PPC – AMS2(Lecture 10)

掃部 輝機

PHYS 823

1

Phys. Lett. B 505 (2001) 161 (Tevatron)Phys. Lett. B 538 (2002) 121 (Tevatron)Phys. Lett. B 611 (2005) 223 (ILC)Phys. Lett. B 618 (2005) 182 (ILC)

Eur. Phys. J. C46 (2006) 43 (LHC+ILC) “ Supersymmetry Parameter Analysis: SPA Convention and Project ”

Phys. Lett. B 639 (2006) 46 (LHC)Phys. Lett. B 649 (2007) 73 (LHC)Phys. Rev. Lett. 100 (2008) 231802 (LHC)Phys. Rev. D 79 (2009) 055002 (LHC) Phys. Rev. D 82 (2010) 115009 (LHC)Phys. Lett. B 703 (2011) 475 (“BEST” at LHC)

PPC Projects at A Glancehttp://faculty.physics.tamu.edu/kamon/research/TEVpheno/http://faculty.physics.tamu.edu/kamon/research/ILCpheno/http://faculty.physics.tamu.edu/kamon/research/LHCpheno/

1

2

3

2

Lecture 3

Lecture 6

Something is missing ...

Lecture 9

Alpha Magnetic Spectrometer on ISSAMS 2

3

Find how one can search for the dark matter annihilation.

AMS

The Alpha Magnetic Spectrometer (AMS) Experiment

Yuan-Hann Chang, NCUPPP9, Chung-Li, 2011.06.04

AMS is a Particle detector in Space

• Particle detector: The cosmic rays carry a lot of information. Detailed study of cosmic ray is key to understand certain aspect of the universe.

• Space: These particles cannot be observed on ground, because the earth is protected by a thick layer of atmosphere.

• Traditionally the study of cosmic rays are carried out by balloon experiments. They typically operates for just a few days.

• AMS is a large magnetic spectrometer in orbit, to be operating for 20 years on ISS.

• The key problem is a magnet that can be delivered to and operate in space.

Trac

ker

1

2

7-8

3-4

9

5-6

TRDIdentify e+, e-

Silicon TrackerZ, P

ECALE of e+, e-, �

RICHZ, E

TOFZ, EParticles and nuclei are defined by their

charge (Z) and energy (E ~ P)

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

AMS: A TeV precision, multipurpose particle physics spectrometer in space.

MagnetZ USA

FLORIDA 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)NLAA (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

AMS is US Dept of Energy (DOE) led International Collaboration16 Countries, 60 Institutes and 600 Physicists, 17 years

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

The Permanent Magnet: on the Shuttle - AMS-01 and on ISS – AMS-02

B

Time of Flight (TOF)Measures the time of particles to ~ 150 picoseconds

ScintillatorPMTs

Light Guides

PMTs

Provides trigger

PPC – AMS2(Lecture 10)

掃部 輝機

PHYS 823

1

Phys. Lett. B 505 (2001) 161 (Tevatron)Phys. Lett. B 538 (2002) 121 (Tevatron)Phys. Lett. B 611 (2005) 223 (ILC)Phys. Lett. B 618 (2005) 182 (ILC)

Eur. Phys. J. C46 (2006) 43 (LHC+ILC) “ Supersymmetry Parameter Analysis: SPA Convention and Project ”

Phys. Lett. B 639 (2006) 46 (LHC)Phys. Lett. B 649 (2007) 73 (LHC)Phys. Rev. Lett. 100 (2008) 231802 (LHC)Phys. Rev. D 79 (2009) 055002 (LHC) Phys. Rev. D 82 (2010) 115009 (LHC)Phys. Lett. B 703 (2011) 475 (“BEST” at LHC)

PPC Projects at A Glancehttp://faculty.physics.tamu.edu/kamon/research/TEVpheno/http://faculty.physics.tamu.edu/kamon/research/ILCpheno/http://faculty.physics.tamu.edu/kamon/research/LHCpheno/

1

2

3

2

Lecture 3

Lecture 6

Something is missing ...

Lecture 9

Alpha Magnetic Spectrometer on ISSAMS 2

3

Find how one can search for the dark matter annihilation.

Transition Radiation Detector: TRDIdentify e+, reject P

Transition Radiation Detector: TRDIdentify e+, reject P

Silicon Tracker: 200,000 Channels in 9 planes, resolution 10 microns

ReflectorRing Imaging CHerenkov (RICH)

Li C OHe Ca

Single Event displays from the Test beam E=158 GeV/n

Particle

Intensity � Z2

� � V

detectors

tensity � Z2

�

NaFRadiator

Detector RICH Detector

10,880 photosensors

e�

1mm Lead foil

1mm Fibers

Calorimeter (ECAL)

e

XYXYXYXYX

Fiber direction

9 super layers provide 3D measurement of shower profile

X

YZ

50,000 fibers, ����mm, distributed uniformly inside 1,200 lb of lead which provides a precision, 3-dimensional, 17X0 measurement of the directions and energies of light rays and electrons up to 1 TeV

National Cheng Kung University

AIDC

National Central UniversityAcademia Sinicathe leading research institution directly under the Presidential Office

Chung-Shan Institute of Science and Technologythe research arm of the Defense

National Space Organizationthe space agency of Taiwan

National ChiaoTung University

Taiwan in AMS

Manufacture of AMS Electronics

Space Qualification Test of AMS Electronics

JIM-CANJIM-HRDL

JIM-AMSW&1553JBU

JHIFJSBC

Taiwan collaborated closely with MIT, INFN, KITin the design and production of the electronics system of the AMS detector: In total 775 boards and 48 crates.

4

Thermal Blanket installation on Electronics, 2009

19AMS-02 Avionics & DAQ

AMS in the ESA Thermal Vacuum Chamber, Noordwijk, the Netherlands Test at CERNAMS in accelerator test beam Feb 4-8 and Aug 8-20, 2010

AMS

27 km

CERN Accelerator Complex

7 km

19 January 2010

AMS in Test Beam – 8-20 Aug 2010 Test Beam ResultsVelocity measured to an accuracy of 1/1000for 400 GeV protons

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

N

N

Energy

N

TRD: 400 GeV protons

The ultra-precision of the AMS detector enables it to measure the particles with accuracy of:1- The coordinates: to 10 microns (10 millionths of a yard)2- The travel time: 100 ps (one-tenth of a billionth of a second)3- The velocity: to an accuracy of 1 in 1000

It will also, simultaneously, measure all cosmic ray atomic nuclei to an energy of a trillion electron-volts.

Test results from accelerator

Nuclear Charge Z

����

r-1

m-2

sr-1

GeV

-1)

AMS will measure cosmic ray spectrafor nuclei, for energies from 100 MeV to 2 TeVwith 1% accuracy over the 11-year solar cycle.

Example of AMS physics:

1. Search for the Dark matter :

XpXe

����

We look for excess in the e+ and p spectrum.

e+ /( e

++

e� )

e+ Energy [GeV]O. Adriani et al., Nature 458 (2009) 607-609

M. Aguilar et al., Phys. Lett. B 646 (2007) 145-154

Berwick, S. W. et al., Astrophys. J. 482 (1997) L191-L194

I.Cholis et al, astro-ph 30 Apr 2009

AMS – search for DM:1. Large acceptance and long duration2. e+/p ~ 10-6

We present four studies based on four modelsto highlight AMS sensitivity

case 1

AMS-02(18 Yrs)

I.Cholis et al, arXiv:0810.5344v3

m�

=100

m�

=200

m�

=400

m�

=800

e+ Energy (GeV)

e+/(

e++

e- )

m�=400 GeV

m�=200 GeV

m�=800 GeV

case 2

L.Bergstrom et al, PRL 103 (2009) 031103

AMS-02 (18 Yrs)

e+ Energy [GeV]

TeV Scale Singlet Dark MatterEduardo Pontón and Lisa Randall

Kaluza-Klein Bosons are also Dark Matter candidates

AMS-02 (18 yrs)

10-1

10-2

10-3

10310210e+ Energy (GeV)

Posit

ron

frac

tion

e+ /(e

++

e- )

sdm_500_18Yb

500 GeV

Fig.5

case 3

arXiv:0811.1029v2 [hep-ph] 20 Jan 2009 - Fig.5

P. Brun, Phys.Rev.D76:083506,2007 and private communication

case 4:DM signal from p

p/p

From a Model of Cosmic Ray collisions

From Dark Matter (M� = 840 GeV) Collisions

AMS-02 (18 yrs)

6·102

(cannot be seen at LHC)

10-5

10-4

10-3

p Kinetic Energy (GeV)102101

Physics of AMS (2): Search for Antimatter Universe

After the Big Bangthere must have been

equal amounts of matter and antimatter.

AMS on the Space Station for 20 years will search for the existence of antimatter to the edge of the universe

AMS on ISS

The Universe began with the Big Bang.

AMS-02 (18 Yrs)

There are six types of Quarks found in accelerators (u, d, s, c, b, t).

All matter on Earth is made out of only two types (u, d) of quarks. “Strangelets”

are new types of matter composed of three types of quarks (u, d, s) which should

exist in the cosmos.

Carbon NucleusZ/A ~ 0.5

StrangeletZ/A ~ 0.1

34

uud

us uuuss

ssdd

dd s

ds

s duuu

d uuud uududd

ududduuududduud

uudduddsddddddddddddddus

dddddddddddddddddddddddddddddddssddddddddddddddddddddddddddddddduuuu

suuuuuuuuuuuu

suuuuddd

dssd

dd duuussuuuuuuddd dd

ddd dd

dddd

ddddddddddddddddddudddudd

d dddduuuu ud uu

uddd

sss

ssddssuu

sssssssssssssssssssssssssssssssssssssuddd

sssddddssssssssssssssssuuu s

ddddddddddddddddddd

uu sssss

dddddddd s

ddd ddd uuu

uuu

uudu

du uu uud

dddd

ddd u

uu uu uud

ddd ddd u ddd ddd u ddd ddd uddd ddd u

uuuu uu uud

uuu uu uud

uu uu uud

p n

AMS will provide a definitive search for this new type of matter.

Physics of AMS (3)Search for New Matter in the Universe

Jack Sandweiss, Yale University

E. Witten, Phys. Rev. D,272-285 (1984)

Z/A

Z/A = 0.114 0.01

AMS-02 measurement of Strangelets based on the candidate measured with AMS-01

�strangelets = 5x10-10(cm2s sr)-1

Search limit down to 2x10-12(cm2s sr)-1

Trac

ker

1

2

7-8

3-4

9

5-6e+e�

�Identifying � Sources with AMS

Unique constraints

P+ = E+ = P��= E�

+ ��

E�

P�

E+

P+

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 ExperimentsGround Experiments

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

EGRET

The Launch and Installation of AMS

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.)

26 August: U.S. Air Force C-5 transported AMS to KSC

AMS Ready for Installation in Endeavour’s Payload Bay, Aug. 28, 2010

AMS Ready for Launch in Endeavour’s Payload Bay Closing Endeavour’s Payload Bay Doors

April 26, 2011

May 16, 2011 @ 08:56 AM

Punching through the other side of the clouds

Endeavour approaching ISS – May 18, 2011

Endeavour approaching ISS – May 18, 2011

Endeavour approaching ISS with Soyuz in foreground

May 18, 2011

AMS about to be picked up by the shuttle robotic arm

AMS in transit, picked up by the ISS robotic arm AMS on the ISS truss. May 19, 2011

Data from the 1st few minutes – 20 GeV proton Data from the 1st few minutes – 42 GeV/c Carbon

• The AMS probes the fundamental physics in the search for the Dark matter and antimatter in the universe.

• The AMS provides precise measurement of the cosmic ray spectra over a large energy range and extended period of time.

• We are excitingly waiting for new phenomena that have not yet been predicted.

Thank you

Realization of AMS1. Strong endorsement of the AMS science from reviews by the

world’s leading scientists

2. Unanimous support from the US Senate and House

3. Major worldwide support from:

NASADOEMIT

FRANCECNRS

GERMANYDLRRWTH-I

ITALYINFNASI

SPAINCIEMAT

SWITZERLANDETHNSF

CHINA

Academy of ScienceMinistry of ScienceNLAAShandongGuangdongJiangsu

TAIWANACAD. SINICA

CSIST

ESA and CERN

Veto System rejects random cosmic rays

Measured veto efficiency better than 0.99999

10 mil pitch

Silicon Tracker

Provides coordinate resolution of 10 microns

Cosmic Ray Measurements Showing Maximium Measurable Energy of 2.2 TeV

� AMS with Superconducting Magnet

� AMS with Permanent Magnet

Even

ts *

TeV

1/Energy

Experimental work on Antimatter in the Universe

Search forBaryogenesis

Proton decaySuper K(�p > 6.6 * 1033 years )

Direct search

y06K299a

New CPBELLEBaBar(sin 2�= 0.672 0.023consistent with SM)

FNAL KTeV(Re( ’/ ) = (19.2 2.1)*10-4)

CERN NA-48 CDF, D0

LHC-bATLASCMS

AMSIncrease in sensitivity: x 103 – 106

Increase in energy to ~TeV

Dark Matter at high energieswith large acceptance and long duration and e+/p ~ 10-6

Model of I. Cholis et al, arXiv:0810.5344v3

AMS-02m�

=100

m�

=200

m�

=400

m�

=800

e+ Energy (GeV)

e+/(

e++

e- )

m�=400 GeV

m�=200 GeV

m�=800 GeV

The Origin of Dark Matter

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

A Galaxy as seen by telescope If we could see Dark Matter in the Galaxy

Search for the origin of Dark Matter:Collisions of Dark Matter will produce additional e+

These characteristics of additional e+ can be measured very accurately by AMS

Cosmic Rays: protons, electrons, Helium …Collision of Cosmic Rays will produce e+ …

e+ /( e

++

e� )

e+ Energy [GeV]O. Adriani et al., Nature 458 (2009) 607-609

M. Aguilar et al., Phys. Lett. B 646 (2007) 145-154

Berwick, S. W. et al., Astrophys. J. 482 (1997) L191-L194

I.Cholis et al, astro-ph 30 Apr 2009

AMS-02 (3 Yrs)

e+ Energy [GeV]

AMS-02 (18 Yrs)

e+ Energy [GeV]e+ /( e

++

e� )

The leading candidate for Dark Matter is a SUSY neutralino (��0 )Collisions of ��0 will produce excess in the spectra of e+ different from known cosmic ray collisions

m�0 = 200 GeV

Experimental work on Antimatter in the UniverseCurrently, minimal direct searches

The new Large Hadron Collider (LHC) will continue this search

AMS on ISS

Assumption: Antimatter does not exist.Search for explanations

Major experiments worldwide over the last 40 years,including 2 dedicated accelerators

No explanation found

Assumption:Antimatter exists.Search for its existence

Increase in sensitivity: x 103 – 106

Increase in energy to ~TeV

Mirko Boezio, Commissione II, 2010/04/2

Facility Original purpose,Expert Opinion

Discovery withPrecision Instrument

Brookhaven

2 types of neutrinosBreak down of time reversal symmetryNew form of matter

FNALNeutrino physics 5th and 6th types of quark

SLAC SpearProperties of quantum electricity

Quark inside protons4th type of quark3rd kind of electrons

PETRA6th kind of quark Gluon

Super Kamiokande Proton life time Neutrino has mass

AMS on ISS Dark Matter, Antimatter,Strangelets,…

?

Hubble SpaceTelescope

Galacticsurvey

Curvature of the universe, dark energy

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

(1960’s)

(1970’s)

(1970’s)

(1980’s)

(2000)

(1990’s)

Nuclear force30 GeV Proton Accelerator

400 GeV Proton Accelerator

Electron Positron Collider

Electron Positron Collider

Large Underground Cave

CERN

Neutral Currents(1960’s) Nuclear force30 GeV Proton Accelerator

Two types of cosmic rays in space

2- Charged cosmic rays: A nearly unexplored region in science.A magnetic spectrometer (AMS) on ISS is the only way to provide long duration (20 years), high precision measurements of charged cosmic rays.

Fundamental Science on the International Space Station

1- Light rays have been measured (e.g., COBE, HUBBLE, INTEGRAL, FERMI,HERSCHEL, WMAP, PLANCK, ….) for over 50 years. Fundamental discoveries have been made.

AMS