unexpected behaviours 1. The flux increases up 2. From 10-35 Gev, 3. Above 35 GeV, there to 10 GeV it is nearly flat is a structure AMS Positron Flux Data Comparison with early work Fermi data above 100 GeV are off scale Electron flux measurement before AMS AMS Electron flux measurement compared with early work 39 (e+ + e−) flux measurement before AMS AMS (e+ + e−) flux - New Understanding In the past hundred years, measurements of charged cosmic rays by balloons and satellites have typically contained ~30% uncertainty. AMS will provide cosmic ray information with ~1% uncertainty. The 30 times improvement in accuracy will provide new insights. The Space Station has become a unique platform for precision physics research.
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