9/26/2006 Katsushi Arisaka, UCLA 1

Katsushi ArisakaKatsushi Arisaka

University of California, Los Angeles

Department of Physics and Astronomy

arisaka@physics.ucla.edu

Unveiling the Mystery of Ultra High Energy Cosmic

Rays

Unveiling the Mystery of Ultra High Energy Cosmic

Rays

9/26/2006 Katsushi Arisaka, UCLA 2

Energy Spectrum of Cosmic Rays

• Energy Spectrum ~ E-3

• The spectrum extends beyond 1020 eV (=1011 GeV =100 EeV).

• Beyond 1020 eV, Flux is only one particle per km2-century.

TeVGeV EeVPeV

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Talk Outline

Physics Motivation Why is 1020 eV so special?

Past and Ongoing Experiments AGASA HiRes Pierre-Auger

Preliminary Results from Pierre-Auger Energy Spectrum Composition Angular Distribution

Future Projects

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Physics Motivation

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Particle Physics in Early Universe

10-45sec

10-40

10-35

10-30

10-25

10-20

10-15

10-10

10-5

105 sec

1

1 year103

106

109 year

Time (sec)

Temp. (oK)

1018

1015

1012

109

1PeV

1TeV

1GeV

1MeV

1KeV

1eV

1030

1025

1020

1015

1010

105

1

Energy (GeV)

10-3eV

Planck

EW

Now

GUT

Gra

vit

atio

n

Str

on

g

We

ak

Ele

ctr

om

agn

eti

c

FundamentalInteraction

Ele

ctr

o-W

eak

GU

T

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Particle Physics in Early Universe

10-45sec

10-40

10-35

10-30

10-25

10-20

10-15

10-10

10-5

105 sec

1

1 year103

106

109 year

Time (sec)

Temp. (oK)

1018

1015

1012

109

1PeV

1TeV

1GeV

1MeV

1KeV

1eV

1030

1025

1020

1015

1010

105

1

Energy (GeV)

10-3eV

Planck

EW

Now

GUT

Super Symmetry

Super StringQuantum GravityGrand Unification

Inflation

Dark Matter

Dark Energy

Big Bang!

Baryogenesys

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Particle Physics in Early Universe

10-45sec

10-40

10-35

10-30

10-25

10-20

10-15

10-10

10-5

105 sec

1

1 year103

106

109 year

Time (sec)

Temp. (oK)

1018

1015

1012

109

1PeV

1TeV

1GeV

1MeV

1KeV

1eV

1030

1025

1020

1015

1010

105

1

Energy (GeV)

10-3eV

Planck

EW

Now

GUT

Accelerator

Telescope

UHE Cosmic Rays

Inflation

Dark Matter

Dark Energy

Big Bang!

Baryogenesys

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Top-down or Bottom-up?

10-45sec

10-40

10-35

10-30

10-25

10-20

10-15

10-10

10-5

105 sec

1

1 year103

106

109 year

Time (sec)

Temp. (oK)

1018

1015

1012

109

1PeV

1TeV

1GeV

1MeV

1KeV

1eV

1030

1025

1020

1015

1010

105

1

Energy (GeV)

10-3eV

Planck

EW

Now

GUT

Big Bang

Active Galactic Nuclei

Gamma Ray Burst

Supernova Neutron Star Black Holes

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The Extreme Universe

Pulsar

GRB

AGN

SNR

Radio Galaxy

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Possible Acceleration Sites

• Several possible accelerators in nature up to 1020 eV.

• Extremely difficult to accelerate above 1020 eV.

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Interaction Length of UHE Protons

Blasi, astro-ph/0307067

PhotopionLoss Length

InteractionLength

PairProduction

10Mpc

1Gpcp + (2.7oK) p + ’s

GZK Cutoff

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E=1019 eVE=1020 eV E=1018 eV

Trajectory of Protons in the Galaxy

Galactic Magnetic Field ~ 2 µG

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Deflection of Protons >41019eV

Dolag, astro-ph/0310902

0o360o

< 100 Mpc Extra Galactic Magnetic Field ~ 1 nG

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1019 eV

1021 eV

1020 eV

1018 eV

Top-Down?

GZK?

Bent by Extra-Galactic B (~nG)

Ankle

Charge Particle Astronomy

Trapped by Inner-Galactic B (~G)

Bottom-Up

UHE Gamma Rays

UHE Neutrinos

Straight Trajectories

?

Rich Physics and Astronomy

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Past and Ongoing Experiments

AGASAHiResPierre-Auger

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Detection Technique

e

Fluorescence Fluorescence Detector (FD)Detector (FD)

10km

~ 27Xo

~ 11I

MC Simulation of 1019eV Proton Shower

Surface Detector (SD)

AGASA

HiRes

Pierre-Auger

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SD vs. FD

SD (Surface Detector) used by AGASA. Operational 24 hours a day, but Sparse sampling at the tail of shower.

FD (Fluorescence Detector) used by HiRes. Totally calorimetric energy measurement, but ~10% duty factor (only at moonless night).

Pierre-Auger utilizes both!

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Akeno Giant Air Shower Array

0 4km

• 111 Electron Detectors• 100 km2

• 27 Muon Detectors• Operation 1991 - 2004

M. Teshima

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The Highest Energy Event by AGASA

2.5 x 102.5 x 1020 20 eV on 10 May 2001eV on 10 May 2001

M. Teshima

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Energy Spectrum by AGASA

M. Teshima

Bottom-upwith GZK Cutoff

Top-down?

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Two HiRes Detectors HiRes1 21 mirrors, 1 ring 3o < altitude < 17o

HiRes212.6 km SW of HiRes1.42 mirrors, 2 rings3o < altitude < 31o

G. Thomson

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Stereo View by HiRes 1 & 2

C. Finley

HiRes 1

HiRes 2

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Energy Spectrum by HiRes

Consistentwith GZK Cutoff

C. Finley

(1999-2004)(1996-2005)

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Energy Spectrum by HiRes

C. Finley

Consistent withGZK Cutoff !!

Galactic

Extra-Galactic

(1999-2004)(1996-2005)

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Energy Spectrum

Ralph Engel

AGASA (SD)

HiRes (FD)

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Pierre-Auger

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Pierre Auger Collaboration

15 Countries 50 Institutions~350 Scientists

Italy Argentina

Czech Republic Australia France BrazilGermany Bolivia* Poland MexicoSlovenia USASpain Vietnam* United Kingdom

*Associate Countries

Jim Cronin Alan Watson

Founders

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#S

#SS

Pierre-Auger Observatory

N

Northern Augerin Colorado

Southern Augerin Argentina

50km

9/26/2006 Katsushi Arisaka, UCLA 2950km

Southern-Auger in Argentina

Surface Detector 1600 Water Tanks 1.5 km spacing 3100 km2

Fluorescence Detector 4 Telescope Sites 6 Telescopes per Site 24 Telescopes Total

9/26/2006 Katsushi Arisaka, UCLA 30Aerial view of Los Leones Fluorescence Site

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Six Telescopes looking at 30o x 30o each

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corrector lens

Camera440 PMTs

11 m2 Mirror

UV-Filter 300-400 nm

Corrector Ring

Optical

Shutter

9/26/2006 Katsushi Arisaka, UCLA 34Tanks aligned seen from Los Leones

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Water Tank on Site

Real water tank under operation at Malargue

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Installing Electronics

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Southern Auger as of Sept. 2006

50km

1100 Water Tanks (out of 1600)~ 20 x AGASA

AGASA

Los Leones

Coihueco

Los Marados

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All the rest will be deployed by Summer of 2007

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Comparison of Integrated Aperture

100

1000

10000

100000

1000000

1985 1990 1995 2000 2005 2010 2015 2020Year

Inte

gra

ted

Ap

ertu

re (

km2 *s

tr*y

ear)

Fly'e Eye

AGASA

HiRes

Auger-S

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A Typical Event (“Young” Shower, Zenith~35o)

203

204

116

114S(1000)~81019eV

S(1000)~71019eV

203

204

116

114

215

217

Lateral Distribution Function

206

1.05

( ) 1700 700

(1000) sec

r rS r k

m m

E S f

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A Typical Event (“Young” Shower, Zenith~35o)

EM

EM

Muon

Muon

203

204

116

114

203

204

215

217

(nsec)

S(1000)~71019eV

Muon

EM

EM

Muon

217

215

Lateral Distribution Function

206

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A Typical Inclined Event(“Old” Shower, Zenith~72o)

Muon

~61019eV

Direct Cherenkovon PMT 1

Muon

Lateral Distribution Function

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A Stereo-Hybrid Event (Zenith~70o)

Fluores.Telescope

Fluores.Telescope

~81019eV

Lateral Distribution Function

26 June 2004

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A Stereo-Hybrid Event (Zenith~70o)

Coihueco

Los Leones

Fluores.Telescope

Fluores.Telescope

26 June 2004

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A Stereo-Hybrid Event (Zenith~70o)

Los Leones

Pulse findingTime vs fit

Coihueco

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A Stereo-Hybrid Event (Zenith~70o)

Coihueco

Los Leones

Time vs fitShower Profile

~61019eV

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Preliminary Results

Energy SpectrumCompositionAngular Distribution

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Energy Spectrum

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S(1000) at 38o vs. FD Energy

S(1000) at 38o

1 EeV 10 EeV 100 EeV

50

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Proton, SIBYLL (AIRES)

Proton, QGSJET (AIRES)

Proton, GEISHA, QGSJET (CORSIKA)

Proton, FLUKA, QGSJET (CORSIKA)

Proton, GEISHA, QGSJET2 (CORSIKA)

Proton, FLUKA, QGSJET2 (CORSIKA)

Iron, SIBYLL (AIRES)

Iron, QGSJET (AIRES)

50

34

(VEM)

SD+MC Average ( 18%)

FD Average ( 30%)

Fixed Beta

Floating Beta

Proton, SIBYLL (AIRES)

Proton, QGSJET (AIRES)

Proton, GEISHA, QGSJET (CORSIKA)

Proton, FLUKA, QGSJET (CORSIKA)

Proton, GEISHA, QGSJET2 (CORSIKA)

Proton, FLUKA, QGSJET2 (CORSIKA)

Iron, SIBYLL (AIRES)

Iron, QGSJET (AIRES)

Summary of S(1000) at 38o and 10 EeV

Proton

Iron

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Energy Spectrum E3 (FD Energy)

Presented at ICRC 2005(only one year of data)

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Energy boosted by 30%

Energy Spectrum E3 (SD+MC Energy)

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Summary of Energy Spectrum

Energy spectrum based on FD Energy is consistent with HiRes. fits reasonably well with the GZK cutoff. Injection spectrum of 1/E2.6.

Energy spectrum based on SD+MC Energy is similar to AGASA. a hint of Super-GZK events? but not as many as AGASA observed.

Possible Causes: FD: Poor measurement of fluorescence photon yield. SD: MC can not produce enough number of muons.

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Composition

Constant Intensity CutPhoton Flux LimitNeutrino Flux Limit

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Constant Intensity Cut

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S(1000) vs. Sec()

60o45o30o 38o

50 VEM

34 VEM

SD+CIC

Iron

Proton

Photon

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S(1000) MC/CIC vs. sec() at 10 EeV

60o45o30o 38o

FD+CIC

SD+CIC

Sensitive to Xmax

Sensitive to Muon Richness

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Muon Richness vs. Xmax

Iron/QGSJET

Iron/SIBYLL

Proton/QGSJET

Proton/SIBYLL

Gamma/QGSJETGamma/SIBYLL

CICXmax Proton likeMuon Richness Iron like

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Photon Limit

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What is Dark Matter?

Super HeavyDark Matter

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Super Heavy Dark Matter fit to AGASA

Photon flux can be predicted by decay of Super Heavy Dark Matter based on AGASA data

Gelmini, et al, astro-ph/0506128

AGASA Data

Bottomup Proton

P from SHDM

from SHDM

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Photon (MC Simulation)

Photon (> 10 EeV)

Muon Rich Muon Poor

Dee

p X

max

S

hallo

w X

max

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Proton (MC Simulation)

Proton (> 20 EeV)

Muon Rich Muon Poor

Dee

p X

max

S

hallo

w X

max

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Expected Photon Fraction Limit

Super Heavy Dark Matter

Topological Defects

Z Burst

Expected Limit

GZK Photons

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Expected Sensitivity on Photon Flux

Expected Limit

Super Heavy Dark Matter

Topological Defects

Z Burst

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Future Sensitivity on Photon Flux

Topological Defects

Z BurstExpected Limit

2010

2015

Super Heavy Dark Matter

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Summary of Photon Limit

Pierre-Auger Observatory Surface Detector is a background free photon detector. Extremely sensitive to top-down models.

Pierre-Auger already has enough data to test top-down models inspired by the AGASA spectrum. Analysis of real data is being prepared for

publication.

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Neutrino Limit

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Detection of Neutrino

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Neutrino Sensitivities (per year)

by Dmitri Semikoz

AGNCore

ExoticHadron

GZK(Max)

GZK(W&B)

TopDown

AUGER

AUGER e

ICECUBE

AMANDA II

ANITA 30 days

ray BoundRICE

Atmospheric

EUSO

Strong DIS

No DIS

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Angular Distribution

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Clustering of UHECR (>40 EeV) by AGASA

• 6 doublets and 1 triplet within 2.5o cone.

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AGASA Auto-Correlation

40 EeV 2.5o

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HiRes Correlation with BL Lacs

Gorbunov et al., astro-ph 0406654

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Six combinations were tested with independent data (with m<18):

Note: These are not independent results: the samples overlap. Analysis has been a posteriori, so F values are not true probabilities. Must be tested with independent data

R.U. Abbasi et al., Astrophys.J. 636 (2006) 680 [astro-ph/0507120]

New HiRes Analysis

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Angular Resolution of Auger SD

>10 EeV

>3 EeV

>1 EeV

HiRes (Stereo)

AGASA

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AGASA Galactic Center

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Auger Galactic Center

AGASA

Sugar

G.C

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Summary of Auger

Pierre-Auger is finally a reality. SD: 30 times larger than AGASA. (2/3 complete) FD: 4 stations of HiRes-like telescopes. (3/4 complete.)

Hybrid observation is giving critical information to determine the energy and composition. Why AGASA and HiRes differ ~30% in energy? Cosmic rays appear much richer than expected!

New physics results are expected soon. Energy Spectrum Photon and Neutrino limits, or discovery! Clustering, BL Lac correlation…

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Future Projects

TAAuger-NorthEUSO

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TA(Telescope Array)

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3 x Fluorescence StationsAGASA x 4

576 CountersAGASA x 9

Low Energy Extension

TALETALE

Comm. Tower

CLF

Millard County in Utah / USA

M. Fukushima

9/26/2006 Katsushi Arisaka, UCLA 84M. Fukushima

9/26/2006 Katsushi Arisaka, UCLA 85M. Fukushima

9/26/2006 Katsushi Arisaka, UCLA 86M. Fukushima

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350 assembled in Utah in Feb - Mar 2006, 150 to be produced after July18 test-deployed. 500 to be deployed in several batches this year.

M. Fukushima

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Auger-South Upgradeand Auger-North

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1019 eV

1021 eV

1020 eV

1018 eV

Top-Down?

GZK?

Bent by Extra-Galactic B (~nG)

Ankle

Charge Particle Astronomy

Trapped by Inner-Galactic B (~G)

Bottom-Up

Straight Trajectories

?

Original AugerSD

Hybrid

Infill + 2-FD

Auger-South

Expanded Auger

Auger-North

Future Expansion of Auger

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Auger-North in Colorado State

Colorado State

Auger-North

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Auger-North

Total area: 10,000 km2

100 x AGASA 3 x Auger-South

4000 surface detector 1 mile (1.6 km) spacing 84 x 48 mile rectangle

Lamar

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Pruitt Mound in Colorado Site

View to west, Sept 23, 2003

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Neutrino Sensitivities

by Dmitri Semikoz

AGNCore

ExoticHadron

GZK(Max)

GZK(W&B)

TopDown AUGER (S+N, 5 years)

AUGER

AUGER e

ICECUBE

AMANDA II

ANITA 30 days

ray BoundRICE

Atmospheric

EUSO

Strong DIS

No DIS

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EUSO(Extreme UniverseSpace Observatory)

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Observation Principle of EUSO

F. Kajino

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JEM-EUSO Telescope at ISS

JEM-EUSO Telescope will be attached to Exposure Facility of Japanese Experiment Module (JEM/EF) of ISS in about 2012.

Vertical Mode Tilted Mode

Larger effective area with ~45°tiltF. Kajino

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JEM-EUSO Telescope Structure

Multi-pixel PMT

Electronics

Fresnel Lens

F. Kajino

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Shower Image on the EUSO Focal Surface

Y

X

20 events of 1020eV proton showers are superimposed on the EUSO focal surface with 192 k pixels.

x-t view y-t view

F. Kajino

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Summary

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Comparison of Integrated Aperture

100

1000

10000

100000

1000000

1985 1990 1995 2000 2005 2010 2015 2020Year

Inte

gra

ted

Ap

ertu

re (

km2 *s

tr*y

ear)

Fly'e Eye

AGASA

HiRes

Auger-S

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Comparison of Integrated Aperture

100

1000

10000

100000

1000000

1985 1990 1995 2000 2005 2010 2015 2020Year

Inte

gra

ted

Ap

ertu

re (

km2 *s

tr*y

ear)

Fly'e Eye

AGASA

HiRes

Auger-S Auger-N

Auger (S+N)

TA

EUSO

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Conclusions

The origin of UHECR is still unknown. Any events beyond the GZK cutoff? If so, signals from the early Universe??

Pierre-Auger (South) is nearly complete. Already 2.5 years of data with partial detectors.

• ~3 x AGASA statistics Several publications expected soon.

• Energy Spectrum, Photon Limit, Angular Distribution…

More experiments will follow Auger. TA, Auger-North, EUSO…