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Ultra-High Energy AstroParticles!

Angela V. Olinto

The University of Chicago

ICFA 2008

International Committee for!

Future Accelerators !

Ancient Accelerators! !


from 103 to 109 years old!


from 103 to 109 years old!

Ancient but Powerful!!

! ~ 10 TeV !

! ~ 103 TeV !

Hadrons ~ 108 TeV!!! !

How do they accelerate !

to such high energies?!

We’ll call you as soon as we know!

May take a couple of years…

Beginning to unveil the nature of !the Most Energetic Accelerators in Nature!

A New Era of AstroParticle Physics!

Multimessengers that require Multiple Techniques:

Cosmic Rays: ground arrays, atmospheric fluorescence,

balloons, satellites, space station

HE Gamma-rays: ground arrays, satellites

HE Neutrinos: underground ice and water, balloons, radio

telescopes

A New Era of AstroParticle Physics!Beginning to unveil the nature of !

the Most Energetic Accelerators in Nature!

UHE Cosmic Rays: Pierre Auger South, Telescope Array

HE Gamma-rays: FGST, Milagro, MAGIC, HESS, VERITAS

HE Neutrinos: IceCube, Antares, ANITA

Cosmic Ray!Spectrum!

Non-thermal

Phenomena

Extreme Accelerators

Emax > 1020 eV

Features:

knee, ankle, GZK cutoff

accelerators

propagation

interactions

E-2.7

E-3.1

12 orders of magnitude

32 o

rder

s of

magn

itu

de

RH

IC

Tev

atro

n

LH

C

Ankle

(1 particle /km2 yr)

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

Engel’08

knee

ankle

Each Energy !range tells its story!

108 eV < E < 1011 eV

Solar Modulation

1011eV < E < 1017.5-18.5? eV

Galactic Propagation

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

Extragalactic Sources

Each Energy !range tells its story!

108 eV < E < 1011 eV

Solar Modulation Barger et al 08

Galactic Accelerators!

E < 1017.5-18.5? eV


Galactic Sources?


E < 1017.5-18.5? eV


Galactic Sources?

CREAM

Kascade Grande

IceTop

FGST

ACTs


E < 1017.5-18.5? eV


Galactic Sources?

Tycho SN SNR1006

CHANDRA NASA/CXC/SAO

HESS - TeV !’s !!

Hinton, WatsonFest, Leeds

RX J1713 - 20 " Gamma-rays X-rays

CHANDRA

smoking guns of CR acceleration!

see Anders Borgland

R. Dubois


E < 1017.5-18.5? eV


Ankle



SNR shock acceleration

in the Galaxy?

HESS SNe

?

Extragalactic Accelerators!

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

Extragalactic Sources

Extreme Accelerators

Emax > 1020 eV

= 108 TeV!

E-2.7

E-3.1 Ankle



Extragalactic Accelerators?

Extragalactic Accelerators!

Challenging Accelerators!to reach 1020 eV !

LHC magnetic field,"

radius ~ 107 km (Sun – Mercury)!

E = Ze B L!

10% efficiency

1020eV Protons

1020eV Iron

B(G)

L(cm)

E = Ze B L!

10% efficiency

1020eV Protons

1020eV Iron

B(G)

L(cm)

others

GRBs

Galaxy Jets from Black Holes?

Ultra High Energy Cosmic Ray Accelerators?!

Gamma Ray Bursts?

Neutron Stars? Magnetars?

Highest Energies!

E-2.7

E-3.1

RH

IC

Tev

atro

n

LH

C

Ankle



Pointing

Feature

Cosmologically Meaningful Termination !

GZK Cutoff

Greisen, Zatsepin, Kuzmin

1966

p+!cmb" #+ " p + $0

" n + $ +

Proton Horizon

~1020 eV

Chargeless vs Charged!@ Highest Energies!

Photons:

1600s:

G. Galilei

Cosmic Rays

1912: V. Hess

Att

enua

tion

Len

gth!

Lee’95

GZK Feature!

E-2.7

E-3.1 Ankle


“Cosmologically

Meaningful” Feature

High Resolution Fly’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

# Anisotropies in Sky Distribution

#! Particle* Astronomy!!!

*(electrically charged)

Horizon - observed Protons !

AO, Armengaud, Allard, Kravtsov ‘07

Horizons:!

Gpc

1019 eV ~ 1 Gpc!

1020 eV < 100 Mpc!

100 Mpc

THE SLOAN GREAT WALL

Protons with > 1020.5 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!

HIGH QUALITY

LARGE QUANTITY

Auger South!

1660 tanks in a

3,000 km2

Surface Array

4 Fluorescence

Detector Sites

tanks aligned seen from Los Leones!

4 times 6 telescopes overlooking the site!

Cosmic Ray!

Spectrum!

E-2.7

E-3.1 Ankle


“Cosmologically

Meaningful” Feature

Energy spectrum from SD showers with $ " 60°!

calib. uncert. 10%

FD syst. unc. 22%

5165 km2 sr yr ~ 0.8 full Auger year

Energy spectrum from SD showers with $ " 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 = 6"

High Resolution !Fly’s Eye!

AGASA !



AGASA !


HiRes 2008


AGASA !


AUGER 08

HiRes 2008

Spectrum 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

Composition & Spectrum!

HEAT

High Elevation Angle Telescopes

AMIGA

Auger Muon and Infill Ground Array

Auger South Low Energy Extension !

20 km

20 km

Millard County

Utah/USA

24 x 24 Scintillators

(1.2 km spacing) 900 km2

~0.3 Auger South

3 x Fluorescence Stations

AGASA x 10 by stereo

Telescope Array !

Low Energy Hybrid

Extension

Aperture

1.4 103 km2 sr

Engel’08

knee

ankle

High Energy Cosmic Rays!

OBSERVABLES:

Spectrum

Composition

Sky Distribution

Composition-sensitive observables!

Depth of shower maximum development: Xmax

low E! high E! high E!

low A! high A!atmospheric

depth (g/cm2)!

Stochastic process large

fluctuations!

small

fluctuations!

Composition observable: !shower maximum !

Expectations from different hadronic models

+ fluctuations in Xmax smaller for heavier nuclei

Shower maximum over 2 decades in E!

+ fluctuations in Xmax to be exploited

Horizons for Etot=60 EeV!

Allard et al 08

Observed Composition

Allard et al ‘07



Need input from LHCf & TOTEM to

test Hadronic interaction models

?????

Photon limit!

Photon-induced showers look very different

Showers at E = 1019 eV, " = 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

Super heavy dark

matter (SHDM)

models are excluded

as UHECR sources!

Auger results (photon limit)!

Auger results (photon limit)!

Topological defects

(TD) are still possible

UHECR sources

Cosmologically Meaningful Termination!Implies Cosmogenic Neutrinos! !

GZK Cutoff

Greisen, Zatsepin, Kuzmin

1966

p+!cmb" #+ " p + $0

" n + $ +

Proton Horizon

~1020 eV

Auger results!TD models closer to

be constrained by

Auger neutrino limits

Neutrinos at EeV Soon!!

Neutrinos Soon!!

IceCube 22- !Point Source search!

2.2. sigma spot !

Bigas Cazon 06

Cosmogenic Neutrino

are just around the corner?

High Energy Cosmic Rays!

OBSERVABLES:

Spectrum

Composition

Sky Distribution

Main Auger result!

Highest energy cosmic rays have an anisotropic distribution!

First evidence that CR

astronomy is possible!

Correlation with z < 0.018 AGNs in

the 12th Véron-Cetty/Véron catalogue

Opening of a new era:

Study of particle acceleration in

HE astrophysical sources

Multi-messenger study of sources

HEP interactions at 300 TeV cm!

Auger main anisotropy result !

* - VCV AGN catalogue

- 27 highest energy events UHECRs

correlation is most significant above E = 56 EeV whre the CR flux drops…

(supports GZK interpretation)

Auger main anisotropy result !

Significance of the anisotropy result !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 fluctuation!

Auger 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

Significance of the anisotropy result !

2nd step: predefine a region in the sky of excess CR flux &

test if next UHECRs come from this region

Independent data set, prescribed parameters

unambiguous 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)

Astrophysical Implications?!

UHECR sources are extragalactic!!!

They exist within the GZK sphere!!!!

What are the sources? Not clear yet!

Very low statistics to check against any specific model

YES!Can UHECRs come from AGNs?

Do UHECRs have to come from AGNs? NO!!

NOT Galactic Accelerators: Neutron Stars, Magnetars, Microquasars

shocks in the Galaxy

NOT very Distant Accelerators: Clusters of Galaxies(cluster shocks)

Quasars, BL Lacs

E = Ze B L!

10% efficiency

1020eV Protons

1020eV Iron

B(G)

L(cm)

others

GRBs

E = Ze B L!

10% efficiency

1020eV Protons

1020eV Iron

B(G)

L(cm)

others

GRBs

X

X

X X

Centaurus A, Virgo, etc. !

Centaurus A!

3.4 Mpc

AGN Acceleration Models

Astro/Phys Implications !

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

If Proton Primaries - need to understand

>100 TeV interactions - Xmax, %Xmax, Nµ

+ Cosmogenic Neutrinos around the corner

If Heavy Primaries – need to understand

The Astrophysical Accelerators

+ Cosmogenic Neutrinos low flux

Magnetic Deflection

Plausible Bgalactic

E> 56EeV

Engel et al 08

What Next?!

Auger SOUTH 2007

Auger NORTH, JEM-EUSO, ….

Armengaud

10-3/Mpc3 AN+S 7 105L

Source Spectra!

Blasi & DeMarco

The Pierre Auger Observatory!of Ultra-High Energy Cosmic Rays!

Southern site

3 000 km2!

Northern site

20 000 km2!

Argentina!

Australia!Brasil!Bolivia*!Czech Republic!France # # !Germany !Italy!Mexico!Netherlands!Poland!

> 300 PhD scientists from !> 70 Institutions !and 17 countries!

Portugal# !Slovenia !Spain !UK#!USA!Vietnam*!

*Associate Countries!

Auger South Area !

Auger North Area!

Auger North in SE Colorado

Auger SOUTH & NORTH !Auger SOUTH

3,000 km2 = 1,157 mile2

Hexagonal grid -

1.5 km separation

FD sites - 4 (180o)

Auger NORTH

20,000 km2 ~ 8,000 mile2

SQUARE GRID -

1.414 mile separation

(2.26 km)

1 large PMT / tank 40 FD telescopes 7x Area for 2x the price

Auger NORTH !

1609 m!

1 mile!

Auger SOUTH

3,000 km2 = 1,157 mile2

Hexagonal grid - 1.5 km separation

FD sites - 4 (180o)

Auger NORTH

20,000 km2 ~ 8,000 mile2

SQUARE GRID -

1.414 mile separation

1 large PMT / tank 40 FD telescopes

Apertures & Energy Threshold!

Anisotropies

Nadir (2 yrs)

35o tilt (3 yrs)

- 3 x area, but

Eth > 1020 eV

Fluorescence only

~ 20% duty cycle

no muons info

Lin

dsle

ys

A New Era of AstroParticle Physics!Beginning to unveil the nature of !

the Most Energetic Accelerators in Nature!

UHE Cosmic Rays: Pierre Auger North, JEM-EUSO

HE Gamma-rays: FGST, HAWC, AGIS, CTA

HE Neutrinos: IceCube, Km3Net

Particle Astrophysics @ UHEs!The Energy Frontier

TeV PeV EeV ZeV 12 15 18 21

12 15 18 21

12 15 18 21 !

&

CR

Leading & FUTURE Projects

IceCube Auger S

IceRay ANITA II

TA/TALE

Auger South

Auger S HAWC ! desert

ARIANNA

Auger North

Auger N

JEM EUSO

JEM EUSO

JEM EUSO Auger N KM3net

CTA

AGIS

FGST

AstroParticle Physics @ UHEs!The Energy Frontier

TeV PeV EeV ZeV 12 15 18 21

12 15 18 21

12 15 18 21 !

&

CR

Leading & FUTURE Projects

IceCube Auger S

IceRay ANITA II

TA/TALE

Auger South

Auger S HAWC ! desert

ARIANNA

Auger North

Auger N

JEM EUSO

JEM EUSO

JEM EUSO Auger N KM3net

CTA

AGIS GLAST

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