Neutrino search in Auger Ricardo A. Vázquez University of Santiago de Compostela, Spain for the...
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![Page 1: Neutrino search in Auger Ricardo A. Vázquez University of Santiago de Compostela, Spain for the Pierre Auger collaboration Beijing, April 2006.](https://reader036.fdocuments.in/reader036/viewer/2022062516/56649d805503460f94a652eb/html5/thumbnails/1.jpg)
Neutrino search in AugerRicardo A. Vázquez
University of Santiago de Compostela, Spain
for the Pierre Auger collaboration
Beijing, April 2006
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1.The Pierre Auger Observatory
2. Neutrino Search:
3. Fluorescence Detector (FD) Search
4. Surface Detector Search
5. Conclusions
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The Pierre Auger Observatory
Aims at measuring The Highest Energy Cosmic Rays
Energy Spectrum - Direction – Composition - AnisotropyHybrid detection: Fluorescence and Surface detectors
Two Large Air Shower DetectorsMendoza Province, Argentina (under construction)Colorado, USA
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The Auger CollaborationParticipating CountriesArgentina MexicoAustralia NetherlandsBolivia* PolandBrazil Slovenia Czech Republic SpainFrance United Kingdom Germany USAItaly Vietnam* *Associate
63 Institutions, 369 Collaborators
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Surface Array100% duty cycleUniform sky coverageSimple robust detectorsMass determination using rise time,
& muon/em
Fluorescence DetectorCalorimetric energy measurementDirect view of shower development:Xmax measurement, mass
determinationGood angular resolution (< 1o)
Hybrid concept
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Advantages• Independent measurement techniques allow cross
calibration and control of systematics
• More reliable energy and geometry reconstruction
• Primary mass
Hybrid concept:
Surface Detector Array and Fluorescence Detectors
Two observatories: allow full sky coverage
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Auger Southern
Site
Mendoza province, Argentina
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The Observatory Plan
Surface Array 1600 detector stations 1.5 km spacing 3000 km2
Fluorescence Detectors 4 Telescope enclosures 6 Telescopes per
enclosure 24 Telescopes total
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The Auger Surface Detector
Three 8” PM Tubes
Plastic tank
White light diffusing liner
12 m2 of de-ionized water
Solar panel and electronic box
Commantenna
GPSantenna
Battery box
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Fluorescence Detector Building
at Los Leones
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The Fluorescence Detector
3.4 meter diameter segmented mirror
Aperture stop and optical filter
440 pixel camera
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Atmospherecalibrated (movable) light sourcescloud monitors
LIDARlasers
balloon sondes
2. Intl Workshop Liebenzell Castle
Dec 11-14
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On-line monitoring(Big Brother) • Detector elements are monitorized every 10 mins.• Alarms inform about anomalies.
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Auger Center Building
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Detector Assembly Building
Cerenkov detector tanks being prepared for deployment
The Auger Campus
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The communications system
Rigging the antennas
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Array status by the End 2004337 tanks deployed
~100% duty cycle
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905 surface detector stations deployed
Three fluorescence buildings complete each with 6 telescopes
End of 2005
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Status of the array @ March 2006 ~ 1000 stations
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The First Data SetCollection period – 1 January
2004 to 5 June 2005
Zenith angles - 0 - 60º
Total acceptance – 1750km2 sr yr
(~ AGASA)
Surface array events (after quality cuts)
Current rate - 18,000 / month
Total -~180,000
Hybrid events (after quality cuts)
Current rate – 1800 / month
Total ~ 18000
Cumulative number of eventsJa
nu
ary
04
July
04
Jan
ua
ry 0
5
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Official First FD Event
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Surface Detector First 4 – fold event – 12 August
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Flash ADC traces
Lateral density distribution
Hybrid Event Θ~ 30º, ~ 8 EeV
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Fitted Electromagnetic Shower
from Fly's Eye 1985
Tim
e μ
sec
Angle Χ in the shower-detector plane
Hybrid EventΘ~ 30º, ~ 8 EeV
Tanks
Pixels
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Example Event 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
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Lateral density distribution
Surface Detector Event Θ~ 60º, ~ 86 EeV
Flash ADC traces
Flash ADC Trace for detector late in the shower
PMT 1
PMT 2
PMT 3
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Hybrid event
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Performance: Resolution of Core Position
Hybrid – SD only core position
Hybrid DataLaser Data
Core position resolution
– Hybrid: < 60 m Surface array: ~150 m
Laser position – Hybrid and FD only (m)
-500
+500
En
trie
s 5
01
M
ea
n
5.8
± 6
.5 m
RM
S
14
7 m
Entries 501 Mean 68 ± 8 m RMS 173 m
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Performance: 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
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Energy Determination and the Spectrum
The detector signal size at 1000 meters 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 based on fluorescence measurements without reliance on a specific interaction model or assumptions about the composition.
Zenith angle ~ 48º
Energy ~ 70EeV
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Energy Determination and the Spectrum
The energy converter:
Compare ground parameter S(1000) with the fluorescence detector energy.
Transfer the energy converter to the surface array only events.
Log S(1000)
Log (
E/E
eV
) 10EeV
1 EeV
Hybrid EventsStrict event selection: track length >350g/cm2 Cherenkov contamination <10%
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Auger Energy Spectrum
E/E~30%
E/E~50%
ICRC 2005 spectrum
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Neutrino search in Auger• FD search
– Auger can detect neutrinos directly with the
fluorescence detector
• SD search– Deep inclined (neutrino) showers should have
a different time structure (risetime/falltime), curvature, etc. and electromagnetic component Different strategies
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M. Roth et al., Karlsruhe
FD search
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M. Roth, Karlsruhe
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a real vertical event (20 deg)
Noise !
doublet
SD search
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a real horizontal event (80 deg)
“single” peaks : fast rise + exp. light decay ( ~ 70 ns) accidental background signals are similar
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Simulated + (5.1) 0(16.1) 1800 m above ground
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EM signal in shower plane
Proton
1 EeV
θ = 80 deg
x shower plane [m]
y s
how
er
pla
ne
[m]
[VEM]
ρ, ε → Sμ,EM
3167 g/cm2
3306 g/cm2
3570 g/cm2
3968 g/cm2
4100 g/cm2
4238 g/cm2
4371 g/cm2
4503 g/cm2
4636 g/cm2
4768 g/cm2
4901 g/cm2
3438 g/cm2
3703 g/cm2
3035 g/cm2
Xinjection
J. Alvarez-Muniz
Downgoing showers
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Controlled calculation: strategyWe need ΔX where neutrino triggers are expected → Effective volume
Calculate size of active region (where SEM>Sthreshold)
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2D EM signal maps at ground
EM signal [VEM]
x [km]
y [km]
Proton, E = 1017 eV, hint = 0 m
θ = 90.1 deg θ = 90.5 deg θ = 91 deg θ = 110 deg θ = 92 deg θ = 93 deg θ = 95 deg θ = 100 deg θ = 105 deg
AIRES + SIBYLL 2.1
Fixed proton interaction height hint = 0 m
J. Alvarez-Muniz
Upcoming showers
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2D EM signal maps at ground
EM signal [VEM]
x [km]
y [km]Proton, E = 1017 eV, θ = 91 deg.
hint = 0 m
AIRES + SIBYLL 2.1
hint = 50 mhint = 100 mhint = 300 mhint = 500 mhint = 1000 mhint = 3000 m
Fixed zenith angle θ = 91 deg.
J. Alvarez-Muniz
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Event 850018
Event 1432390
= 71.5±0.02 = -57.2±0.02E ~ 50 EeV R= 22.9 km /dof =2.4NTanks =48
= 77.1± 0.01 = -36.1 ± 0.01E ~ 30 EeV R= 33.11 km/dof =1.81NTanks = 59
Some events
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Event 767138
= 87.6 = -134.9E ~ 30 EeV/dof =1.7NTanks = 37
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Post-San Valentin day eventEvent 1999991
= 83 = -102E ~ 40 EeV
/dof =2.3NTanks = 61
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10% 50%• Risetime is defined as the time from 10% - 50% of the integrated pulse.• Falltime time from 50% - 90%
Risetime/Falltime S [VEM]
90%
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Falltime vs Risetime (2 cuts)S ≥ 15 VEM & r ≥ 500 m
θ ≥ 70 deg.
θ ≤ 45 deg.
Neutrino candidates should have θ ≥ 70 deg and should show up here.
No events up to now!
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L Cazon, RAV, A. Watson, E. Zas (Ap Phys 2004)
Curvature analysis
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Arrival Time of first muon (& average)
-like delay large
p-like delay:small (flat)
L. Cazon, RAV, E. Zas
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footprint analysis
Variables defined from the footprint (in any configuration, even aligned)
• length L and width W (major and minor axis of the ellipsoid of inertia)• “speed” for each pair of stations (distance/difference of time)
major axis
titjdij
P. Billoir & O. Blanch
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candidate selection 2. Discriminating variables
cuts: L/W > 5 0.29 < av. Speed < 0.31 r.m.s. < 0.08
Search for long shaped configurations, compatible with a front moving horizontally at speed c, well contained inside the array(background: vertical or inclined showers, d/Dt > c )
from years 2004-2005: no real event survived…
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Auger sensitivity
Points: 1 event / year / decade of energy
“pessimistic
” energy loss
un
cert
ain
ty
ran
ge
GRB
TD
AGN GZK
prelim
inary
P. Billoir & O. Blanch
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3C2 & 4C42C1 & 3C2 & 4C4
2C1 & 4C23C1 & 4C2
not saturated yet at 1019 eV
compacity ofthe trigger matters !
L. Nellen, V. Van Elewyck & RAV
Log(E/eV)
Understanding the background: HAS
Optimal trigger?
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Conclusions
-The Pierre Auger Observatory is performing well and steadily taking data
-Due to the Hybrid characteristics several neutrino searches are possible
-Need to understand the background, model dependence on the aperture, systematics,….
-We will keep looking for neutrinos !