The AMS Experiment. S. Ting

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1 The AMS Experiment 1 15 April 2015 S. Ting

Welcome to the AMS Days at CEN Roberto BATTISTON, ASI, Trento Kfir BLUM, IAS, Princeton John ELLIS, King s College, London, CERN Jonathan FENG, UC Irvine Masaki FUKUSHIMA, Tokyo William GERSTENMAIER,

2 Welcome to the AMS Days at CEN Roberto BATTISTON, ASI, Trento Kfir BLUM, IAS, Princeton John ELLIS, King s College, London, CERN Jonathan FENG, UC Irvine Masaki FUKUSHIMA, Tokyo William GERSTENMAIER, NASA Francis HALZEN, Wisconsin Werner HOFMANN, MPI Heidelberg Gordon KANE, Michigan Peter F. MICHELSON, Stanford Igor V. MOSKALENKO, Stanford Angela OLINTO, Chicago Piergiorgio PICOZZA, INFN, Tor Vergata Vladimir S. PTUSKIN, IZMIRAN, Moscow Lisa RANDALL, Harvard Michael SALAMON, DOE Subir SARKAR, Oxford, Niels Bohr Inst. Eun-Suk SEO, Maryland Tracy SLATYER, MIT Edward C. STONE, Caltech Alan A. WATSON, Leeds Yue-Liang WU, UCAS/ITP, CAS Supported by: CERN, University of Geneva Fabio ZWIRNER, Padua, CERN 1 2

Fundamental discoveries have been made. B.

3 There are two kinds of cosmic rays traveling through space A. Neutral cosmic rays (light rays and neutrinos): have been measured for many years (Hubble, COBE, EGRET, WMAP, Planck, Fermi-LAT and Super Kamiokande, IceCube, HESS, ). Fundamental discoveries have been made. B. Charged cosmic rays: Following the pioneering experiments with balloons and satellites (ACE/CRIS, ATIC, BESS, CREAM, HEAT, PAMELA, ), 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. A+B. Physics of extreme high energy cosmic rays: Auger, TA, HESS-CTA, IceCube, JEM-EUSO. Fundamental Science on the ISS AMS 3

4 4

1.3m H/He ratio Pamela Results Proton and Helium spectra p He TOF(S1) ANTICOINCIDENCE TOF(S2) ANTICOINCIDENCE ANTICOINCIDENCE SPECTROMETER TOF(S3) O. Adriani et al.

5 1.3m H/He ratio Pamela Results Proton and Helium spectra p He TOF(S1) ANTICOINCIDENCE TOF(S2) ANTICOINCIDENCE ANTICOINCIDENCE SPECTROMETER TOF(S3) O. Adriani et al., PRL 102 (2009) Nature 458 (2009) 607 PRL 105 (2010) Astropart. Phys. 34 (2010) 1 PRL 105 (2010) Science, 332 (2011), 6025 PRL 111 (2013) Phys. Rep. (2014) Communication from Professor Piergiorgio Picozza S4 CALORIMETER NEUTRON DETECTOR 5

6 p/p 1 Pamela Results F(e + )/(F(e + )+ F(e - )) p flux [GeV m2 s sr] - e + flux x E 3 (s -1 sr -1 m -2 GeV 2 ) 6

7 6 300,000 electronic channels 650 processors 5m x 4m x 3m 7.5 tons 7

8 Tracker 8 AMS: A TeV precision, multipurpose spectrometer Particles and nuclei TOF are defined Z, E by their charge (Z) and energy (E ~ P) TRD Identify e +, e - Silicon Tracker Z, P ECAL E of e +, e Magnet ±Z RICH Z, E Z and P are measured independently by the Tracker, RICH, TOF and ECAL

AMS goals: He/He = 1/10 10, e + /p > 1/10 6 & Spectra to 1% 9 e + /p > 1/10 2 TRD Magnet e + /p = 1/10 4 ECAL a) Minimal material in the TRD and Tracker, so that the detector itself does not become a

9 AMS goals: He/He = 1/10 10, e + /p > 1/10 6 & Spectra to 1% 9 e + /p > 1/10 2 TRD Magnet e + /p = 1/10 4 ECAL a) Minimal material in the TRD and Tracker, so that the detector itself does not become a source of background nor of large angle scattering b) Repetitive measurements of momentum, to ensure that particles which had large angle scattering are not confused with the signal. c) e ± detectors are separated by magnetic field, so that secondary particles from TRD do not enter into ECAL.

AMS is a U.S. DOE sponsored international collaboration 10 CERN provided assembly, testing and the Control Center Strong support from R. Heuer, S. Lettow, S. Bertolucci, S. Myers, A.

10 AMS is a U.S. DOE sponsored international collaboration 10 CERN provided assembly, testing and the Control Center Strong support from R. Heuer, S. Lettow, S. Bertolucci, S. Myers, A. Siemko, FINLAND UNIV. OF TURKU USA MIT - CAMBRIDGE NASA GODDARD SPACE FLIGHT CENTER NASA JOHNSON SPACE CENTER UNIV. OF HAWAII UNIV. OF MARYLAND - DEPT OF PHYSICS YALE UNIVERSITY - NEW HAVEN MEXICO UNAM NETHERLANDS ESA-ESTEC NIKHEF FRANCE LUPM MONTPELLIER LAPP ANNECY LPSC GRENOBLE PORTUGAL LAB. OF INSTRUM. LISBON SPAIN CIEMAT - MADRID I.A.C. CANARIAS. SWITZERLAND ETH-ZURICH UNIV. OF GENEVA ITALY GERMANY RWTH-I. KIT - KARLSRUHE TURKEY METU, ANKARA ASI IROE FLORENCE INFN & UNIV. OF BOLOGNA INFN & UNIV. OF MILANO-BICOCCA INFN & UNIV. OF PERUGIA INFN & UNIV. OF PISA INFN & UNIV. OF ROMA INFN & UNIV. OF TRENTO RUSSIA ITEP KURCHATOV INST. KOREA EWHA KYUNGPOOK NAT.UNIV. CHINA CALT (Beijing) IEE (Beijing) IHEP (Beijing) NLAA (Beijing) SJTU (Shanghai) SEU (Nanjing) SYSU (Guangzhou) SDU (Jinan) TAIWAN ACAD. SINICA (Taipei) CSIST (Taipei) NCU (Chung Li)

DOE and NASA support Former NASA Administrator Dan Goldin has

Professors Jim Siegrist and Mike Salamon from DOE strongly

William Gerstenmaier has visited AMS more than 10 times, at CERN,

11 DOE and NASA support Former NASA Administrator Dan Goldin has supported AMS from the beginning. Professors Jim Siegrist and Mike Salamon from DOE strongly support AMS. Mr. William Gerstenmaier has visited AMS more than 10 times, at CERN, ESTEC, KSC. AMS has received strong support from the NASA-JSC team of Trent Martin, Ken Bollweg, Tim Urban, Phil Mott, Craig Clark and many others

12 Professors R. Battiston S.C. Lee S. Schael 12

5,248 straw tubes selected from 9,000, 2

13 Transition Radiation Detector (TRD) Identifies Positrons, Electrons by transition radiation and Nuclei by de/dx Completion of the TRD a 10 year effort 5,248 straw tubes selected from 9,000, 2 m length centered to 100mm. K. Luebelsmeyer, S. Schael 13

14 1/N dn/2 ADC One of 20 layers TRD performance on the Space Station Probability radiator electron proton p e ± Measurement with 1 of the 20 TRD Layers! Electrons Protons Transition Radiation ISS Data TRD estimator = -ln(p e /(P e +P p )) Normalized probability Amplitude [ADC] TRD likelihood = -Log 10 (P e ) TRD classifier = -Log 10 (P e )-2 14

15 Proton rejection at 90% e + efficiency TRD performance on the Space Station ISS data ε e 70% 80% 90% Rigidity (GV) 15

16 TRD Lifetime on the ISS Xe storage: 49kg CO 2 Storage: 5kg Lifetime: 5000g / 0.44g/d = 11364d = 31y 16

Palmonari H He Velocity [Rigidity>20GV] Velocity [Rigidity>20GV] Li Be B C N O F

17 Event s Event s Time of Flight System Measures Velocity and Charge of particles x10 3 Z = 2 s = 80ps Z = 6 s = 48ps Bologna Prof. A. Contin, G. Laurenti, F. Palmonari H He Velocity [Rigidity>20GV] Velocity [Rigidity>20GV] Li Be B C N O F Plane 4 Ne Mg Na Al Si P S Mn Cl Ar Ca Fe 3, K 4 Ti Sc V Cr Ni Zn Professors A. Zichichi and V. Bindi 17

18 Veto System rejects random cosmic rays Measured veto efficiency better than

19 2 1 Tracker 9 planes, 200,000 channels The coordinate resolution is 10 mm Laser rays ECAL Inner tracker alignment stability monitored with IR Lasers. The Outer Tracker is continuously aligned with cosmic rays in a 2 minute window 19

20 Tracker Perugia (R. Battiston, G. Ambrosi, B. Bertucci, ) and Geneva (M.Pohl, ) groups 20

21 Alignment accuracy of the 9 Tracker layers over 40 months 21

Particle Aerogel NaF Θ V Intensity Z 2 Z = 13 (Al) P = 9.

22 22 AMS Ring Imaging CHerenkov (RICH) Measurement of Nuclear Charge (Z 2 ) and its Velocity to 1/1000 Particle Aerogel NaF Θ V Intensity Z 2 Z = 13 (Al) P = TeV/c Z = 20 (Ca) P = TeV/c 22 Z = 26 (Fe) P = TeV/c

23 10,880 photosensors 23

24 Calorimeter (ECAL) Prof. F. Cervelli, M. Incagli, LAPP (S. Rosier, J.P. Vialle,..), IHEP (H. S. Chen, ) 50,000 fibers, f =1mm, distributed uniformly inside 600 kg of lead which provides a precision, 3-D, 17X 0 measurement of the directions and energies of e ± to TeV 24

25 Energy resolution (%) Fraction of events Calorimeter (ECAL): Test beams at CERN DQ 68 ( o ) 25 Energy(GeV) E beam (GeV) Electron/Proton Separation on ISS Boosted Decision Tree (BDT): 3D shower shape Data: GeV protons ε e = 90% electrons ECAL estimator

26 Proton rejection: 1. ECAL 3-D Shower Shape of e ± 2. P from the Tracker = E from ECAL Tracker Data from ISS 1 Tracker: P ECAL: E Rigidity (GV) 26

27 Extensive tests and calibration at CERN AMS 27 km 7 km θ Φ 19 January

28 AMS in SPS Test Beam, 2010 Particle Momentum (GeV/c) Positions Purpose Protons ,650 Full Tracker alignment, TOF calibration, ECAL uniformity Electrons 100, 120, 180, each TRD, ECAL performance study Positrons 10, 20, 60, 80, 120, each TRD, ECAL performance study Pions 20, 60, 80, 100, 120, each TRD performance to 1.2 TeV 28

29 Electronics 29 To get one board working on orbit, we needed to make ~10 boards In total: 464 boards on orbit of 70 different types. MIT team M.Capell A.Lebedev X.Cai A.Kounine V.Koutsenko Academia Sinica, Acad. S.C. Lee CSIST, General Hao Jinchi

30 May 16, 2011 May 16, 2011 CERN Director General visits KSC, April 4,

31 AMS Operations TDRS Satellites White Sands, NM 24 hours x 365 days x years ISS Astronaut with AMS Laptop M. Capell A. Lebedev A. Rozhkov POCC at CERN 24/7, 365d/y V. Koutsenko X. Cai J. Burger 31

ECAL Temperature changes from -10 o C to 30 o C over 9 months 20 o Large

32 Thermal Operations ECAL SDU (Prof. Cheng Lin) has made major contributions to the thermal operations 30 o Example: ECAL Temperature changes from -10 o C to 30 o C over 9 months 20 o Large temperature variations 10 o AMS has no control of the Space Station orientation 0 o C -10 o

33 In 4 years on ISS, AMS has collected >60 billion cosmic rays. To match the statistics, systematic errors studies have become important. 33

34 AMS is a very precise particle physics detector. The data was analysed by at least two independent AMS international teams V. Choutko A. Kounine J. Berdugo B. Bertucci M. Heil S. Schael M. Duranti H. Gast J. Casaus L. Derome M. Capell I. Gebauer M. Incagli S. Haino, A. Oliva M. Pohl P. Zuccon S. Rosier-Lees Z. Weng 34

35 35 AMS Data Analysis Conducted at the Science Operations Center at CERN and in the regional centers around the world. FZJ Juelich IN2P3 LYON CIEMAT MADRID GENEVA NLAA BEIJING SEU NANJING INFN MILANO BICOCCA CNAF INFN BOLOGNA ASDC ROME ACAD. SINICA TAIPEI

The isotropic proton flux Φ i for the i th rigidity bin (R i, R i +ΔR i ) is N i is the number of events, 300 million proton events have been selected; A i is the effective acceptance; ε i is the

36 The isotropic proton flux Φ i for the i th rigidity bin (R i, R i +ΔR i ) is N i is the number of events, 300 million proton events have been selected; A i is the effective acceptance; ε i is the trigger efficiency; T i is the collection time (which depends on the geomagnetic cutoff). To match the statistics, extensive systematic errors study has been made. To be presented by V. Choutko (MIT) 36

37 Systematic errors on the Proton Flux: 1) σ trig. :trigger efficiency 2) σ acc. : a. the acceptance and event selection b. background contamination c. geomagnetic cutoff 3) σ unf. a. unfolding b. the rigidity resolution function 4) σ scale. : the absolute rigidity scale 37

38 AMS proton flux AMS million events 38

39 AMS proton flux 39

40 AMS proton flux fit with two power laws: R, R +Δ with a characteristic transition rigidity R 0 and smoothness s Φ Φ Φ Solid curve fit of Eq. Φ to the data. (Fit to data above 45 GV: χ 2 /d.f.= 25 /26) Dashed curve uses the same fit values but with Δ set to zero. 40

41 Spectral Index AMS proton spectral index variation: Model independent measurement of spectral index = d log (Φ)/ d log (R) 41

42 Spectral index of the proton flux for 2011 to

Physics of 11 million e +, e - events Fraction of events Normalized

radiation) to identify e ± electron proton ISS data:83-100 GeV TRD

proton: E<p proton electron E/p ECAL (shower shape) to separate e ± from

43 Physics of 11 million e +, e - events Fraction of events Normalized entities Probability 43 Measuring electrons and positrons TRD (transition radiation) to identify e ± electron proton ISS data: GeV TRD estimator ISS data: GeV ECAL measures E Tracker measures p e ± : E=p proton: E<p proton electron E/p ECAL (shower shape) to separate e ± from protons Boosted Decision Tree, BDT: ISS data: GeV proton electron ε e =90% ECAL BDT

44 e + /(e + + e - ) 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+, p.. Collisions of Dark Matter (neutralinos, ) will produce additional e+, p, Positrons: + e + + m =400 GeV m =800 GeV Antiprotons: + p + m = 1 TeV I. Cholis et al., JCAP 0912 (2009) 007 e ± energy [GeV] Donato et al., PRL 102, (2009) To be presented by A.Kounine (MIT) To identify the Dark Matter signal we need 1. Measurement of e +, e and p. 2. Precise knowledge of the cosmic ray fluxes (p, He, C, ) 3. Propagation and Acceleration (Li, B/C, ) 44

45 Positron Fraction 45 AMS million e +, e - events

46 Verification of Positron Fraction with two independent samples Positron fraction analysis with TRD Only Positron fraction TRD ECAL Outside ECAL vs inside ECAL e - Good agreement between two independent samples 46

47 Positron Fraction from AMS 47

48 48 The energy beyond which it ceases to increase. 11 million e +, e - events Energy [GeV]

49 Positron fraction 0.2 The expected rate at which it falls beyond the turning point. Current status 0.15 Pulsars ±32 GeV m = 700 GeV 0.05 Collision of cosmic rays e ± energy [GeV] 49

50 Positron fraction The expected rate at which it falls beyond the turning point. In 10 years from now Pulsars 275±32 GeV m = 700 GeV Collision of cosmic rays e ± energy [GeV] 50

51 to be presented by Professor S. Schael (RWTH-Aachen) 51 Measurement of the flux of electrons and positrons N e± is the number of electron or positron events A eff is the effective acceptance ε trig is the trigger efficiency T is the exposure time

52 Electron flux (before AMS) 52

53 Electron Flux 53

54 Electron Flux 54

55 30 Positron flux (before AMS) See O. Adriani et al., PRL 111 (2013)

56 Positron Flux 56

57 Positron Flux 57

58 The Electron Flux and the Positron Flux spectral index = d log (Φ)/ d log (E) Observations: 1. The electron flux and the positron flux are different in their magnitude and energy dependence. 2. Both spectra cannot be described by single power laws. 3. The spectral indices of electrons and positrons are different. 4. Both change their behavior at ~30GeV. 5. The rise in the positron fraction from 20 GeV is due to an excess of positrons, not the loss of electrons (the positron flux is harder). 58

59 The (e + + e - ) flux before AMS 59

60 Combined (e + + e - ) Flux: event selection bending view TRD: identifies electron Tracker and Magnet: ECAL: identifies electron and measures its energy Independent of charge sign measurement no charge confusion High selection efficiency : TeV Small systematics on acceptance: TeV To be presented by Professor Bruna Bertucci (INFN-Perugia) 60

61 3 ) sr sec ] [ m F (GeV E AMS Results: (e + + e - ) flux 400 AMS-02 ATIC 350 BETS 97&98 PPB-BETS 04 Fermi-LAT 300 HEAT H.E.S.S. H.E.S.S. (LE) Energy Range: 0.5 GeV to 1 TeV Energy (GeV) 3 61

62 Spectral Index = d log (Φ)/ d log (E) 62

63 Φ(e + +e ) = C E γ= ± (stat + syst.) ± (energy scale) E > 30 GeV The flux is consistent with a single power law above 30 GeV. 63

64 Antiproton/proton ratio MAGNET AC C 1 TRD 2 Antiproton event: R = 423 GV Tracker 7-8 RICH 9 ECAL To be presented by A. Kounine (MIT) 64

65 AMS p/p results 65

66 AMS p/p results 66

67 AMS p/p results and modeling 67

68 The Origin of Dark Matter Collision of ordinary Cosmic Rays produce e+, p.. Collisions of Dark Matter (neutralinos, ) will produce additional e+, p, 11 million e +, e - events AMS p/p results and modeling e ± energy [GeV] To identify the Dark Matter signal we need 1. Measurement of e+, e, and p-bar. 2. Precise knowledge of the cosmic ray fluxes (p, He, C, ) 3. Propagation and Acceleration (Li, B/C, ) 68

69 Scattering 69 Three independent methods to search for Dark Matter AMS, Fermi-LAT, HESS, Annihilation e, p,,... LUX DARKSIDE XENON 100 CDMS II c c p, p,e -,e +,g p, p,e -,e +,g... p Production LHC p

70 SLAC partons, electroweak Scattering 70 Physics of electrons and protons SPEAR, DORIS, PEP, PETRA, LEP, Ψ, τ Annihilation e e p, p, e, e, e p, p,e -,e +,g e p, p,e -,e +,g... e e p p Production BNL, FNAL, LHC CP, J, Υ, t, Z, W, h 0

Tracker Measurement of Nuclei with AMS AMS: Multiple Independent Measurements of the Charge ( Z ) 1 1. Tracker Plane 1 2. TRD Carbon (Z=6) ΔZ (cu) 0.

71 Tracker Measurement of Nuclei with AMS AMS: Multiple Independent Measurements of the Charge ( Z ) 1 1. Tracker Plane 1 2. TRD Carbon (Z=6) ΔZ (cu) Upper TOF (1 counter) 4. Tracker Planes Lower TOF (1 counter) 6. RICH 7. Tracker Plane

72 AMS Nuclei Measurement on ISS H He Li Be B C N O F Ne Mg Na Al Si P S Cl Ar K Ca Sc Ti V Cr Mn Fe Co Ni To be presented by V. Choutko, L. Derome, S. Haino, M. Heil, A. Oliva 72

73 AMS Helium Flux 50 million events To be presented by S. Haino (Academia Sinica, Taiwan) 73

74 AMS Helium Flux 74

75 AMS Helium Flux Fit to data with Δγ=0 Solid curve fit of Eq. Φ to the data. (Fit to data above 45 GV: χ 2 /d.f.= 20.5 /27) Dashed curve uses the same fit values but with Δ set to zero. 75

76 Model Independent Spectral Indices Comparison = d log (Φ)/ d log (R) 76

77 proton/he flux ratio Φ p /Φ He = C R γ Single power law fit (R > 25 GV) AMS days - He flux 77 77

78 AMS Lithium flux current status AMS Orth et al (1978) Juliusson et al (1974) To be presented by L. Derome (LPSC, Grenoble) 78

79 Lithium flux with two power law fit Slope changes at about the same rigidity as for protons and helium 79

80 Boron-to-Carbon Orth et al. (1972) B/C Ratio Dwyer & Meyer ( ) Simon et al. ( ) HEAO3-C2 (1980) Webber et al. (1981) CRN-Spacelab2 (1985) Buckley et al. (1991) AMS-01 (1998) ATIC-02 (2003) CREAM-I (2004) TRACER (2006) PAMELA (2014) AMS-02 Exposure time of 40 months 7M Carbons, 2M Borons Rigidity (GV) Kinetic E To be presented by A. Oliva (CIEMAT) 80

81 Boron-to-Carbon Ratio B/C Ratio converted in Kinetic Energy AMS-02 PAMELA (2014) TRACER (2006) CREAM-I (2004) ATIC-02 (2003) AMS-01 (1998) Buckley et al. (1991) CRN-Spacelab2 (1985) Webber et al. (1981) HEAO3-C2 (1980) Simon et al. ( ) Dwyer & Meyer ( ) Orth et al. (1972) Fit to positron fraction by secondary production model Cowsik et al. (2014) Kinetic Energy (GeV/n) 3 81

82 In the past hundred years, measurements of charged cosmic rays by balloons and satellites have typically contained ~30% uncertainty. 82 AMS is providing cosmic ray information with ~1% uncertainty. The improvement in accuracy will provide new insights. The Space Station has become a unique platform for precision physics research.

83 The Origin of Dark Matter Collision of ordinary Cosmic Rays produce e+, p.. Collisions of Dark Matter (neutralinos, ) will produce additional e+, p, 11 million e +, e - events AMS p/p results and modeling e ± energy [GeV] To identify the Dark Matter signal we need 1. Measurement of e+, e, and p-bar. 2. Precise knowledge of the cosmic ray fluxes (p, He, C, ) 3. Propagation and Acceleration (Li, B/C, ) 83

84 The Electron Flux and the Positron Flux spectral index = d log (Φ)/ d log (E) Energy [GeV] Φ(e + +e ) = C E γ= ± (stat + syst.) ± (energy scale) E > 30 GeV 84

85 AMS proton flux Boron-to-Carbon Ratio 0.4 Boron-to-Carbon Boron-to-Carbon Lithium flux Orth et al. (1972) Dwyer & Meyer ( ) Simon et al. ( ) AMS Helium Flux HEAO3-C2 (1980) B/C Ratio Webber et al. (1981) CRN-Spacelab2 (1985) Buckley et al. Exposure (1991) time of 40 months 7M Carbons, 2M Borons AMS-01 (1998) ATIC-02 (2003) CREAM-I (2004) TRACER (2006) PAMELA (2014) AMS Rigidity (GV) Rigidity [GV] 85

$The latest AMS measurements of the positron fraction, the antiproton/proton ratio, the behavior of the fluxes of electrons, positrons, protons, helium, and other nuclei provide precise and unexpected$

86 The latest AMS measurements of the positron fraction, the antiproton/proton ratio, the behavior of the fluxes of electrons, positrons, protons, helium, and other nuclei provide precise and unexpected information. The accuracy and characteristics of the data, simultaneously from many different types of cosmic rays, require a comprehensive model to ascertain if their origin is from dark matter, astrophysical sources, acceleration mechanisms or a combination. 86

AMS Days at CERN The Future of Cosmic Ray Physics and Latest Results CERN, Main Auditorium, April 15-17, 2015 Wednesday, 15 April 2015 08:30-12:00 Chairman: R Heuer 08:30 R.

Schael, RWTH-Aachen The e Spectrum and e + Spectrum from AMS 11:45 Lunch 13:00-16:15 Chairman: F. Ferroni 13:00 F. Zwirner, Padova, CERN New Physics, Dark Matter and the LHC 14:00 J. L. Feng, UC Irvine Complementarity of Indirect Dark Matter Detection 15:00 I.

87 AMS Days at CERN The Future of Cosmic Ray Physics and Latest Results CERN, Main Auditorium, April 15-17, 2015 Wednesday, 15 April :30-12:00 Chairman: R Heuer 08:30 R. Heuer, CERN Welcome 09:00 S. Ting, CERN, MIT Introduction to the AMS Experiment 10:00 A. Kounine, MIT Latest AMS Results: The Positron Fraction and the p-bar/p ratio 11:00 Break 11:15 S. Schael, RWTH-Aachen The e Spectrum and e + Spectrum from AMS 11:45 Lunch 13:00-16:15 Chairman: F. Ferroni 13:00 F. Zwirner, Padova, CERN New Physics, Dark Matter and the LHC 14:00 J. L. Feng, UC Irvine Complementarity of Indirect Dark Matter Detection 15:00 I. V. Moskalenko, Stanford Cosmic Rays in the Milky Way and Other Galaxies 16:00 Break 16:15-18:15 Chairman: H. Schopper 16:15 K. Blum, IAS, Princeton It's about time: interpreting AMS antimatter data in terms of cosmic ray propagation 17:00 V. S. Ptuskin, IZMIRAN Acceleration and Transport of Galactic Cosmic R 18:00 Break 18:15 R. Heuer 18:15 W. Gerstenmaier, NASA Public Lecture: Human Space Exploration AMS 08:30 B. Bertucci, Perugia The (e plus e + ) Spectrum from AMS 09:00 V. Choutko, MIT The Proton Spectrum from AMS 09:30 S. Haino, Academia Sinica, Taiwan The Helium Spectrum from AMS 10:00 Break 10:15 L. Randall, Harvard Indirect Detection: Enhanced Density Models and Antideuteron Searches 11:15 S. Sarkar, Oxford, Niels Bohr Inst. Background to Dark Matter Searches from Galactic Cosmic Rays 12:15 Lunch 08:00 T. Slatyer, CTP, MIT Scrutinizing Possible Dark Matter Signatures with AMS, Fermi, and Planck 08:30 J. R. Ellis, King s College, London, CERN Super-symmetric Dark Matter 09:30 A. Oliva, CIEMAT AMS Results on Light Nuclei - B/C 09:45 L. Derome, LPSC, Grenoble AMS Results on Light Nuclei - Li 10:00 M. Heil, MIT AMS Results on Light Nuclei - C/He 10:15 Break 10:30 Y. L. Wu, UCAS/ITP, CAS Implications of AMS02 Experiment 11:15 A. Olinto, Chicago The Highest Energy Cosmic Particles 12:15 M. Fukushima, Tokyo Recent Results on Ultra-High Energy Cosmic Rays from the Telescope Array 12:45 Lunch Thursday, 16 April :30-12:45 Chairman: F. Linde 14:00-18:15 Chairman: Y.F. Wang Friday, 17 April :00 P. Picozza, INFN, Rome Tor Vergata The JEM-EUSO Program 15:00 F. Halzen, Wisconsin Latest Results from Ice Cube 16:00 Break 16:15 A. Watson, Leeds Latest Results from the Pierre Auger Observatory and Future Prospects in particle physics and high energy astrophysics with cosmic rays 17:15 P. Michelson, Stanford Latest Results from Fermi-LAT 18:15 Break 18:30 E. C. Stone, Caltech Public Lecture: The Odyssey of Voyager 08:00-10:15 Chairman: A. Yamamoto 13:30-17:45 Chairman: J. Trümper 10:30-12:45 Chairman: F. Gianotti 18:15 S. Ting 13:30 E.-S. Seo, Maryland Cosmic Ray Energetics and Mass: From Balloons to the ISS 14:30 W. Hofmann, MPI Heidelberg Latest Results from HESS and the Progress of CTA 15:30 G. Kane, Michigan Are there currently well-motivated and phenomenologically allowed dark matter candidates (besides axions) 16:30 Break 16:45 M. Salamon, DOE The Cosmic Frontier at DOE 17:15 R. Battiston, ASI, Trento What next in fundamental and particle physics in space? 17:45 S. Ting, MIT, CERN Summary Contact: Ms. Laurence Barrin <laurence.barrin@cern.ch>

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Recent&results&from&the&Alpha&Magne4c& Spectrometer&(AMS)&Experiment&& on&the&interna4onal&space&sta4on Federico Pilo - INFN Pisa Vulcano, May 19 th 2014 3 Experimental Challenges Search for Dark Matter