ams as an astroparticle physics experiment 제 4 회 고에너지물리 여름학교 6 월 19 일 (...
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AMS as an Astroparticle Physics ExperimentAMS as an Astroparticle Physics Experiment
제 4 회 고에너지물리 여름학교
6 월 19 일 ( 토 )
김 귀년
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Astroparticl Physics is
Connecting Quarks with the Cosmos
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Periodic System of Elementary ParticlesPeriodic System of Elementary Particles
e-N eutrino e
-N eutrino
E lec tron eMuon Tau
C harge -1 C harge 0D ow n
B ottom
U p uC harmTop
C harge +2/3 C harge -1/3
ct b
sd1st Family:
2nd 3rd
G ravitation
Weak Interac tion
E lec tromagnetic Interac tion
S trong Interac tion
Family:Family:
uudduu
uudd dd NeutronNeutronNeutronNeutron
ProtonProtonProtonProton
e-N eutrino e
-N eutrino
E lec tron eMuon Tau
C harge -1 C harge 0D ow n
B ottom
U p uC harmTop
C harge +2/3 C harge -1/3
ct b
sd1st Family:
2nd 3rd
G ravitation
Weak Interac tion
E lec tromagnetic Interac tion
S trong Interac tion
Family:Family:
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Inflation(Big Bang plus
10-34 Seconds)
Big Bang plus 300,000 Years
Big Bang plus 15 Billion Years
What Powered the Big Bang?
Nowgravitational waves
light
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What is the Dark Energy?
We do not know what 95% of the universe is made of!
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Cosmic Rays
What are cosmic rays? Elementary particles,
nuclei, EM radiation of extra-terrestrial origin, including , ,
At the edge of the Earth's atmosphere
50% protons, 25% , 13% C/N/O nuclei, <1% e-, <0.1%
Discovery of cosmic rays Victor. F. Hess, Nobel Prize
in 1936
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Where Cosmic Ray come from? Where Cosmic Ray come from?
S. Swordy
CR ASTRONOMY
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Cosmic Rays composition in spaceCosmic Rays composition in space ~88% proton, ~ 9% He nuclei, ~88% proton, ~ 9% He nuclei,
~1% Z > 2 nuclei, ~ 2% electrons, <0.1% gamma~1% Z > 2 nuclei, ~ 2% electrons, <0.1% gammaDevelopment of Cosmic-Ray Air-Shower
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AMS AMS 실험은실험은
국제우주정거장에서 수행되는 세계최초의 고에너지물리실험국제우주정거장에서 수행되는 세계최초의 고에너지물리실험 20072007 년 년 77 월에 국제우주정거장월에 국제우주정거장 (ISS) (ISS) 설치되어 설치되어 3-5 3-5 년 동안 수행년 동안 수행 1414 개국 개국 4646 개 기관의 개 기관의 200200 명 이상의 과학자와 산업체가 참여하는 명 이상의 과학자와 산업체가 참여하는
다국적 국제공동연구다국적 국제공동연구
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International CollaborationInternational Collaboration~200 scientists + dozens of contractors from 14 countries
Spokesperson: TING, Samuel C. C.
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AMS 02 AMS 02 검출기의 특징검출기의 특징
► 우주에서 수행되는 최초의 고에너지 물리실험 검출기로서 3-5 년 동안 무인 우주실험에 사용됨으로 여러 가지 제약 점이 있다 .
질량 : 6200 kg 이내크기 : ~ 3.2 x 2.7 m소모전력 : 2 kW 이내이륙시 중력가속도 : 9 g작동온도 범위 : -180o + 50oC유출 기체 한계 : <10- 12 g/s/cm2
Trigger rate: ~ 200 HzData rate: ~ 3 Mb/s
질량 : 6200 kg 이내크기 : ~ 3.2 x 2.7 m소모전력 : 2 kW 이내이륙시 중력가속도 : 9 g작동온도 범위 : -180o + 50oC유출 기체 한계 : <10- 12 g/s/cm2
Trigger rate: ~ 200 HzData rate: ~ 3 Mb/s
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AMS02 : technological challengeAMS02 : technological challenge
AnticoincidenceAnticoincidence: veto plastic scintillators used in Trigger
Time of FlightTime of Flight: 2x2 planes of scintillator hodoscopeResolution T=120 ps .
Used in Trigger Velocity measurement L/ct1-ct2 /3.5% E/dx measurements
TrackerTracker : 8 planes of double sided Silicon (6 m2). 110 and 208 pitchResolution =17 in bending plane and 30 non bend.
Rigidity pc/Ze=0.3BR measurements up to ~3 TeVdE/dx ~ Z2 measurement.Conversion of gamma e+e-
Superconductive Magnet:Superconductive Magnet: B
dipol =0.87 Tesla I~459A
Size: d=1.2m l=0.8 m; Mass 2.3 tcooled to 1.8K by superfluid He (2500 l)
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AMS02 : technological challengeAMS02 : technological challenge
Ring Image Cherenkov Detector:Ring Image Cherenkov Detector: radiators (NaF n=1.336 and Aerogel n=1.035) +PMT's
velocity measurements (up to 20 GeV / 0.1%) Absolute charge measurements N
photons~Z 2 (=0.2)
up to Z=26
Electromagnetic Calorimeter:Electromagnetic Calorimeter: Pb+ scintillators fibers readout by 324 PMT's (2x2cm readout granularity)Overall 18 x-y planes. Size 65x65 cm2 . Weight 640 kg. Thickness ~16 X
o and ~ 0.5
nucl. .
Energy measurements for leptons dE/E=0.03+0.13/E[GeV]
Used in gamma triggere, / h separation ~10 3 E=1-1000 GeV
Transition Radiation Detector:Transition Radiation Detector: 20 layers of 6 mm straw tubes(Ntot=5248) filled with Xe/CO2 (44 kg Xe+3.7kg CO2) interposed with fleece radiator (22 mm).
dE/dx measurements .Separation e/h ~10 3 - 10 2 p=1-250 GeV
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AMS AMS 실험 목적은실험 목적은 우주에서의 반물질 검색우주에서의 반물질 검색 (( 세계 최고의 감도로세계 최고의 감도로 , , 세계 최초세계 최초 ))
– 우주 대폭발 ( 빅뱅 ) 시 물질 / 반물질 비 =1– 현재 우주는 대다수 반물질이 아닌 물질로 구성– 만일 100 억분의 하나가 반물질로 자연에 존재할 경우 , 이를 측정하고자 함 .– 현재 한계는 < 1.1 x 10-6 ( <100 GeV) - AMS 01 실험과 BESS 실험에 의하여
암흑물질 암흑물질 (( 우주물질의 우주물질의 90%90% 가량가량 ) ) 탐색탐색 (( 우주에서 직접 수행하는 세계 최초 실우주에서 직접 수행하는 세계 최초 실험험 ))– 암흑물질의 충돌로 반물질인 반양성자 , 양전자 , 광자 등이 다수 생성되며 ,– 이들의 스펙트럼에 bump 로 나타남 .– 따라서 , 반물질의 스펙트럼을 측정
우주선의 기원에 대한 연구우주선의 기원에 대한 연구 (( 직접 우주에서 수행하는 첫 실험직접 우주에서 수행하는 첫 실험 ))– 갤럭시 내에서 입자전파 현상에 대한 정보 제공 – 109 동위원소를 측정 (D, He, Li, Be, B, C 등 )– 이들의 측정 시 배후과정인 보통의 우주선 측정
직접 직접 s s 쿼크들로 구성된 쿼크들로 구성된 strangeletstrangelet 를 탐색를 탐색 (( 가설을 최초로 검증가설을 최초로 검증 ))– Strangelet 는 중성별과 같이 보통의 상태에서는 존재하지 않은 특별한 상태의 물질– S 쿼크는 실험실에서만 검출되었음
고에너지 감마선 검출고에너지 감마선 검출 (( 최고 에너지의 감마선 측정 능력 보유최고 에너지의 감마선 측정 능력 보유 ))
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Is the Universe Composed only of Matter?
How to explain Baryon Asymmetry?Principles of Baryogenesis (D.Sakharov 1967)three conditions have to be fulfilled: non-conservation of baryons Violation both C and CP Deviation from thermal equilibruim
Different models of baryogenesis:✔Grand Unified Theory (GUT) inspired (D.Sakharov)✔SUSY condensate (I.Afleck et al)✔Spontaneous baryogenesis (A.Cohen et al)✔ Etc
Local domains of antimatter are not excluded by baryogenesis.antistars, antiblackholes...
Present bounds are coming from gamma rays and CMB spectra lB>10 Mpc
Unambiguous proof would be an observation of heavy (Z>=2) anti-nuclei in Cosmic rays (A.Dolgov et al)
Anti-matter Domain
Anti-CR
Us
Matter Domain
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(1) Indirect Search for Antimatter: Photons
If the Universe contains regions of antimatter and matter,annihilation radiation at the boundaries should occur viathe process:
This should result in:• a distortion of the cosmic microwave background (COBE measures a quite isotropic blackbody radiation for a distance up to about 10 Mpc)• a signal in the extragalactic diffuse -ray background induced by the (redshiffed) annihilation photons.Non-observation of this radiation excludes large zones of antimatter in our supercluster of galaxies.
sesNN ',,',0
ee
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(2) Direct Searches for Antimatter
Antiproton measurements do not provide evidence for extragalactic antimatter.
The p-flux near the earth can be explained mainly by secondary interactions of cosmic rays depending on: - incident spectra - interstellar gas composition - solar modulation at lower energies
However the probability to produce antinuclei by high energy interactions falls drastically with the amount of antinucleons. (more than 104 per antinucleon) - Discovery of antinucleus (e.g. antihelium) evidence for cosmologically significant amounts of antimatter. - Discovery of anticarbon nuclei antistars ?
Up to now, No antinucleus with Z2 has ever been found in the cosmic radiation.
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NHe/NHe = 1.1·10-6 , R ( pc/Ze)<100 GVSame spectrum for He, He
Any Spectrum from He
Antihelium Search (AMS 01 Results)(Ref. Phys. Lett. B461(1999)387-396)
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Antimatter Search Results for Heavier Nuclei
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AMS02 discovery potential : AntimatterAMS02 discovery potential : Antimatter
Antimatter search Negative Z >=2 nuclear background He
secondary /He < 10 -12 ;
AMS01 limit 10 – 6, AMS02 expected ~10 -9 is limited by statistics
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Dark Matter Search Dark Matter Search
►Direct search: nuclear interactions with detector (ground based experiments)► Indirect search: products of annihilation (in Space )
AMS 02 -indirect Search for the relic Dark Matter in Space
Supersymmetric Dark Matter is a prime candidateLightest Supersymmetric(mSUGRA) Particle (LSP) is heavy (>100GeV) stable (R parity conserved)weakly interacts with baryonic matter (WIMPS) < 10-42 cm2
can annihilate and produce stable SM particles (p,antiprotons, e+.e-, )
Different candidates : axions, magnetic monopoles etc.
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Neutralino Dark MatterNeutralino Dark Matter
Properties of Neutalino Mass: ~ 100 GeV
Interactions: weak
The “typical” WIMP (but note: neutralinos are Majorana fermions – they are their own anti-particle)
• Direct detection: see Prof. S. Kim’s talk
• Indirect detection: annihilationin the halo to e’s: AMS-02, PAMELA…
in the center of the galaxy to ’s: GLAST, AMS/, telescopes,…
in the center of the Sun to ’s: AMANDA, NESTOR, ANTARES,…
Neutralinos:
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Supersymmetric Dark MatterLSP is a bino-like neutralinoneutralino is a spin ½ Majorana particle and can annihilate
Neutralino is the Dark Matter candidate.
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Signature of Dark Matter: eSignature of Dark Matter: e++, p, , p,
Background Cosmic Ray spectra is dominant by SM stable particles : p, He, e-Have chance to see signal from annihilation in e+, p and components where backgrounds from nuclear interactions is smaller.
Flux for i -component is :
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Annihilation of neutralino
Monochromatic gamma lines E =m m mz
2/4m
Signal signatures : cross sectionsSignal signatures : cross sections
After hadronization and decays ->stable particles with continuum spectra
< eff
V> thermal averaged cross section depends strongly on tan , m
1/2 (m~0.4m
1/2, s~1/m
2) and m
o
Tree diagrams
1 loop diagrams
Dominant channel>90%
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Hard Positron SignalHard Positron SignalTurner, Wilczek (1990)
Kamionkowski, Turner (1991)
Best hope: e+e- If are Majorana-like ( Pauli Jinit = 0), This process is highly suppressed
Next best hope: W+W-, ZZ e+…Problem: conventional wisdom in simple models,≈ B
ino, does not couple to SU(2) gauge bosons
We are left with soft e+: bb ce+n…
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AMS02 discovery potential : Dark MatterAMS02 discovery potential : Dark Matter
Hard PositronsMost promising channel.Specific bump at ~ 5-100 GeV.Small contamination and large significance
A.Baltz et al. Astro-ph/9808243MSSM scan
Signal flux is ~ 1/m4 . For the high m one
needs larger Boost factors to see signal
m=130 GeV m=336 GeV
(by V. Zhukov University of Karlsruhe)
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AMS02 discovery potential : DarkMatterAMS02 discovery potential : DarkMatter
Antiprotons AntiDeutronsDifficult case since the shapes of the signal and background are similar and at the low energy part(<10GeV) flux is prone to the solar modulation and the background is not well defined
p+n->d Significance can be better than for antiprotons
(by V. Zhukov University of Karlsruhe)
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Signal signatures : DM halo profile Signal signatures : DM halo profile
From rotation curves - neutralino is spherically distributed around galactic center.Navarro, Frenk, White type Dark Matter halo profile :
define the slope
0 - local density 0.3-0.7 GeV/cm3
a -scale parameter (depends on 0)
We are here ro~ 8kpc
Local 'clumps ' of DM can significantly increase signal from the Dark Matter annihilation (Boost factors)
J.F.Navarro Et al Ap.J.462(1996)
L.Bergstrom et al astro-ph/9806072
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Composition and Energy Spectrum of Conventional Cosmic Rays
The relative abundance of particles, elements and isotopes is related to:• Primordial nucleosynthesis for the particles created just after the Big-Bang:
• Astrophysical sources accelerating primary particles:
• Interactions with interstellar gas create secondaries:
(Spallation), 10Be/9Be ratio depends on propagation time• Propagation described by the Leaky Box model
LiHeHeDep 734 ,,,,,,
FeOCHepe ,,,,,
BBeLippe ,,,,,
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AMS02 discovery potential : CR compositionAMS02 discovery potential : CR composition
AMS 02 will measure chemical compositions up to ~1 TeV/nand will constrain a propagation model.
Propagation model:- describes propagation (diffusion, convection, reacceleration) of cosmic ray particles in galaxies- calculates nuclear interaction of primary produced particles with interstellar medium(ISM)
Predicts abundances of element. Estimates backgrounds.
I.Moskalenko and A.Strong Astro.J 509 (1998)
Main parameters of the model:diffusion constant, size of ISM disk, density of the ISM, reacceleration speed, etccan be fixed by ratios of abundances
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AMS02 discovery potential : CR compositionAMS02 discovery potential : CR composition
1 year
10Be (t1/2
=1.5myr) / 9Bewill allow to estimate thepropagation time andsize of the ISM
B is secondary produced in nuclear interaction, C is primary produced in stars. B/C is sensitive tothe diffusion constant
3He/4He ratio is sensitive to the densityof the ISM
6 months 1 day
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High Energy -ray Physics
• Astrophysical sources of -rays:
- point sources: blazars, GRBs, and pulsars - diffuse sources: ray background, from WIMP annihilation
GRBsGRBs
PulsarsPulsarsAGNsAGNs
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Gamma ray astrophysics powerful tool to test the Univers
AMS02 discovery potential: Gamma AMS02 discovery potential: Gamma astrophysicsastrophysics
Detailed study of gamma spectrum.Extra Galactic F ~ E-2.7 and galactic component F ~ E-2.1
Probe the model of gamma rays production and propagation.
Study gamma rays profile vs galactic latitude and longitude.
●● Gamma from neutralino annihilation reflects the DM halo profile.
Monochromatic lines from neutralino annihilation->at E=m can
constrain the clumpiness.Experimental data , models and AMS02 projection
Diffuse gamma spectrum up to few hundred GeV
A.W.Strong Et al. Astr.J.537 (2000)
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AMS02 discovery potential : Gamma astrophysicsAMS02 discovery potential : Gamma astrophysics
Point sources: Active Galactic Centers(AGN), pulsars etc.EGRET(1991) third source Catalog
Point like sources observed by EGRET at E<30GeV 271 sources >100MeV
AMS02 angular resolution:< 2.5o ECAL mode E>10GeV< 0.1o Tracker conversion E >10GeV(EGRET 2-3o GLAST 0.1o)Acceptances: A(=0) 1750 cm2 ECAL
450 cm2 Tracker conversion (EGRET 1500cm2,GLAST 12000 cm2)
Time variable point sources: Gamma Ray Bursts(GRB), blazars
Source identification at E>20GeV
Energy spectra of sources
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Sensitivity of –ray detectors
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Energy vs Time for X and Gamma ray detectors
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SummarySummary
• AMS-02 : an exciting challenge - Cosmic rays will be measured with order of magnitude higher precision than before and up to the TeV region - Search for antinuclei (antihelium sensitivity: 10-9) - Search for dark matter - High energy gamma ray physics (0.3 < E<100 GeV)
- Physics beyond the standard model- Astrophysics- Strangelets and other exotics- ????
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The Space Experiment PAMELAThe Space Experiment PAMELAMirko Boezio – INFN TriesteMirko Boezio – INFN Trieste
The Satellite: Resurs DK1The Satellite: Resurs DK1
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TRDTRD
CalorimeterCalorimeter
ToFToF
AnticoincidenceAnticoincidenceshieldshield
Shower tail catcher Shower tail catcher scintillatorscintillator
Magnetic Magnetic spectrometespectrometerr
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PAMELA StatusPAMELA StatusDetectors are ready and compling with the design performances
Detectors tested at PS / SPSTest facilities as Prototypes and in FM configuration
Mass/Termal ModelsQualified, March-May 2003
Integration of PAMELA TechnologicalModel completed and delivery toRussia underwayIntegration of PAMELA FMunderway at INFN – Roma2
The PAMELA Launch is in 2004 from Baikonur
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PAMELA CapabilitiesPAMELA Capabilities
PAMELA will explore:Antiproton flux 80 MeV - 190 GeVPositron flux 50 MeV – 270 GeVElectron flux up to 400 GeVProton flux up to 700 GeVElectron/positron flux up to 2 TeVLight nuclei (up to Z=6) up to 200 GeV/nAntinuclei search (sensitivity of 10-7 in He/He)
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Cosmic-ray Antimatter SearchCosmic-ray Antimatter Search
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AGNsAGNs
SNRsSNRs Cold Dark MatterCold Dark Matter
PulsarsPulsars
GRBsGRBs
Tests of Quantum Tests of Quantum Gravity effectsGravity effects
Cosmological Cosmological -Ray Horizon-Ray Horizon
The MAGIC Physics TopicsThe MAGIC Physics Topics
Origin of Origin of Cosmic Cosmic RaysRays