Ultra High Energy Cosmic Rays Pierre Auger Observatory · Ultra High Energy Cosmic Rays & Pierre...

Ultra High Energy Cosmic Rays &

Pierre Auger Observatory

Angela V. OlintoKICP

The University of Chicago

Nature sends 1020 eV particles

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Pierre Auger Observatory observed anisotropic sky at theHighest Energiesthrough correlation betweenUHECRs and catalog of nearbyActive Galactic Nuclei (AGN)

Top discovery of 2007in the Physical Sciences(by Science Magazine)

New Era of Charged Particle Astronomy

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Chargeless vs ChargedCosmic Particles

Photons:1600s: G. Galilei1900s: Mount Wilson -

sets distance scaleLONG list: ground & space,from Radio to Gamma-rays

(23 o.o.m.)2008+: SKA,

JWST, GSMTCTA/AGIS, …

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Attenuation Length

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Chargeless vs ChargedCosmic Particles

Photons:1600s: G. Galilei1900s: Mount Wilson -

sets distance scaleLONG list: ground & space,from Radio to Gamma-rays

(23 o.o.m.)2008+: SKA,

JWST, GSMTCTA/AGIS, …

Neutrinos: Solar, SN87a,2008+: IceCube, Km3Net, ANITA,…Gravitons:2008+: LIGO, Virgo, LISA…

Cosmic Rays (hadrons): 1912: V. HessShort List: ground & space,from o.1 GeV to 0.1 ZeV

(12 o.o.m)UHE: AGASA, HiRes2007: Auger S -

observed anisotropies2008+: Auger N + S,

JEM-EUSO, …

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Brief History of UHECRs

1961 Volcano Ranch - John Linsley - a 1020 eV event1 Linsley = 1 km2 sr yr = L

1965 CMB 1966 Greisen, Zatsepin, Kuzmin:“cosmologically meaningful termination”

1960-1990s: Haverah Park, SUGAR, Yakutsk arrays102 L

1990- 2006: AGASA array, Flye’s Eye, HiRes fluorescence 103 L

2008: Auger South completed 104 L to 105L

2010+: Auger North, JEM-EUSO106L - GOAL

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Cosmic Magnetic Fields

Halo B?

Extra-galactic B?B < nG

γ

weak deflection

RL = kpc Z-1 (E / EeV) (B / μG)-1 EeV=1018 eV

RL = Mpc Z-1 (E / EeV) (B / nG)-1

kpc

10 kpc

strong deflection

Milky wayB ~ μG

E > 1019eV

E < 1018eV

“Known unknown”

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High Energy Cosmic Rays

OBSERVABLES:

SpectrumCompositionSky Distribution

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CR arrival directionsbefore 2007

Isotropic!

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OBSERVABLES:


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Cosmic RaySpectrum

Non-thermal Phenomena

Extreme AcceleratorsEmax > 1020 eV

Features:knee, ankle, GZK cutoff

acceleratorspropagationinteractions

E-2.7

E-3.1

12 orders of magnitude

32 o

rder

s of m

agni

tude

RH

IC

Teva

tron

LHC

Ankle(1 particle /km2 yr)

Ecm = PeV (Euhecr /ZeV)1/2 (2A)1/2

Swordy ‘02

Engel’08

knee

ankle

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Each Energyrange

tells its story

108 eV < E < 1011 eV- Solar Modulation

1011eV < E < 1017.5-18.5? eV - Galactic Propagation

1017-19eV < E < 10 20 - 2? eV - Extragalactic Sources

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Galactic Accelerato

rs

E < 1017.5-18.5? eV Galactic PropagationGalactic Sources?

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Tycho SN SNR1006

CHANDRA NASA/CXC/SAO

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HESS - TeV γ’s !

Hinton, WatsonFest, Leeds

RX J1713 - 20 σX-rays

CHANDRA

smoking guns of CR acceleration

Gamma-rays

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Galactic Accelerat

ors

E < 1017.5-18.5? eV - Galactic Propagation



SNR shock accelerationin the Galaxy?

HESS SNe

?

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Extragalactic

Accelerators

1017-18eV < E < 10 20 - 2? eV Extragalactic Sources

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Extreme Accelerators

Emax > 1020 eV

E-2.7

E-3.1Ankle(1 particle /km2 yr)


Extragalactic Accelerators?

Extragalactic

Accelerators

Challenging Acceleratorsto reach 1020 eVLHC magnetic field,radius ~ 107 km (Sun - Mercury)

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E = Ze B L

10% efficiency

1020eV Protons1020eV Iron

B(G)

L(cm)

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E = Ze B L

10% efficiency


B(G)

L(cm)

Sources?

Sources?

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E = Ze B L

10% efficiency


B(G)

L(cm)

others

GRBs

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Galaxy Jets from Black Holes?

Ultra High Energy Cosmic Ray Accelerators?

Gamma Ray Bursts?

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Neutron Stars? Magnetars?

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Highest Energies

E-2.7

E-3.1

RH

IC

Teva

tron

LHC



- Pointing- Feature

Cosmologically Meaningful Termination



GZK CutoffGreisen, Zatsepin, Kuzmin 1966

p+γcmb→ Δ+ → p + π0

→ n + π +

Proton Horizon~1020 eV

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Attenuation length

e+e–

π

Interaction length

Attenuation length

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Energy loss Features for protons Berezinsky et al. 03

modification factor: Jobs (E,z) = η(E,z) x Jinjec(E)

GZKpairredshift

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GZK Feature

E-2.7


“CosmologicallyMeaningful” Feature

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High ResolutionFly’s Eye (1997-2006)2 fluorescence telescopes

AGASA (1984-2003)100 km2 area,

111 scintillators, 1km spacing

No GZK cutoff Consistent w/ GZK cutoff

1998

GZK Effect

⇒ Spectral Feature

+ LSS⇒ Anisotropic Sky Distribution

⇒ Particle Astronomy!!!

Horizon - observed Protons

AO, Armengaud, Allard, Kravtsov ‘07

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Horizons:

Gpc

1019 eV ~ 1 Gpc

1020 eV < 100 Mpc

100 Mpc

THE SLOAN GREAT WALL

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Protons with > 1020.5 eV


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Protons with > 1020 eV


Protons with > 1019.5 eV


Charged Particle Astronomy

Window of opportunity

1019 to 1021 eV

Maximize the Statistics in this window

The Pierre Auger Observatory

The Pierre Auger Observatoryof Ultra-High Energy Cosmic

Rays

Southern site3 000 km2

Northern site20 000 km2

ArgentinaAustraliaBrasilBolivia*Czech RepublicFrance Germany ItalyMexicoNetherlandsPoland

> 300 PhD scientists f> 70 Institutions and 17 countries

PortugalSlovenia Spain UKUSAVietnam*

*Associate Countries

The First Hybrid UHECR Observatory

HIGH QUALITY

LARGE QUANTITY

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Auger South

1660 tanks in a3,000 km2

Surface Array4 FluorescenceDetector Sites

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The Surface Detector Array

1662 deployed 1640 filled1591 taking dataof the1600+ tanks, 3,000km2



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surface detector

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tanks aligned seen from Los Leones

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Cherenkov water tankAuger SD station

PMT

Plastic tank 12 m3 of clean water

Solar panel

Comms antenna

GPS antenna

battery

Diffusive white “liner”

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Tank 1660

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Example Event 1A moderate angle event 762238

Zenith angle ~ 48º, Energy ~ 70 EeV

Flash ADC tracesFlash ADC traces

Typical flash ADC trace

Detector signal (VEM) vs time (ns)

Lateral density distribution

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Example Event 2A high zenith angle event - 787469

Zenith angle ~ 60º, Energy ~ 86 EeV

Lateral density distribution

Flash ADC traces

Flash ADC Trace for detector late in the shower

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photonselectrons/positrons

muons neutrons

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γ

e±

μ±

Proton/SIBYLLProton/QGSJETIron/SIBYLLIron/QGSJET

K. Arisaka

36o25o

45o

53o

60o

0o

66o

Particle vs. zenith

Signal vs. zenith

μ±

e±

γ36o25o

45o

53o

60o

0o

66o

Proton/SIBYLLProton/QGSJETIron/SIBYLLIron/QGSJET

K. Arisaka

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view of Los Leones Fluorescence

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ture boxter UV passty curtain

corrector lens(aperture x2)

440 PMT camera 1.5° per pixel

segmented spherical mirror

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4 times 6 telescopes overlooking the site

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A Hybrid Event

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Hybrid Era

HYBRID SD only FD only

Energy A & M indep depend independ

Aperture E, A, M indep independ depend

Angular ~ 0.2o ~1-2o ~3-5o

Resolution

E = energy, A = mass, M = hadronic model

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1st - 4 Fold Hybrid Event

20 May 2007 E ~ 1019 eV

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Cosmic Ray

Spectrum

E-2.7


“CosmologicallyMeaningful” Feature

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Energy spectrum from SD showers with θ ≤60°

calib. uncert. 10%FD syst. unc. 22%

5165 km2 sr yr ~ 0.8 full Auger year

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Energy spectrum from SD showers with θ ≤60°

5165 km2 sr yr ~ 0.8 full Auger year

Exp. Obs.>1019.6 eV 132 ± 9 51

> 1020 eV 30 ± 2.5 2

calib. uncert. 10%FD syst. unc. 22%

Slope = -2.62 ± 0.03

significance = 6σ

Olinto SSI 08ankle

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High ResolutioFly’s EyeAGASA

No GZK cutoff Consistent w/ GZK cutoff

AUGER 08HiRes 2008

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Spectrum factsSpectrum facts

There is an ankle

Galactic/Extragalactic transition?

Pair-production of pure-proton source?

analyse composition!

or

There is a “cut-off”

GZK suppression?

Limit of the acceleration process? Emax

analyse arrival directions!

or

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Composition & Spectrum

Engel’08

knee

ankle

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HEAT

High Elevation Angle Telescopes

AMIGA

Auger Muon and Infill Ground Array

Auger South Low Energy Extension

Olinto SSI 0820 km

20 km

Millard CountyUtah/USA

24 x 24 Scintillators(1.2 km spacing)

AGASA x 9

3 x Fluorescence StationsAGASA x 10 by stereo

Telescope Array

Low Energy HybridExtension

Aperture1.4 103 km2 sr

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OBSERVABLES:


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Composition-sensitive observablesComposition-sensitive observables

Depth of shower maximum development: Xmax

low E high E high Elow A high Aatmospheric

depth (g/cm2)

Stochastic process large fluctuations

small fluctuations

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Composition observable:

shower maximum

Composition observable:

shower maximum

+ fluctuations in Xmax smaller for heavier nuclei

Expectations from different hadronic models

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Shower maximum over 2 decades in E

+ fluctuations in Xmax to be exploited

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111 69 25 12426

326

Large number of events allows good control and understanding of systematics

Comparison with previous studies

Comparison with previous studies

Proton Horizon

Allard

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Helium Horizon

Allard

GOOD NEWS!!

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CNO Horizon

Allard

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Fe Horizon

Allard

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Observed Composition

Allard

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Photon limit

Photon-induced showers look very different

Showers at E = 1019 eV, θ = 0º :

Top-down models predict large UHE photon flux

SHDM models: decay of super-heavy dark matter accumulated in Galactic halo

TD models: supermassive particle decay from topological defect interaction or annihilation

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Constraints on Super-Heavy Dark Matter as sources of UHECRs

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Super heavy dark matter (SHDM) models are excluded as UHECR sources!

Auger results (photon limit)Auger results (photon limit)

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Constraints on topological defects as sources of UHECRs

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Auger results (photon limit)Auger results (photon limit)

Topological defects (TD) are still possible UHECR sources

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Auger resultsAuger results TD models closer to be constrained by Auger neutrino limits

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Neutrino fluxes : Proton & Mixed

Allard et al ‘06

Emax

(see Yoshida @ PM)

Bigas Cazon 06

Cosmogenic Neutrinos

p+γcmb→ Δ+ → p + π0

→ n + π +

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OBSERVABLES:


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Auger anisotropy resultsAuger anisotropy results

Angular resolution of ~1°: good enough!

No large-scale signal (dipole) at any energy above 1 EeV

No significant excess from Galactic Center (as possibly seen by AGASA)

No signal from BL-Lacs (as possibly seen by HiRes)

e.g. α < 0.7% for 1 EeV ≤ E ≤ 3 EeV

none of the previous reports have been confirmed…

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Main Auger resultMain Auger result

Highest energy cosmic rays have an anisotropic distribution!

First evidence that CR astronomy is possible!

Correlation with z < 0.018 AGNs inthe 12th Véron-Cetty/Véron catalogue

Opening of a new era:



Study of particle acceleration in HE astrophysical sources

Multi-messenger study of sourcesHEP interactions at 300 TeV cm!

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Equal Exposure PlotArrival Directions for E>3 EeV

+25 deg

0 deg

-30 deg

-60 deg RA = 0 deg

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The 27 highest energy events

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Veron-Cetty AGNs (red dots)

Supergalactic Plane (blue line)

Swift x-ray galactic black holes (blue circles)

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Auger main anisotropy resultAuger main anisotropy result

* - VCV AGN catalogue- 27 highest energy events UHECRs

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Δθ ≤ 3.1°Δθ ≤ 3.1° z ≤ 0.018z ≤ 0.018

(D ≤ 75 Mpc)(D ≤ 75 Mpc)E ≥ 56 EeVE ≥ 56 EeV


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correlation is most significant above E = 56 EeV whre the CR flux drops…(supports GZK interpretation)


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Significance of the anisotropy resultSignificance of the anisotropy result

Véron-Cetty / Véron, 12th Edition, 2006

“This catalogue should not be used for any statistical analysis as it is not complete in any sense, except that it is, we hope, a complete survey of the literature.”

Not an “AGN correlation” result!

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Not an “AGN correlation” result!1st step: search for correlations between arrival directions of

UHECR and various source catalogues

Very large “raw significance” found w/ 12th VCV catalogue of AGNs

Did not seem to be fluctuationAuger collaboration set up a prescription for future data

Even after generous penalty factors for a posteriori searches and scanning of parameter space

(data from 2004/01/01 to 2006/05/26)

12 out of 15 events E > 56 EeV closer than 3.1° from an AGN in 12th VCV with z ≤ 0.018 (D ≤ 75 Mpc)

Most significant a posteriori “correlation signal”:

3.2 expected from isotropic distribution

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2nd step: predefine a region in the sky of excess CR flux & test if next UHECRs come from this region

Independent data set, prescribed parametersunambiguous significance

Result: 99% CL that excess in the original data set is not a random fluctuation from an isotropic CR distribution

CR distribution is anisotropic at the highest energies!

Corroborated by other analyses, independent of source catalogue

21% chance from isotropic distribution

8 correlating events out of 13 (2.7 expected)

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Astrophysical Implications?Astrophysical Implications?

Not clear yet! Very low statistics to check against any specific model

NB: no claim from Auger!

YESCan UHECRs come from AGNs?

Do UHECRs have to come from AGNs? NO!

See further analysis of the correlation, analyses with other catalogues, catalog independent anisotropy studies

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Centaurus A, Virgo, Fornax, etc.Centaurus A, Virgo, Fornax, etc.

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Centaurus A

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Centaurus A, Virgo, Fornax, etc.Centaurus A, Virgo, Fornax, etc.

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E = Ze B L

10% efficiency


B(G)

L(cm)

others

GRBs

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E = Ze B L

10% efficiency


B(G)

L(cm)

others

GRBsX

XX X



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Astrophysical Accelerators

NOT Galactic AcceleratorsNeutron Stars MagnetarsMicroquasarsshocks in the Galaxy

NOT very Distant AcceleratorsClusters of Galaxies(cluster shocks)QuasarsBL Lacs















AGN Acceleration Models

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Astro/Phys Implications

Intergalactic Fields Brms< 10-9 G (Mpc/Lc)1/2

(if) Proton Primaries on Earth (likely)300 TeV interactions - Xmax, ΔXmax, Nμ

Cosmogenic Neutrinos

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What Next?

Auger SOUTH 2007

Auger NORTH, JEM-EUSO, ….

Increase Exposure!

Armengaud

10-3/Mpc3 AN+S 7 105 L

Source Spectra

Blasi & DeMarco

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Sky Exposure Auger North

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Sky ExposureAuger North + South

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Auger North in SE Colorado

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Auger SOUTH & NORTHAuger SOUTH3,000 km2 = 1,157 mile2

Hexagonal grid -1.5 km separationFD sites - 4 (180o)

Auger NORTH 20,000 km2 ~ 8,000 mile2

SQUARE GRID -1.414 mile separation(2.26 km)

1 large PMT / tank40 FD telescopes

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Auger North FD Layout Plans

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Auger NORTH

(1 mile = 1.609 km)

1609 m

1 mile

based on the GREAT SUCESS ofAuger South Design

Enlarge Exposure& Lower Costs

SQUARE GRID -1.414 mile separation

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Apertures & Energy Threshold



Anisotropies

Auger

North

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Auger SD NORTH

Need Insulation!!!

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JEM-EUSODesign Study is ongoing in JAXA

Japanese Experiment Module of ISS in 2013Extreme Universe Space Observatory

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Nadir (2 yrs)35o tilt (3 yrs)- 3 x area, but Eth > 1020 eV

Fluorescence only~ 20% duty cycleno muons info

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Next to next generation:Free Flyers: OWL, Super EUSO, …

Free FlyerFluorescence from ABOVE!

Lind

sley

s

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Pierre Auger Project

South & Northto discover

Ultra-High Energy Cosmic Ray Sources; study

Ultra-High Energy interactions& detect

Ultra-High Energy Neutrinos

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Extra Slides

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ExtragalacticProtons

ExtragalacticMixedComposition

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Xmax Fluctuations

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