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![Page 1: 1. 2 David Schramm Symposium: NEW VIEWS OF THE UNIVERSE Recent Studies of Ultra High Energy Cosmic Rays Alan Watson University of Leeds, UK (regular KICP.](https://reader036.fdocuments.us/reader036/viewer/2022062516/56649d4b5503460f94a291a4/html5/thumbnails/1.jpg)
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David Schramm Symposium:
NEW VIEWS OF THE UNIVERSE
Recent Studies of Ultra High Energy Cosmic Rays
Alan WatsonUniversity of Leeds, UK
(regular KICP Visitor)
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Dave Schramm: 15 November 1997
(re- UHECR)
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Outline:• Present Status of Detectors - Auger
• The Issues: i Changes to Hadronic Interaction Models
- inferences for mass composition
ii Energy Spectrum – is there a GZK-effect?
iii Arrival Directions - Clusters? BL Lac associations?
• Summary
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Exposure and Event Numbers from various Instruments
km2 sr year Approximate rate > 10 EeV (km2 sr year)-1
AΩt N rate
AGASA: closed in January 2004: 1600 827 0.52 Scintillator arrayHiRes I: monocular ~5000 403 0.08 Fluorescence Detector(HiRes II: monocular
HiRes: stereo (PRELIMINARY) ~2500 ~500 0.20
Yakutsk: ~900 171 0.19 Scintillator plus air-Cherenkov light
Auger: data taking since Jan 2004 1750 444 0.25 Fluorescence plus water-Cherenkov
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Water-Cherenkov detectors respond to muons, e±, γ
Fluorescence in UV →
11
Hybrid Approach of Auger Observatory
AND
300 – 400 nm
Nitrogen fluorescence
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1056 surface detector stations deployed with 919 taking data (2 Dec 2005)
Three fluorescence buildings complete each with 6 telescopes
First tri-oculars in August
Status
CLF
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θ~ 48º, ~ 70 EeV
Flash ADC tracesFlash ADC traces
Lateral density distribution
Typical flash ADC trace
Detector signal (VEM) vs time (ns)
PMT 1
PMT 2
PMT 3
-0.5 0 0.5 1.0 1.5 2.0 2.5 3.0 µs
18 detectors triggered
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Lateral density distribution
θ~ 60º, ~ 86 EeV
Flash ADC traces
Flash ADC Trace for detector late in the shower
PMT 1
PMT 2
PMT 3
-0.5 0 0.5 1.0 1.5 2.0 2.5 3.0 µs
35 detectors triggered
Much sharper signalsthan in more vertical events leads toν- signature
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Pixel geometryshower-detector plane
Signal and timingDirection & energy
FD reconstruction
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11~4 x 1019eV
Stereo-Hybrid Event
x
x x
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The Central Laser Facility of the Pierre Auger Observatory
355 nm, frequency tripled, YAG laser, giving < 7 mJ per pulse: GZK energy
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ti
Geometrical Reconstruction
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Angular and Spatial Resolution from Central Laser Facility
Laser position – Hybrid and FD only (m)Angle in laser beam /FD detector plane
Mono/hybrid rms 1.0°/0.18° Mono/hybrid rms 566 m/57 m
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A Big Event - One that got away!
Shower/detector plane
Fluorescence Mirror
Energy Estimate
>140 EeV
19 April 2004
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(ii) Muon Content of Showers:-
N (>1 GeV) = AB(E/A)p (depends on mass/nucleon and model)
N(>1 GeV) = 2.8A(E/A)0.86 ~ A0.14
So, more muons in Fe showers
(i) Variation of Depth of Maximum with Energy
Methods of Inferring the Primary Mass
HADRONIC M
ODELS REQUIR
ED
FOR INTERPRETATIO
N –
New m
odel, Q
GSJET II,
dis
cuss
ed
at IC
RC
******
******
******
******
Xmax
Log E
Limiting bound = 2.3 X0 g cm-2 per
decade (Linsley 1977)
p
Fe
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Regions of most interest for shower modelling
Pseudo-rapidity
Multiplicity
Energy distribution
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New hadronic model: QGSJETII Heck and Ostapchenko ICR 2005
Multiplicity vs. Energy
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19Heck and Ostapchenko: ICRC 2005
Xmax vs. Energy for different models compared with data
*
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Hooper, Sarkar and Taylor 2005
Assumption: Fe with E-2 with sharp cut-off at 1022 eV
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Spectrum measurements: Issues of concern
1: SURFACE DETECTOR ARRAYS (e.g. AGASA, Yakutsk)
APERTURE:
- relatively easy to determine
ESTIMATION OF PRIMARY ENERGY:
- mass assumption required
- hadronic interaction model must be assumedfor which systematic uncertainty in UNKNOWABLE
- QGSJETII model will lead to revisions
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2. FLUORESCENCE DETECTOR (e.g. HiRes):
ENERGY ESTIMATES depend only weakly on assumptions about models and mass
BUT determination of energy requires- atmospheric corrections for each event- Cherenkov light subtraction (< 25% used)
APERTURE is difficult to measure- does not saturate- depends on atmosphere- mass of primary- models- spectral shape
so, aperture can be systematically uncertain
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3. Hybrid Detectors (e.g. Auger)
ENERGY CALIBRATION of size parameter measured by surface detectors is made with fluorescence detectors on carefully selected sample of events:
- long tracks in atmosphere: > 350 g cm-2
- Cherenkov light contamination: < 10% (Auger criteria)
HIGH STATISTICS from surface array
APERTURE: well-defined
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24Pierog et al. ICRC 2005
Ratio of total energy to electromagnetic energy for fluorescence detector
Etot/Ecal
log 10 Etot (eV)
1.10
~7%
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Auger Aperture
AGASA aperture
Rel
ativ
e A
pert
ure
1.0
0.5
Energy (eV)1018 1019
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HiRes Monocular Spectra: ICRC
The HiRes grouphave yet to releasea stereo spectrum.
It will have hour-by-houratmospheric correctionsusing monitoring data
Should also help to resolvethe aperture uncertainties- at least at smalldistances
Choice of data usedin the fit is entirelysubjective and nopropagation of Eerrors into y-direction
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Auger Energy Determination: Step 1
The detector signal at 1000 m from the shower core
– called the ground parameter or S(1000)
- is determined for each surface detector event using the lateral density function.
S(1000) is proportional to the
primary energy.
The energy scale is determined from the data and does not depend on a knowledge of interaction models or of the primary composition – except at level of few %.
Zenith angle ~ 48º
Energy ~ 70EeV
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Auger Energy Determination: step 2
log S(1000) from SD
log (
E/E
eV
) fr
om
FD
10EeV
1 EeV
Hybrid Events with STRICT event selection:
aerosol content measured
track length > 350 g cm-2
Cherenkov contamination <10%
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Spectrum measured with Auger Observatory
The function is
F=(30.9±1.7)(E/EeV)-1.84+/- 0.03
with χ 2 = 2.4 per degree of freedom
Issues of aperture, massand hadronic interactionsunder control – systematic uncertainties being assessed
S(1000)Fluorescence YieldAbsolute FD calibrationS(1000) to energy – and limited statistics
systematicuncertainty
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))ln(
(100
FEd
dI
F
Percentage Deviation from the Power-Law Fit
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Summary Spectrum above 2 EeV
aaw/Sept 2005
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Deviations of data from E-3 line through first point of Auger data
aaw/Oct 2005
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HiRes stereo events > 10 EeV plus AGASA events above 40 EeV
HiRes Collaboration: ICRC 2005: Westerhoff et al.
Candidate Clusterα = 169.0 δ = 56.2
Analysis uses likelihood ratio method:
p = 43% for 271 HiRes and 47 AGASA events
NB: Previously, Finley and Westerhoff had shown previouslythat AGASA clustering was statistically unconvincing
- Clustering is very far from being established
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HiRes does see
correlations with BL Lacs:Veron 11th Catalogue:
178 objects with magnitude < 18
Claim: excess number of BL Lacs seen near HiRes events > 1010 GeV, consistent with the HiRes angular
resolution ~ 0.6º
GOOD ANGULAR RESOLUTION
see 11 pairs < 0.8º and expect ~ 3,
⇒ probability ~ 5×10-4
But these BL Lacs are hundreds of Mpc distant!
Few % of primaries must be neutral @ 1010 GeV!!
Gorbunov et al (2004)
Westerhoff et al ( 2005)
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2 x 10-4
5 x 10-4
10-3
2 x 10-4
10-5
2 x 10-4
Finley and Westerhoff ICRC 2005
Group is awaiting independent data set recorded post January 2004up to closure in March 2006 before making any claims. They have concerns about ‘over tuning’
Summary of BL Lac Searches
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Auger sees no concentration of events along the Galactic or Super-Galactic planes
(Antoine Letessier-Selvon, ICRC 2005)
Auger Observations show NO concentration of events along
Galactic or Super-Galactic Plane
A: 1 – 5 EeV: Galactic Plane
B: > 5 EeV: SGP
C: > 10 EeV: SGP
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If highest energy particles were protons, and there is no anisotropy, exotic origin ideas have to be invoked
• Decay of super-heavy relics from early Universe (or top down mechanisms) Wimpzillas/Cryptons/Vortons
• New properties of old particles or new particles
• Breakdown of Lorentz Invariance
Predictions: dominance of neutrinos and photons
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38Picture by Dieter Heck
On-set of LPM effect
γ + B → e++ e-
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39(Risse for Auger Collaboration, ICRC 2005)
… the highest energy particles seem NOT to be dominantly photons
Constrains (but does not yet rule out) ‘top-down’ models of UHECR origin
Photon limit from Auger observations
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Ideas to explain the Enigma• Decay of super heavy relics from early Universe (or top down mechanisms)
Wimpzillas/Cryptons/Vortons
Few photons: <26% at 1019 eV (Auger claim)
Model predictions have changed
Is there need for exotic explanations?
or is it ‘simple’?• Are the UHE cosmic rays iron nuclei at source?
• Are magnetic field strengths really well known?
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Summary: I
• Arrival Directions:
No convincing evidence for anisotropyPossibility of BL Lac associations could
be clarified in ~ 2 years
• New Hadronic Interaction Model:
suggests that there could be a heavier mass > 10 EeV than has been supposed by many in the past
Heavier mass would ease acceleration, isotropy and spectrum issues
BUT – Nature may have surprises to show at the LHC
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Energy Spectrum: Auger: ~ 5 to 7 X AGASA by 2007Spectrum that is largely mass and model independent
AGASA/HiRes/Auger differences could – possibly – be understood through combination of improved understanding of HiRes aperture (composition/spectrum/ hadronic model and stereo data)AND different models and mass assumptions by AGASA
ALL GROUPS HAVE REPORTED EVENTS ABOVE 100 EeV
QUESTION: WHAT IS THE DETAILED SHAPE OF THE SPECTRUM?
Summary: II
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Thanks to all of my Auger colleagues
Spokesperson:Alan Watson
Czech Republic ArgentinaFrance Australia Germany BrasilItaly Bolivia*
Netherlands Mexico Poland USASlovenia Vietnam* Spain United Kingdom
*Associate Countries
~250 PhD scientists from 63 Institutions and 15 countries
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Electromagnetic Acceleration
• Synchrotron Acceleration Emax = ZeBRc
• Single Shot Acceleration Emax = ZeBRc
• Diffusive Shock Acceleration Emax = kZeBRc, with k<1
Shocks in AGNs, near Black Holes……
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Hillas 1984 ARA&A B vs R
Magnetars?
GRBs?
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Some properties of 20 highest energy events :
Curvature
Thickness of shower discFall-off of signal size withdistance from axis
Showers of 30 EeV are just likeshowers at 1 EeV – but bigger
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Resolution of Core Position
Hybrid – SD only core position
Hybrid DataLaser Data
Core position resolution:Hybrid: < 60 m Surface array: < 200 m
Laser position – Hybrid and FD only (m)
-500
+500
501
rms spread ~ 570 m for monocular fit
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Angular Resolution
Surface array Angular resolution (68% CL)<2.2º for 3 station events (E< 3EeV, θ < 60º )< 1.7º for 4 station events (3<E<10 EeV)< 1.4º for 5 or more station events (E>10 EeV)
Hybrid Angular resolution (68% CL) 0.6 degrees (mean)
Hybrid-SD only space angle difference
Hybrid Data
Angle in laser beam /FD detector plane
Laser Beam
Entries 269
σ(ψ) ~ 1.24º
Resolution using a centrally positioned laser
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Ratio of Aperturescomputed with SIBYLLand QGSJET
Sensitivity of HiRes II aperture to shower model
Zech et al. HiRes Collaboration: ICRC 2005
More statistics needed andup-dated model needs to be used.
Mass assumption has onlybeen explored at ± 5% of anassumed proton fraction
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Arrival Direction Studies
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• Fit to power law.
• Single index gives poor χ2
• Evidence for changing index
1019 1020
HiRes Stereo Flux
Springer et al. ICRC 2005F
lux x
1029
log E
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Association with BL Lacs?
Initial claims by Tinyakov et al. – but disputed by Evans et al and others
217 HiRes Stereo events above 10 EeV
σ = 0.4 deg, so that 68% of events would lie within θ = 1.52 σ
This is an impressive angular accuracy
Tinyakov et al. conclusion for m<18 confirmed – but same data set of events and same 157 BL Lacs
BUT for E> 40 EeV, HiRes shows a deficit in the correlation
Presumably primaries are neutral because of anticipatedmagnetic field deflections – worth looking at lower energies.
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105573
12 13 14 km
10 9 8 km
Hybrid events are equivalent to stereo- events and superior to monocular events
Observations with real
showers confirm the
results from Central
Laser Facility
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58Heck and Ostapchenko: ICRC 2005
SIBYLL
Muon Number Ratio for different models and masses
10% reduction in predicted muon numberleads to ~ x 2 increase in the average mass –depending on model details
10%
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Original Claim (2003):
“Consistent with proton dominant component” –
must be revised
19 19.5 20 20.5
Log(Energy [eV])
−2
−1
0
1
Log(
Muo
n de
nsity
@10
00m
[m–2
])Muon measurements with the AGASA array
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60~4 x 1019eV
Stereo-Hybrid Event
x
x x
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Surface Array 1600 detector stations 1.5 km spacing 3000 km2
Fluorescence Detectors 4 Telescope enclosures 6 Telescopes per
enclosure 24 Telescopes total
CLF
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HiRes I and HiRes II
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ti
Geometrical Reconstruction