the ams experiment

The AMS Experiment

S. Ting 15 April 2015

1

1

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 Fabio ZWIRNER, Padua, CERN

Welcome

to the AMS Days at CEN

Supported by: CERN, University of Geneva 2

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.

There are two kinds of cosmic rays traveling through space

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.

AMS

Fundamental Science on the ISS

3

A+B. Physics of extreme high energy cosmic rays: Auger, TA, HESS-CTA, IceCube, JEM-EUSO

….

Proton and Helium spectra

H/H

e r

ati

o

p

He

Pamela Results

O. Adriani et al.,

PRL 102 (2009) 051101

Nature 458 (2009) 607

PRL 105 (2010) 121101

Astropart. Phys. 34 (2010) 1

5 Communication from Professor Piergiorgio Picozza

PRL 105 (2010) 121101

Science, 332 (2011), 6025

PRL 111 (2013) 081102

Phys. Rep. (2014)

TOF(S1)

TOF(S3)

CALORIMETER

NEUTRON

DETECTOR

ANTICOINCIDENCE

ANTICOINCIDENCE

ANTICOINCIDENCE

S4

SPECTROMETER

TOF(S2)

1.3

m

p/p

p

flu

x [

GeV

m2 s

sr]

-

1

F(e

+)/

(F(e

+)+

F(e

- ))

e+ f

lux x

E3 (

s-1

sr-

1 m

-2 G

eV

2)

6

Pamela Results

6

5m x 4m x 3m 7.5 tons

300,000 electronic

channels 650 processors

7

Tra

cker

1

2

7-8

3-4

9

5-6

TRD Identify e+, e-

Silicon Tracker Z, P

ECAL E of e+, e-

RICH Z, E

TOF Z, E

Particles and nuclei

are defined

by their charge (Z)

and energy (E ~ P)

Z and P are measured independently by the

Tracker, RICH, TOF and ECAL

AMS: A TeV precision, multipurpose spectrometer

Magnet ±Z

8

TRD

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 goals: He/He = 1/1010, e+/p > 1/106 & Spectra to 1%

Magnet

e+/p > 1/102

e+/p = 1/104

9

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

FINLAND

UNIV. OF TURKU

FRANCE

LUPM MONTPELLIER

LAPP ANNECY

LPSC GRENOBLE

GERMANY

RWTH-I.

KIT - KARLSRUHE

ITALY

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

NETHERLANDS

ESA-ESTEC

NIKHEF

RUSSIA

ITEP

KURCHATOV INST.

SPAIN

CIEMAT - MADRID

I.A.C. CANARIAS.

SWITZERLAND

ETH-ZURICH

UNIV. OF GENEVA

CHINA

CALT (Beijing)

IEE (Beijing)

IHEP (Beijing)

NLAA (Beijing)

SJTU (Shanghai)

SEU (Nanjing)

SYSU (Guangzhou)

SDU (Jinan)

KOREA

EWHA

KYUNGPOOK NAT.UNIV.

PORTUGAL

LAB. OF INSTRUM. LISBON

ACAD. SINICA (Taipei)

CSIST (Taipei)

NCU (Chung Li)

TAIWAN

TURKEY

METU, ANKARA

10

AMS is a U.S. DOE sponsored international collaboration

CERN provided assembly, testing and the Control Center

Strong support from R. Heuer, S. Lettow, S. Bertolucci, S. Myers, A. Siemko, …

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.

11 11

12

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

5,248 straw tubes selected from 9,000, 2 m length centered to 100mm.

K. Luebelsmeyer, S. Schael

Transition Radiation Detector (TRD) Identifies Positrons, Electrons by transition radiation and Nuclei by dE/dx

Completion of the TRD a 10 year effort

13

TRD performance on the Space Station

14

On

e o

f 20 l

ayers

radiator

e± p

electron proton

TRD classifier = -Log10(Pe)-2

TRD likelihood = -Log10(Pe)

0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2

TRD estimator = -ln(Pe/(Pe+Pp))

10-1

10-2

10-3

10-4

10-5

10-6

10-7

Pro

bab

ilit

y

Normalized probability

Protons

Electrons

Measurement with 1 of the 20 TRD Layers !

Transition Radiation

ISS Data

1/N

dn

/2 A

DC

10-2

10-3

10-4

10-5

Amplitude [ADC]

0 200 400 600 800 1000 1200 1400

Pro

ton

reje

cti

on

at

90%

e+ e

ffic

ien

cy

Rigidity (GV)

• ISS data

TRD performance on the Space Station

70%

80%

90%

εe

15

16

Xe storage: 49kg CO2 Storage: 5kg Lifetime: 5000g / 0.44g/d = 11364d = 31y

TRD Lifetime on the ISS

Time of Flight System

Measures Velocity and Charge of particles

x103

Velocity [Rigidity>20GV]

Eve

nt

s

Velocity [Rigidity>20GV]

Eve

nt

s

Plane 4

3, 4

H He

Li Be B C

N O

F Ne

Na Mg

Al Si

Cl Ar K Ca

Sc Ti V P S

Cr Fe

Ni

Mn

Zn

Bologna Prof. A. Contin, G. Laurenti, F. Palmonari

17

Professors A. Zichichi and V. Bindi

Z = 2

s = 80ps

Z = 6

s = 48ps

Veto System rejects random cosmic rays

Measured veto efficiency better than 0.99999 18

Inner tracker alignment stability

monitored with IR Lasers.

The Outer Tracker is continuously aligned

with cosmic rays in a 2 minute window

1

5

6

3

4

7

8

9

2

ECAL

Laser rays

Tracker

9 planes, 200,000 channels

The coordinate resolution is 10 mm.

19

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

Tracker

20

Alignment accuracy of the 9 Tracker layers over 40 months

21

22

Measurement of Nuclear Charge (Z2) and its Velocity to 1/1000

Particle

AMS Ring Imaging CHerenkov (RICH)

Θ

Intensity ⇒ Z2

⇒ V

Aerogel NaF

22

Z = 13 (Al) P = 9.148 TeV/c Z = 20 (Ca)

P = 2.382 TeV/c

Z = 26 (Fe) P = 0.795 TeV/c

23

10,880

photosensors

50,000 fibers, f =1mm, distributed uniformly inside 600 kg of lead

which provides a precision, 3-D, 17X0 measurement

of the directions and energies of e± to TeV

Calorimeter (ECAL)

Prof. F. Cervelli, M. Incagli,

24

LAPP (S. Rosier, J.P. Vialle,..),

IHEP (H. S. Chen, …)

Calorimeter (ECAL): Test beams at CERN

25

Boosted Decision Tree (BDT):

3D shower shape

protons electrons

εe = 90%

Data: 83–100 GeV

ECAL estimator

Fra

cti

on

of

even

ts

Energy(GeV) E beam (GeV)

Electron/Proton Separation on ISS

En

erg

y r

eso

luti

on

(%

)

DQ

68(o

)

Proton rejection: 1. ECAL 3-D Shower Shape of e±

2. P from the Tracker = E from ECAL

26 Rigidity (GV)

Tra

cker

1

2

7-8

3-4

9

5-6

Tracker: P

ECAL: E

Data from ISS

Extensive tests and calibration at CERN

AMS 27 km

7 km

19 January 2010

θ

Φ

27

Particle Momentum (GeV/c) Positions Purpose

Protons 400 + 180 1,650

Full Tracker alignment,

TOF calibration,

ECAL uniformity

Electrons 100, 120, 180, 290 7 each TRD, ECAL performance study

Positrons 10, 20, 60, 80, 120, 180 7 each TRD, ECAL performance study

Pions 20, 60, 80, 100, 120, 180 7 each TRD performance to 1.2 TeV

AMS in SPS Test Beam, 2010

28

Academia Sinica, Acad. S.C. Lee

CSIST, General Hao Jinchi

To get one board working on orbit, we needed to make ~10 boards

In total: 464 boards on orbit of 70 different types.

A.Lebedev V.Koutsenko X.Cai M.Capell A.Kounine

MIT team

29

Electronics

May 16, 2011

May 16, 2011

30

CERN Director General

visits KSC, April 4, 2011

AMS Operations

White Sands, NM

TDRS Satellites

A. Lebedev M. Capell

V. Koutsenko X. Cai

24 hours

x 365 days

x 10-20 years

A. Rozhkov

J. Burger

ISS Astronaut with AMS

Laptop

31

POCC at CERN

24/7, 365d/y

Example: ECAL Temperature changes from -10oC to 30oC over 9 months

0oC

10o

20o

30o

1.7.11 1.9.11 1.11.11 1.1.12 1.3.12

-10o

1.5.11

ECAL

Large temperature

variations

Thermal Operations

AMS has no control

of the Space Station

orientation 32

32

SDU (Prof. Cheng Lin)

has made major

contributions to the

thermal operations

In 4 years on ISS,

AMS has collected >60 billion cosmic rays.

To match the statistics,

systematic errors studies have become important.

33

AMS is a very precise particle physics detector. The data was analysed by at least two independent AMS international teams

M. Incagli

S. Schael V. Choutko A. Kounine J. Berdugo

S. Rosier-Lees

B. Bertucci

S. Haino, A. Oliva P. Zuccon Z. Weng

M. Duranti H. Gast J. Casaus L. Derome M. Capell I. Gebauer

M. Pohl 34

M. Heil

IN2P3 – LYON

FZJ – Juelich

INFN MILANO BICOCCA

CNAF – INFN BOLOGNA

ASDC – ROME

CIEMAT – MADRID

AMS@CERN – GENEVA

NLAA – BEIJING

SEU – NANJING

ACAD. SINICA – TAIPEI

AMS Data Analysis Conducted at the Science Operations Center at CERN and in the

regional centers around the world.

35

The isotropic proton flux Φi for the i th rigidity bin (Ri , Ri +ΔRi) is

Ni is the number of events, 300 million proton events have been selected;

Ai is the effective acceptance;

εi is the trigger efficiency;

Ti is the collection time (which depends on the geomagnetic cutoff).

To match the statistics, extensive systematic errors study

has been made.

36

To be presented by V. Choutko (MIT)

Systematic errors on the Proton Flux: 1) σtrig.:trigger efficiency 2) σacc.: a. the acceptance and event selection b. background contamination c. geomagnetic cutoff 3) σunf.

a. unfolding b. the rigidity resolution function 4) σscale.: the absolute rigidity scale

37

300 million events

AMS proton flux

AMS-02

38

39

AMS proton flux

Solid curve fit of Eq. Φ to the data.

(Fit to data above 45 GV: χ2/d.f.= 25 /26)

Dashed curve uses the same fit

values but with Δ set to zero.

Φ Φ

Φ

40

AMS proton flux fit with two power laws: R, R+Δ with a characteristic transition rigidity R0

and smoothness s

41

AMS proton spectral index variation:

Model independent measurement of spectral index

Sp

ec

tral

Ind

ex

= d log (Φ)/ d log (R)

2011

2012

2013

2011-2013

Spectral index of the proton flux for 2011 to 2013

Measuring electrons and positrons

TRD (transition radiation) to identify e±

ECAL (shower shape) to separate e± from protons

ECAL measures E Tracker measures p

e±: E=p proton: E<p

43

Pro

bab

ilit

y

proton electron

proton electron

proton electron

TRD estimator

ISS data:83-100 GeV

E/p

Boosted Decision Tree, BDT:

ECAL BDT

ISS data:83-100 GeV

εe=90%

No

rma

lize

d e

nti

tie

s

Fra

cti

on

of

eve

nts

ISS data:83-100 GeV

Physics of 11 million e+, e- events

Collision of “ordinary” Cosmic Rays produce e+, p..

Collisions of Dark Matter (neutralinos, ) will produce additional e+, p, …

The Origin of Dark Matter

~ 90% of Matter in the Universe is not visible and is called Dark Matter

Donato et al., PRL 102, 071301 (2009)

Antiprotons: + p + …

m= 1 TeV

Positrons: + e+ + …

m=800 GeV

I. Cholis et al., JCAP 0912 (2009) 007

m=400 GeV

e± energy [GeV]

e+ /(e

+ +

e- )

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

11 million e+, e- events

AMS-02

Po

sit

ron

Fra

cti

on

Verification of Positron Fraction with two independent samples

Positron fraction analysis with TRD Only

Good agreement between two independent samples 46

TRD

e-

ECAL

Outside ECAL vs inside ECAL

Po

sitr

on

fra

ctio

n

47

Positron Fraction from AMS

The energy beyond which it ceases to increase.

48

Energy [GeV]

11 million e+, e- events

49

200 400 600 800 10000

0.05

0.1

0.15

0.2

e± energy [GeV]

Po

sit

ron

fra

cti

on

Pulsars

Collision of cosmic rays

m = 700 GeV 275±32 GeV

Current status

The expected rate at which it falls

beyond the turning point.

50

e± energy [GeV]

Po

sit

ron

fra

cti

on

Pulsars

Collision of cosmic rays

m = 700 GeV 275±32 GeV

In 10 years from now

The expected rate at which it falls

beyond the turning point.

Ne± is the number of electron or positron events Aeff is the effective acceptance εtrig is the trigger efficiency T is the exposure time

Measurement of the flux of electrons and positrons

51 to be presented by Professor S. Schael (RWTH-Aachen)

Electron flux (before AMS)

52

Electron Flux

53

Electron Flux

54

See O. Adriani et al., PRL 111 (2013) 081102

30

25

20

15

10

5

Positron flux (before AMS)

55

Positron Flux

56

Positron Flux

57

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).

Observations:

The Electron Flux and the Positron Flux

58

spectral index = d log (Φ)/ d log (E)

The (e+ + e-) flux before AMS

59

Combined (e+ + e-) Flux: event selection

TRD:

identifies

electron

Tracker and Magnet:

ECAL: identifies electron and

measures its energy

bending

view

Independent of charge sign measurement no charge confusion

High selection efficiency : 70% @ TeV

Small systematics on acceptance: 2% @ TeV

To be presented by Professor Bruna Bertucci (INFN-Perugia) 60

Energy (GeV)1 10

2103

10

)-1

sr

se

c ]

2 [

m2

(G

eV

F ´

3E

0

50

100

150

200

250

300

350

400AMS-02

ATIC

BETS 97&98

PPB-BETS 04

Fermi-LAT

HEAT

H.E.S.S.

H.E.S.S. (LE)

AMS Results: (e+ + e-) flux

Energy Range: 0.5 GeV to 1 TeV

61

= d log (Φ)/ d log (E) S

pe

ctr

al In

de

x

62

γ=−3.170 ± 0.008 (stat + syst.) ± 0.008 (energy scale)

E > 30 GeV

Φ(e++e−) = C E

The flux is consistent with a single power law above 30 GeV.

63

64

TRD

ECAL

RICH

MA

GN

ET

AC

C

Tracker

2

3-4

5-6

7-8

Antiproton event:

R = −423 GV

Antiproton/proton ratio

9

1

To be presented by

A. Kounine (MIT)

65

AMS p/p results

66

AMS p/p results

AMS p/p results and modeling

67




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, …)

AMS p/p results and modeling 11 million e+, e- events

68

c

c

p, p,e-,e+,g

p, p,e-,e+,g

Annihilation

Scat

teri

ng

Production

LHC

LUX DARKSIDE XENON 100 CDMS II …

AMS, Fermi-LAT, HESS, …

Three independent methods to search for Dark Matter

,...,, pe

pp ...

69

e

e

p, p,e-,e+,g

p, p,e-,e+,g

Annihilation

Scat

teri

ng

Production

BNL, FNAL, LHC …CP, J, Υ, t, Z, W, h0

SLA

C …

pa

rto

ns,

ele

ctro

wea

k

SPEAR, DORIS, PEP, PETRA, LEP, … Ψ, τ

Physics of electrons and protons

,,,, eeppee

ppee ...

70

Measurement of Nuclei with AMS

AMS: Multiple Independent Measurements

of the Charge (|Z|)

Carbon (Z=6) ΔZ (cu)

0.30

0.12

0.32

0.30

0.33

0.16

0.16

Tra

cker

1

2

7-8

3-4

9

5-6

71

1. Tracker Plane 1

6. RICH

4. Tracker Planes 2-8

7. Tracker Plane 9

2. TRD

3. Upper TOF (1 counter)

5. Lower TOF (1 counter)

H He

Li Be B C

N O

F Ne

Na

Mg

Al Si

Cl Ar K Ca

Sc V Cr

P S Fe

Ni Ti

Mn

Co

AMS Nuclei Measurement on ISS

72

To be presented by V. Choutko, L. Derome, S. Haino, M. Heil, A. Oliva

73

AMS Helium Flux

To be presented by S. Haino (Academia Sinica, Taiwan)

50 million events

74

AMS Helium Flux

75

Fit to data

with Δγ=0

AMS Helium Flux

Solid curve fit of Eq. Φ to the data.

(Fit to data above 45 GV: χ2/d.f.= 20.5 /27)

Dashed curve uses the same fit

values but with Δ set to zero.

Model Independent

Spectral Indices Comparison

76

= d log (Φ)/ d log (R)

proton/He flux ratio

77 16-04-2015 AMS days - He flux

Single power law fit

(R > 25 GV)

Φp/ΦHe = C Rγ

77

78

AMS Orth et al (1978) Juliusson et al (1974)

AMS Lithium flux – current status

To be presented by L. Derome (LPSC, Grenoble)

79 Slope changes at about the same rigidity as for protons and helium

Lithium flux with two power law fit

Rigidity (GV)10

210

310

Bo

ron-t

o-C

arb

on

0.03

0.04

0.05

0.06

0.1

0.2

0.3

0.4B/C Ratio

Exposure time of 40 months 7M Carbons, 2M Borons

Kinetic Energy (GeV/n)1 10

210

Bo

ron

-to-C

arb

on

Ra

tio

0.03

0.04

0.05

0.06

0.1

0.2

0.3

0.4

Orth et al. (1972)

Dwyer & Meyer (1973-1975)

Simon et al. (1974-1976)

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

To be presented by A. Oliva (CIEMAT) 80


210

310

Bo

ron

-to-C

arb

on

Ra

tio

0.02

0.03

0.04

0.05

0.1

0.2

0.3

0.4

AMS-02

PAMELA (2014)

TRACER (2006)

CREAM-I (2004)

ATIC-02 (2003)

AMS-01 (1998)




HEAO3-C2 (1980)

Simon et al. (1974-1976)


Orth et al. (1972)

B/C Ratio converted in Kinetic Energy

Cowsik et al. (2014)

Fit to positron fraction by

secondary production model

81

In the past hundred years, measurements of charged

cosmic rays by balloons and satellites have typically

contained ~30% uncertainty.

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.

82




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, …)

AMS p/p results and modeling 11 million e+, e- events

83

The Electron Flux and the Positron Flux

spectral index = d log (Φ)/ d log (E)

γ=−3.170 ± 0.008 (stat + syst.) ± 0.008 (energy scale)

E > 30 GeV

Φ(e++e−) = C E

Energy [GeV]

84

85

AMS proton flux

AMS Helium Flux

Lithium flux

Rigidity (GV)10

210

310

Bo

ron-t

o-C

arb

on

0.03

0.04

0.05

0.06

0.1

0.2

0.3

0.4

B/C Ratio

Exposure time of 40 months 7M Carbons, 2M Borons


210

Bo

ron

-to-C

arb

on

Ra

tio

0.03

0.04

0.05

0.06

0.1

0.2

0.3

0.4

Orth et al. (1972)


Simon et al. (1974-1976)

HEAO3-C2 (1980)




AMS-01 (1998)

ATIC-02 (2003)

CREAM-I (2004)

TRACER (2006)

PAMELA (2014)

AMS-02

Bo

ron

-to

-Carb

on

Rigidity [GV]

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.

AMS Days at CERN The Future of Cosmic Ray Physics and Latest Results

CERN, Main Auditorium,

April 15-17, 2015

Wednesday, 15 April 2015

Thursday, 16 April 2015

Friday, 17 April 2015

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

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

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

14:00 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

08:30 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 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 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 W. Gerstenmaier, NASA Public Lecture: Human Space Exploration

AMS

Contact: Ms. Laurence Barrin <[email protected]>

08:30-12:00 Chairman: R Heuer

16:15 - 18:15 Chairman: H. Schopper

08:30-12:45 Chairman: F. Linde 14:00-18:15 Chairman: Y.F. Wang

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

13:00 - 16:15 Chairman: F. Ferroni

18:15 R. Heuer

the ams experiment

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