AMS

R.Battiston

SIFI 2010

Bologna

The Alpha Magnetic Spectrometeron the

International Space Station

September 2010

2- Charged cosmic rays: An unexplored region in science. Using a magnetic spectrometer (AMS) on ISS is the only way to measure high energy charged cosmic rays.

1- Neutral cosmic rays (light rays and neutrinos):Light rays have been measured (e.g., Hubble) for over 50 years. Fundamental discoveries have been made.

Fundamental Science on the International Space Station (ISS)There are two kinds of cosmic rays traveling through space

AMS

The major physical science experiment on the ISS

AMS

3

USAFLORIDA A&M UNIV.FLORIDA STATE UNIVERSITYMIT - CAMBRIDGENASA GODDARD SPACE FLIGHT CENTERNASA JOHNSON SPACE CENTERTEXAS A&M UNIVERSITYUNIV. OF MARYLAND - DEPT OF PHYSICSYALE UNIVERSITY - NEW HAVEN

MEXICOUNAM

DENMARKUNIV. OF AARHUS

FINLANDHELSINKI UNIV.UNIV. OF TURKU

FRANCEGAM MONTPELLIERLAPP ANNECYLPSC GRENOBLE

GERMANYRWTH-IRWTH-IIIMAX-PLANK INST.UNIV. OF KARLSRUHE

ITALYASICARSO TRIESTEIROE FLORENCEINFN & UNIV. OF BOLOGNAINFN & UNIV. OF MILANOINFN & UNIV. OF PERUGIAINFN & UNIV. OF PISAINFN & UNIV. OF ROMAINFN & UNIV. OF SIENA

NETHERLANDSESA-ESTECNIKHEFNLR

ROMANIAISSUNIV. OF BUCHAREST

RUSSIAI.K.I.ITEPKURCHATOV INST.MOSCOW STATE UNIV.

SPAINCIEMAT - MADRIDI.A.C. CANARIAS.

SWITZERLANDETH-ZURICHUNIV. OF GENEVA

CHINA BISEE (Beijing)IEE (Beijing)IHEP (Beijing)SJTU (Shanghai)SEU (Nanjing)SYSU (Guangzhou)SDU (Jinan)

KOREAEWHA

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

95% of the ~$2.0B to build AMS has come from our international partners based on NASA’s commitment to deploy AMS on the ISS

AMS International Collaboration16 Countries, 60 Institutes and 600 Physicists

DESY1965-1972

BNL1972-1974

PETRA1978-1983

LEP1983-2003

Physicists10 20 60 600 400 600

Cost (M$)0.01 0.1 15 ~1,000 ~500 >2,000

Shuttle1994-1998

e-proton e-e+ e- e+

ISS1998-...

The scientists in AMS Experiment are mostly European and have worked togetherfor years.

SiliconVertex

Detector

σ =7µm

L3: 1983 - 2003

. . . .

From: Steve Myers Sent: Mon 2/8/2010 7:58 AM To: Dimitri Delikaris; Dietrich Schinzel

Dear Dimitri,

There is a decision from the Directorate level to give the maximum possible amount of help to AMS.I really appreciate your aid. If there are any “legal” problems please let me know right away.Regards,

Steve

Steve MyersDirector of Accelerators and TechnologyEuropean Organisation for Nuclear Research (CERN)CH-1211 Geneva 23Switzerland

FePe– HePe+

TRD

TOF

Tracker+Magnet

RICH

ECAL

– ___

Physicsexample AntimatterCosmic Ray Physics

StrangeletsDark matter

AMS is the first large magnetic detector in space. It provides a measurement of particles and nuclei with a position resolution of 10 microns in a magnetic field of 1200 Gauss. It measures the velocity (near the speed of light) to an accuracy of 1/1000, and it measures the flight time to 150 picoseconds. It can simultaneously measure all the nuclei in space.

Geometric Factor 5000 cm2 sr ; MDR 2,1 TV 12

4

The AMS-01 Detector (1994-1998)

Tim

e o

f Fligh

tσ

= 1

24

ps

Aerogel

6 planes of Silicon Tracker: 3.2 % X0, 10 m. BL2 = 0.14 Tm2, ΔP/P = 7% at 10 GeV

AMS-01

1998

12

TRDElectrons

Silicon TrackerMass, Charge, Energy

ECALElectrons, Gamma-rays

RICHMass, Charge, Energy

TOFMass, Charge, Energy

AMS on ISSParticles are identified by their

mass, charge and energy.

MagnetMass, ± Charge, Energy

1) no iron ⇒ to reduce weight

2) no field leak out of the magnet⇒ for safety of astronauts

3) no influence from earth magneticfield ⇒ stability

y99084_5a_right.ppt

The AMS superconducting magnet has been designed to operate for 3 years in space, without refilling possibility, according to the NASA-DOE,

signed before the 2003 Columbia accident

B = 0.5 GaussThe AMS superconducting magnet has the

following unique features:

The Superconducting magnet

2,500 liters of Superfluid Helium (1.8K)

For AMS-02, two Magnets were built:One for Space Qualification Tests in Germany and Italy

Transition Radiation Detector: TRDIdentify electrons e± with v = 0.9999c

radiate γ when passing foils/fibers

Proportional Tube

4 – 8 keV γ

Transition Radiation Detector: TRD

5248 tubes2 meter length

centered to 0.1mm

Test results: measure all nuclei simultaneously

Silicon Tracker

Resolution: 10 µm

8 planes, 200,000 channels

Th. Kirn, Status Report on AMS-02 ACC-System

Ring Imaging Cerenkov Counter (RICH)

Radiator

10,880 Photodetectors

Reflector

Particle: Velocity(θ), Charge(Intensity)

γθ

Calorimeter (ECAL)

e±, γ proton

A precision 3-dimensional measurement of the directions and energies of light rays and electrons

10 000 fibers, φ = 1 mmdistributed uniformly Inside 1,200 lb of lead

Vibration

Dedicated Space Qualification Facilities have been developed for AMS in Italy

Radiation

Radiation

Thermal Thermal-Vacuum

Electromagnetic

StructuralRequirements

ThermalRequirements

RadiationRequirements

Mission SuccessRequirements

Test campaigndefinition

Test Execution

Test facility

Test Results

The SERMS Laboratory

Vibration tests of Flight Model Time of Flight

2009: AFTER 9000 hrs of TVT…THE END OF SUB-SYSTEM TESTS

Final test at CERN: AMS in accelerator test beam Feb 4-8.

AMS

27 km

CERN Accelerator Complex

7 km

Progress Report

To Mr. William Gerstenmaier

on AMS19 January 2010

AMS in Test BeamAMS in Test Beam, Feb 4-8, 2010

θ

Φ

TRD

TOF

TRACKER

TOFRICH

ECAL

MA

GN

ET

HE

LIU

M

tracker layers with superconducting magnet1

45

23

67

8

TrackerLayers

Test Beam Results with superconducting magnet – Feb 2010

Velocity measured to an accuracy of 1/1000for 400 GeV protons

Bending Plane Residual (cm)Electron Energy Resolution: 2.5-

3%

N

N

Energy

N

TRD: 400 GeV Protons

Measured combined rejection power at 400 GeV: e+/p = 10-6

32

Alpha Magnetic Spectrometer

14/9/2010

AMS-02 TV test stand - GONDOLA

• Gondola Manufacturing and assembly

• Installation tools

33

34

Trac

ker

1

2

7-8

3-4

9

5-6

TRDIdentify e+, e-

Silicon TrackerZ, P

ECALE of e+, e-, γ

RICHZ, E

TOFZ, EParticles and nuclei are defined by their

charge (Z) and energy (E ~ P)

Z, P are measured independently from Tracker, RICH, TOF and ECAL

AMS: A TeV precision, multipurpose spectrometer

Magnet±Z

Permanent magnet

AMS-01PERMANENTMAGNET

MAGNETWITH INTERFACE SUPPORT

MAGNETINTO VACUUM CASE

TRD

TOF

TRACKER

TOFRICH

ECAL

MA

GN

ET

tracker layers with permanent magnet

1

56

34

78

9

TrackerLayers

2

Tracker Layers 1 and 9 provide much better momentum resolution

With 9 tracker planes, the resolution of AMS with the permanent magnet is equal (to 10%) to that of the superconducting magnet.

AMS-02 (MDRP 2.14 TV)(MDRHe 3.75TV)

AMS-02 SC (MDRP 2.18 TV)

Rig

idity

reso

lutio

n %

Proton Rigidity (GV)

PM vs SC Magnet difference

AMS in Test Beam with permanent magnet – 8-20 Aug 2010

Beam test planning…

41

FEBRUARY

Test Beam Results with permanent magnet – 8-19 Aug 2010

Velocity measured to an accuracy of 1/1000for 400 GeV protons

Bending Plane Residual (cm)e± Energy Resolution: 2.5-3%

N

N

Energy

N

Reconstructed Velocity

TRD: 400 GeV protons

Test Beam Result (august 2010)400 GeV protons

43

AMS-02 (MDRP 2.14 TV)(MDRHe 3.75TV)

AMS-02 SC (MDRP 2.18 TV)

Rig

idity

reso

lutio

n %

Proton Rigidity (GV)

Transportation to KSC from the Geneva airport (1)

Transportation to KSC from the Geneva airport (2)

Search for Cold Dark Matter: χ0Physics example

Collisions of χ0 will produce excesses in the spectra of e+,e-,p different from known cosmic ray collisions

AMS-02 (mχ=200 GeV)

From Dark matter collisions

The spectra of all types of cosmic rays will be measured by AMS simultaneously

DM searches with AMS-02

Accelerators

AMS in Space

The Big Bang origin of the Universe requires matter and antimatterto be equally abundant at the very hot beginning

Physics examplesSearch for the existence of Antimatter in the Universe

AMS

LHC

AMS-02 Antihelium Limits

Current antimattersearches are limited

y06K301

He/

He

(CL

95%

)

Study of high energy (0.1 GeV – 1 TeV) diffuse gammas AMS Physics example

The diffuse gamma-ray spectrum of the Galactic plane40o < 1 < 100o, |b| < 5o

AMS-02

Space Experiments Ground Experiments

T.Prodanovi´c et al., astro-ph/0603618 v1 22 Mar 2006

EGRET

e+e−

γ

1. Pointing precision of 2 arcsec2. UTC time (from GPS, μsec accuracy) allows to relate

AMS measurements with other missions

Pulsars in the Milky Way:

Pulsar: Neutron star sending radiation in a periodic way, currently measured with millisec accuracy.Emission in radio, visible, X- and gamma rays currently measured up to ~1 Gev.

AMS: pulsar periods measured with μsec time precision andenergy spectrum for pulsars measured to 1 TeV(a factor of 1,000 improvement in time and energy).

Similar studies can be made for Blazers and Gamma Ray Bursters

Mark E. Kelly (Captain, USN)

Gregory H. Johnson (Colonel, USAF, Ret.)

E. M. “Mike”Fincke (Colonel, USAF)

Andrew J. Feustel (Ph.D.)

Roberto Vittori(Italian Air Force Colonel)

Gregory Errol Chamitoff (Ph.D.)

AMS astronauts

The issues of antimatter in the universe and the origin of Dark Matter probe the foundations of modern physics.

The Cosmos is the Ultimate Laboratory.Cosmic rays can be observed at energies higher than any accelerator.

AMS februady 26th 2011

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.

y96402nac.ppt

Facility Original purpose,Expert Opinion

Discovery withPrecision Instrument

Brookhaven π N interactionsνe, νμ

CP violation,J

FNAL Neutrino physics b, t quarks

SLAC Spear ep, QED Scaling, Ψ, τ

PETRA t quark Gluon

Super Kamiokande Proton decay Neutrino oscillations

AMS on ISS Dark Matter, AntimatterStrangelets,… ?

Hubble SpaceTelescope

Galacticsurvey

Curvature of the universe, dark energy

P.S. CERN π N interactions Neutral Currents -> Z, W

Exploring a new territory with a precision instrument is the key to discovery.

(1960’s)

(1960’s)

(1970’s)

(1970’s)

(1980’s)

(2000)

(1990’s)