First&six&years&of&AMS&on&the&ISS&

Stefan&Schael,&&RWTH&Aachen

GSI Darmstadt, January 2018

2

Dark Matter 13.7 billion years

COBE, WMAP, PLANCK HUBBLE

Big Bang

?

?

?

?

?

5

Light primary cosmic ryas: p, He, C, N, O and e-

Light secondary cosmic ryas: Li, Be, B and e+, p

6"

7"

Pierre;Auger;Observatorium,&ArgenBnien,&3000&km2&

Pierre;Auger&Observatory"

AMS&

470&kg&

9"

PAMELA&2006;2014&

AMS&

470&kg&

O.&Adriani&et&al.&&Physics&Reports&544&(2014)&323–370&

10"

PAMELA&2006;2014&

AMS&

470&kg&

6,717&kg&

1&m&

O.&Adriani&et&al.&&Physics&Reports&544&(2014)&323–370&

Physics of Charged Cosmic Rays

D L D .D 59L7 0

D L D D H DC. C DC

) D L D DC. 4DK AA

D D( 3 DC P

7 .519DC 1 29 : 9 M 8 6 9

11"

πµ

πππ

µ

µ

µ

e

ee

e

Dark Matter ?

Discoveries: (1)  Pulsar, (2)  Microwave, (3)  Binary Pulsars, (4) X Ray sources,

solar neutrinos (5) Dark Matter,

Dark Energy … …

Hubble, Chandra, GLAST, JWST, JDEM

WHIPPLE, HESS, VERITAS, …

AUGER

SUPER K HiRes

γ ,ν

S. Ting, MIT"

12

USA FLORIDA A&M UNIV. FLORIDA STATE UNIVERSITY MIT - CAMBRIDGE NASA GODDARD SPACE FLIGHT CENTER NASA JOHNSON SPACE CENTER TEXAS A&M UNIVERSITY UNIV. OF MARYLAND - DEPT OF PHYSICS YALE UNIVERSITY - NEW HAVEN

MEXICO UNAM

DENMARK UNIV. OF AARHUS

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 is US Dept of Energy (DOE) led International Collaboration 16 Countries, 60 Institutes and 600 Physicists, 17 years

The detectors were built all over the world and assembled at CERN, near Geneva, Switzerland 13&

TRD

TOF

Tracker

TOFRICH

ECAL

1

2

7-8

3-4

9

5-6

TRD Identify e+, e-

Silicon Tracker Z, P

ECAL E of e+, e-, γ

RICH Z, E

TOF Z, E

&&ParBcles&and&nuclei&are&defined&by&their&&

charge&(Z)&and&energy (E ~ P)

Z, P are measured independently by the Tracker, RICH, TOF and ECAL

AMS: A TeV precision, multipurpose spectrometer

Magnet ±Z

14&

6 5m x 4m x 3m

7 tons

Silicon layer

7 Silicon layers

Silicon layer

TRD

TOF 1, 2

TOF 3, 4

RICH

ECAL

Magnet

300,000 electronic channels 650 processors

Radiators

11,000 Photo Sensors

15&

y97141b..ppt

…WE JUST DECIDED LAUNCHING MONEY DIRECTLY INTO SPACE WAS CHEAPER …

€ CHFDM

£ FFR¥ Lira

16&

A US Air Force C-5 Galaxy has been used for transport

from Geneva to KSC 25. August 2010

17&

AMS

18&

Closing Endeavour s Payload Bay Doors at the Launch Pad

19&

STS-134 launch May 16, 2011 @ 08:56 AM

20&

Endeavour approaches the International Space Station 21&

AMS installed on the ISS Truss and taking data

May 19, 2011

22&

Up to now, AMS has collected >100 billion cosmic rays. This is a unique data set

to serach for new phenomena.

1.03 TeV electron

TRD: identifies electron

Tracker and Magnet: measure momentum

ECAL: identifies electron and measures its momentum

side view

front view

RICH charge of electron

23&

Citations: > 750

25&

!  The&electron&flux&and&the&positron&flux&are&different&in&their&magnitude&and&energy&dependence&

!  Electrons&and&positrons&have&a&different&origin.&

Energy [GeV]1 10 210 310

]2 G

eV

-1 s

-1 s

r

-2 [m3 E~ - e

50

100

150

200

250

]2 G

eV

-1 s

-1 s

r

-2 [m3 E~ + e

5

10

15

20

25El

ectr

on S

pect

rum

Posi

tron

Spe

ctru

m

1,080,000 positrons

16,500,000 electrons

e± energy [GeV]

preliminary

1 10 210 3100

0.1

0.2

0.3

Positron&FracBon&2016&

Φe+&&=&Ce+&� −γe+&+&Cs� −γs&e−E/Es&&Φe;&'=&Ce;&� −γe;&+&Cs� −γs&e−E/Es'

Es'='530'''''''GeV'''χ2/'n.d.f.'='39/59'+170'

−100'

e± energy [GeV]

Posi

tron

Fra

ctio

n

26

Maximum&at&E=265&±&22&GeV&

preliminary

Comparison of the positron fraction measurement with a Dark Matter model

210 310-210

-110

Collision of Cosmic Rays with the ISM

Posi

tron

Fra

ctio

n

e± energy [GeV]

MDM = 1 TeV

Model based on J. Kopp, Phys. Rev. D 88 (2013) 076013

AMS&2016&

17 million events

27"

preliminary

28&

29&

•  The origin of the difference between (AMS, CALET, H.E.S.S.) and (FERMI, DAMPE) is not clear.

•  A sharp cut-off in the (e+ + e-) Flux is visible at E≈1 TeV, the origin is not understood.

The AMS results are in excellent agreement with a Dark Matter Model

AMS 2016

Energy [GeV]1 10 210 310

5

10

15

20

25

Dark Matter 1TeV

30

Posi

tron

Spe

ctru

m E3 F

lux [

GeV3 /(

s sr m

2 GeV

)]

preliminary

2024: Extend measurement to 1 TeV

31

1 10 210 3100

5

10

15

20

25

30]

2 G

eV⋅ -1 s ⋅ -1 sr ⋅ -2

[m3 E~ x+ e

Φ

Energy [GeV]

Dark Matter 1TeV

AMS&MC&&13&years&

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"

H&

Cosmic Nuclei AMS has seven instruments which

independently identify different elements

32

TRD

0.30&

0.12&

0.32&0.30&

0.33&0.16&

0.16&

∆Z&for&Z=6&Tracker Plane 1

Upper TOF

Tracker Plane 2-8

Lower TOF RICH Tracker Plane 9

Rigidity [GV]

1 10 210 310

]1.7

GV

-1se

c-1

sr-2

[m

2.7 R~ ×Fl

ux

0

2

4

6

8

10

12

14310×

AMS-02300 million

events

AMS Proton Flux, accuracy 1%

AMS-02

M. Aguilar et al., Phys. Rev. Lett. 114, 171103 (2015) 33

34

Rigidity (GV)-110 1 10 210 310

-1 )-1

.7 s

r s G

V2

Flu

x (m

× 2.

7R

1

10

210

310

410 Voyager&outside(the(solar(system&

E."C."Stone"et(al.,""Science"341,"150"(2013)"

AMS;02&

Understanding&of&the&Solar&MagneBc&Field:&

Rigidity [GV]

Effect&of&the&Solar&MagneBc&Field&

The proton flux and the effect of the solar magnetic field

C. Corti et al., ApJ 829, 8 (2016) 35

inside(the(solar(system(

AMS;02&

36&

"

"

"

37&

]1.7

GV

-1se

c-1

sr-2 [m2.7 R~ ×

Flux

8

9

1011

12

13

14310×

AMS-02Fit to Eq. (3) Eq. (3) with Δγ=0

Rigidity [GV] 10 210 310

\\\"

Fit to Model χ2"/NDF=25/26"

Fit to Model with =0

(sys)-0.003+0.004(fit)

-0.002+0.002 = -2.849γ

(sys)-0.030+0.046(fit)

-0.021+0.032 = 0.133γ∆

(sys) [GV]-28+66(fit)-44

+68 = 3360R

This&measurement&is&dominated&by&systemaBc&errors,&&we&will&therefore&not&be&able&to&improve&it.&

It&was&expected&that&the&proton&flux&could&be&described&&with&a&single&power&law&with&spectral&index&γ=;2.7.&

50 million helium nuclei

38&

Using&the&TRD&we&will&extend&this&measurement&up&to&~5&TeV&in&2024.&

39"

It&was&expected&that&the&He&flux&could&be&described&&with&a&single&power&law&with&spectral&index&γ=;2.7.&

39&

) [GV]R~Rigidity (

10 210 310

p/H

e

33.5

44.5

55.5

66.5

77.5

8AMS-02Single power law fit (R>45 GV)

Traditional Models

Theoretical prediction

A. E. Vladimirov, I. Moskalenko, A. Strong, et al., Computer Phys. Comm. 182 (2011) 1156

&Protons&and&helium&are&both&“primary”&cosmic&rays.&

&Their&rigidity&raBo&has&tradiBonally&been&assumed&to&be&flat.&

AMS&:&this&raBo&is&not&flat.&&

The AMS proton/helium flux ratio

40&

Helium isotopic composition

41"

preliminary

The AMS Result on the Carbon Flux

Above 60 GV, these fluxes have identical rigidity dependence.

Rigidity dependence of Primary Cosmic Rays

AMS"

Primary&Cosmic&Rays&(p,&He,&C,&O,&…)&

AMS"

Secondary&Cosmic&Rays&(Li,&Be,&B,&…)&

ISM"

44"

TheoreBcal&&predicBon&

AMS:&2.2"million"

Lithium"Events"

The&AMS&Result&on&the&Lithium&Flux&

45"

preliminary

Rigidity [GV]

40 210 210×2 310 310×2

] 1.

7 (G

V)-1

sr-1 s

-2 [

m2.

7 R×

Flux

0

10

20

30

BoronBerilliumLithium

3

6

6

13

46&

Secondary&cosmic&rays&Li,&Be,&and&B&have&idenBcal&rigidity&dependence.&

Lithium&Beryllium&Boron&

B&Be& Li&preliminary

47&

“Secondary”"cosmic"rays"have"a"different""rigidity"dependence"than"

“primary”"cosmic"rays."

Primary&&

Secondary&&

preliminary

48&

Above 200 GV the Li, Be, and B fluxes all harden more than the He, C, and O fluxes.

Φ = C ⋅E−γ

preliminary

49&

50&

Collision of ordinary CR (Moskalenko, Strong)

TheoreBcal&models&to&explain&the&AMS&positron&fracBon.&Among&the&100’s&of&models&there&are&three&classes:&a)  dark&maner&&b)  new&forms&of&propagaBon&&c)  pulsars.&&

b) An example&of&new&propagaBon:&R.&Cowsik,&B.&Burch,&and&T.&Madziwa;Nussinov,&Ap.&J.&786&(2014)&124&

51&

52&

Kolmogorov&turbulance&&model&predicts&δ=1/3.&

22.01.18& 53&

AMS results on the p/p flux ratio

|Rigidity| [GV]100 200 300 400 500

/p ra

tiop

-510

-410

AMS-02PAMELAKinetic energy [GeV]

0.2 0.3 1 2 3 4 5 6 7 8 10

/p ra

tiop

-510

-410

AMS-02PAMELABESS-polarII

54&

AMS&p/p&results&and&modeling&

|Rigidity| [GV]1000 200 300 400 500

/p ra

tiop

5−10

4−10

AMS-02

Dark Matter

Collisions of ordinary cosmic rays

Models&from&Donato&et&al.,&PRL&102,&071301&(2009);&&m = 1 TeV&&&&&

55&

G.Giesen"et"al.,"JCAP09(2015)"023"""

56&

Rigidity [GV]210 310

410

1

10

10

210

1

10]

1.7GV ⋅-1 s ⋅-1 sr ⋅

⋅-2

[m2.7 RΦ

ˇ e-

e+

p

p

20

3x103

p p

e− e+

100 200 300 400 500

-510

-410

AMS-02PAMELA

0

Φ /Φ

rati

o p

p

|Rigidity| [GV]

Unexpected Result: The Rigidity Dependence of Elementary Particles e+, p, p are identical from 60-500 GV.

e- has a different rigidity dependence.

M. Aguilar et al., Phys. Rev. Lett. 117, 091103 (2016) 57

The Space Station has become a unique platform for precision physics research.

“The most exciting objective of AMS is to probe the unknown; to search for phenomena which exist in nature

that we have not yet imagined nor had the tools to discover.” S. Ting