Post on 19-May-2018
Ultra High Energy Cosmic Rays &
Pierre Auger Observatory
Angela V. OlintoKICP
The University of Chicago
Nature sends 1020 eV particles
QuickTime™ and aYUV420 codec decompressor
are needed to see this picture.
Olinto SSI 08
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
Olinto SSI 08
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, …
QuickTime™ and a
TIFF (Uncompressed) decompressor
are needed to see this picture.
Olinto SSI 08
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, …
QuickTime™ and a
TIFF (Uncompressed) decompressor
are needed to see this picture.
Olinto SSI 08
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
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
Olinto SSI 08
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”
Olinto SSI 08
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
Olinto SSI 08
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
Olinto SSI 08
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.QuickTime™ and a
TIFF (Uncompressed) decompressorare needed to see this picture.
Tycho SN SNR1006
CHANDRA NASA/CXC/SAO
Olinto SSI 08
HESS - TeV γ’s !
Hinton, WatsonFest, Leeds
RX J1713 - 20 σX-rays
CHANDRA
smoking guns of CR acceleration
Gamma-rays
Olinto SSI 08
Galactic Accelerat
ors
E < 1017.5-18.5? eV - Galactic Propagation
Ankle(1 particle /km2 yr)
Ecm = PeV (Euhecr /ZeV)1/2 (2A)1/2
SNR shock accelerationin the Galaxy?
HESS SNe
?
Olinto SSI 08
Extreme Accelerators
Emax > 1020 eV
E-2.7
E-3.1Ankle(1 particle /km2 yr)
Ecm = PeV (Euhecr /ZeV)1/2 (2A)1/2
Extragalactic Accelerators?
Extragalactic
Accelerators
Olinto SSI 08
Galaxy Jets from Black Holes?
Ultra High Energy Cosmic Ray Accelerators?
Gamma Ray Bursts?
QuickTime™ and aPhoto decompressor
are needed to see this picture.
Neutron Stars? Magnetars?
Olinto SSI 08
Highest Energies
E-2.7
E-3.1
RH
IC
Teva
tron
LHC
Ankle(1 particle /km2 yr)
Ecm = PeV (Euhecr /ZeV)1/2 (2A)1/2
- Pointing- Feature
Cosmologically Meaningful Termination
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
GZK CutoffGreisen, Zatsepin, Kuzmin 1966
p+γcmb→ Δ+ → p + π0
→ n + π +
Proton Horizon~1020 eV
Olinto SSI 08
Energy loss Features for protons Berezinsky et al. 03
modification factor: Jobs (E,z) = η(E,z) x Jinjec(E)
GZKpairredshift
Olinto SSI 08
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
Charged Particle Astronomy
Window of opportunity
1019 to 1021 eV
Maximize the Statistics in this window
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
Olinto SSI 08
The Surface Detector Array
1662 deployed 1640 filled1591 taking dataof the1600+ tanks, 3,000km2
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
QuickTime™ and aYUV420 codec decompressor
are needed to see this picture.
Olinto SSI 08
Cherenkov water tankAuger SD station
PMT
Plastic tank 12 m3 of clean water
Solar panel
Comms antenna
GPS antenna
battery
Diffusive white “liner”
Olinto SSI 08
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
Olinto SSI 08
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
Olinto SSI 08
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
Olinto SSI 08
ture boxter UV passty curtain
corrector lens(aperture x2)
440 PMT camera 1.5° per pixel
segmented spherical mirror
Olinto SSI 08
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
Olinto SSI 08
Cosmic Ray
Spectrum
E-2.7
E-3.1Ankle(1 particle /km2 yr)
“CosmologicallyMeaningful” Feature
Olinto SSI 08
Energy spectrum from SD showers with θ ≤60°
calib. uncert. 10%FD syst. unc. 22%
5165 km2 sr yr ~ 0.8 full Auger year
Olinto SSI 08
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 08
High ResolutioFly’s EyeAGASA
No GZK cutoff Consistent w/ GZK cutoff
AUGER 08HiRes 2008
Olinto SSI 08
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
Olinto SSI 08
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
Olinto SSI 08
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
Olinto SSI 08
Composition observable:
shower maximum
Composition observable:
shower maximum
+ fluctuations in Xmax smaller for heavier nuclei
Expectations from different hadronic models
Olinto SSI 08
111 69 25 12426
326
Large number of events allows good control and understanding of systematics
Comparison with previous studies
Comparison with previous studies
Olinto SSI 08
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
Olinto SSI 08
Super heavy dark matter (SHDM) models are excluded as UHECR sources!
Auger results (photon limit)Auger results (photon limit)
Olinto SSI 08
Auger results (photon limit)Auger results (photon limit)
Topological defects (TD) are still possible UHECR sources
Olinto SSI 08
Auger resultsAuger results TD models closer to be constrained by Auger neutrino limits
Olinto SSI 08
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…
Olinto SSI 08
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:
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
Study of particle acceleration in HE astrophysical sources
Multi-messenger study of sourcesHEP interactions at 300 TeV cm!
Olinto SSI 08
Equal Exposure PlotArrival Directions for E>3 EeV
+25 deg
0 deg
-30 deg
-60 deg RA = 0 deg
Olinto SSI 08
Veron-Cetty AGNs (red dots)
Supergalactic Plane (blue line)
Swift x-ray galactic black holes (blue circles)
Olinto SSI 08
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
Auger main anisotropy resultAuger main anisotropy result
* - VCV AGN catalogue- 27 highest energy events UHECRs
Olinto SSI 08
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
Δθ ≤ 3.1°Δθ ≤ 3.1° z ≤ 0.018z ≤ 0.018
(D ≤ 75 Mpc)(D ≤ 75 Mpc)E ≥ 56 EeVE ≥ 56 EeV
Auger main anisotropy resultAuger main anisotropy result
Olinto SSI 08
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
correlation is most significant above E = 56 EeV whre the CR flux drops…(supports GZK interpretation)
Auger main anisotropy resultAuger main anisotropy result
Olinto SSI 08
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!
Olinto SSI 08
Significance of the anisotropy resultSignificance 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 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
Olinto SSI 08
Significance of the anisotropy resultSignificance 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 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)
Olinto SSI 08
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
Olinto SSI 08
E = Ze B L
10% efficiency
1020eV Protons1020eV Iron
B(G)
L(cm)
others
GRBsX
XX X
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
Olinto SSI 08
Astrophysical Accelerators
NOT Galactic AcceleratorsNeutron Stars MagnetarsMicroquasarsshocks in the Galaxy
NOT very Distant AcceleratorsClusters of Galaxies(cluster shocks)QuasarsBL Lacs
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
AGN Acceleration Models
QuickTime™ anTIFF (Uncompressed
are needed to see t
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
Olinto SSI 08
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
Olinto SSI 08
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
Olinto SSI 08
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
Olinto SSI 08
Apertures & Energy Threshold
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
Anisotropies
Auger
North
Olinto SSI 08
JEM-EUSODesign Study is ongoing in JAXA
Japanese Experiment Module of ISS in 2013Extreme Universe Space Observatory
Olinto SSI 08
Nadir (2 yrs)35o tilt (3 yrs)- 3 x area, but Eth > 1020 eV
Fluorescence only~ 20% duty cycleno muons info
Olinto SSI 08
Next to next generation:Free Flyers: OWL, Super EUSO, …
Free FlyerFluorescence from ABOVE!
Olinto SSI 08
Pierre Auger Project
South & Northto discover
Ultra-High Energy Cosmic Ray Sources; study
Ultra-High Energy interactions& detect
Ultra-High Energy Neutrinos