The Alpha Magnetic Spectrometer on the International Space … · 2013-07-17 · usa mit - cambridge nasa johnson space center texas a&m university univ. of hawaii china univ. of

The Alpha Magnetic Spectrometer on the International Space Station

S. Ting

USA

MIT - CAMBRIDGE

NASA JOHNSON SPACE CENTER

TEXAS A&M UNIVERSITY

UNIV. OF HAWAII

UNIV. OF MARYLAND - DEPT OF PHYSICS

YALE UNIVERSITY - NEW HAVEN

MEXICO

UNAM

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

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)

NLAA (Beijing)

SJTU (Shanghai)

SEU (Nanjing)

SYSU (Guangzhou)

SDU (Jinan)

KOREA

EWHA

KYUNGPOOK NAT.UNIV.

PORTUGAL

LAB. OF INSTRUM. LISBON

ACAD. SINICA (Taiwan)

AIDC (Taiwan)

CSIST (Taiwan)

NCU (Chung Li)

NCKU (Tainan)

NCTU (Hsinchu)

NSPO (Hsinchu)

TAIWAN

AMS: a U.S. DOE sponsored international collaboration

TURKEY METU

DENMARK UNIV. OF AARHUS

Strong support from

NASA (D. Goldin, C. Bolden, L. Garver, G. Abbey, W. Gerstenmaier, M. Sistilli, T. Martin, K. Bollweg, …)

and DOE (J. Siegrist, M. Salamon, D.Kovar, S. Gonzalez, R. Staffin, J. O’Fallon, …)

16 Countries, 60 Institutes and 600 Physicists

New results from

the first 2 years of AMS

Scaled by R2.7 From 1 GV to 1.8 TV

New results from AMS 1) Proton flux

Proton flux Comparison with past measurements

AMS-02 Data

Pamela Data

Rigidity (GV)

Search for structures

Proton flux

8 Rigidity (GV)

10210

310

2.7

X R

igid

ity

-1 H

e F

lux

(m

^2

sr

se

c G

V)

310

New Results from AMS 2) Helium spectrum , 2GV to 3TV

Helium flux

Comparison with past measurements

R (GV)

Helium flux

Search for structures

AMS-02 Data

Pamela Data

New results from AMS 3) Electron Spectrum , 1GeV to 500GeV

New results from AMS 4) Positron Spectrum, 1GeV to 350GeV

Energy (GeV)1 10

2103

10

3 E

´ -1

s s

r)2

Flu

x (

Ge

V m

50

100

150

200

250

300

New results from AMS 5) All Electron Spectrum, 0.5GeV to 700GeV

Energy (GeV)1 10

2103

10

3 E

´ -1

s s

r)2

Flu

x (

Ge

V m

0

50

100

150

200

250

300

350

400AMS-02ATIC01&02 (2001 & 2003)BETS04 (2004)BETS97&98 (1997 & 1998)CAPRICE94 (1994)Fermi-LAT (2009)HEAT94 (1994)HEAT94&95 (1994 & 1995)HEAT95 (1995)H.E.S.S. (2004 -2007)H.E.S.S. (LE) (2004 & 2005)

(Electron plus Positron) Spectrum

Energy (GeV)1 10

2103

10

3 E

´ -1

s s

r)2

Flu

x (

Ge

V m

0

50

100

150

200

250

300

350

400AMS-02

ATIC01&02 (2001 & 2003)

BETS04 (2004)

Fermi-LAT (2009)

H.E.S.S. (2004 -2007)

H.E.S.S. (LE) (2004 & 2005)

(Electron plus Positron) Spectrum comparison with recent measurements

Precise measurement of the energy spectra of B/C provides information on Cosmic Ray Interactions and Propagation

New results from AMS 6) Boron-to-Carbon ratio, 5GV to 500GV

Tra

cke

r

1

2

7-8

3-4

9

5-6

1. Tracker Plane 1

6. RICH

AMS: Multiple Independent Measurements

of the Charge (|Z|)

4. Tracker Planes 2-8

7. Tracker Plane 9

2. TRD

3. Upper TOF (1 counter)

5. Lower TOF (1 counter)

Carbon (Z=6) ΔZ (cu)

0.30

0.12

0.32

0.30

0.33

0.16

0.16

ZTOF_LOW=5.2

ZTRK_IN=4.8

ZRICH=5.1

ZTRK_L1=6.1

ZTRD=6.0

Z0=9.9

Z1=5.3

front

view

Carbon

Fragmentation

to Boron

R = 10.6 GV

B/C

Ra

tio

10% of total expected data

Boron-to-Carbon ratio

10% of total expected data

B/C

Ra

tio

Boron-to-Carbon ratio

comparison with recent data

10% of total expected data

Boron-to-Carbon ratio

New results from AMS 7) Positron ratio anisotropy (update)

July 8th, 2013

The fluctuations of the positron ratio e+/e− are isotropic

Sig

nif

ica

nc

e (

)

New results from AMS ICRC2013: On the origin of excess positrons

If the excess has a particle physics origin, it should be isotropic

Galactic

coordinates (b,l)

On the origin of excess positrons

Limits on the amplitude of a dipole anisotropy in

any axis in galactic coordinates

on the positron to electron ratio

δ ≤ 0.030 at the 95% confidence level