july 10, 2007 detection of askaryan radio pulses produced by cores of air showers. suruj seunarine,...
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![Page 1: July 10, 2007 Detection of Askaryan radio pulses produced by cores of air showers. Suruj Seunarine, Amir Javaid, David Seckel, Philip Wahrlich, John Clem](https://reader035.vdocuments.us/reader035/viewer/2022062800/56649e035503460f94aee25c/html5/thumbnails/1.jpg)
July 10, 2007
Detection of Askaryan radio pulses produced by cores of air showers.
Suruj Seunarine, Amir Javaid, David Seckel, Philip Wahrlich, John Clem
D. Seckel, Univ. of Delaware
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Topics
• Concept: – A source to test radio techniques– CR composition ?
• Askaryan pulses & air shower dimensions
• Air shower properties (AIRES & CORSIKA)– Particle content– Radial and energy distributions
• Calculation of RF signal– Coherent addition of subshowers– Issues: near zone/far zone, ray tracing
• Composition studies
• Detection– IceCube: shallow array, AURA– ANITA
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Theorist’s view of the UHE neutrino sky
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Recall how radio works
5 m
10 cm
JC, SY: “How do you know when you haven’t seen anything?”
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Radio Goals & Staging
• 100 events/yr above 1018 eV
• >1000 km3 sr
• Validation of design for field work
• Prototype projects – more than upper limits
• Detect Air Showers: Signal/Background/Calib
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Askaryan pulses from air shower core
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Critical dimensions
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
High energy ground level particles at SP
• CORSIKA/AIRES– Primary energy: 1,10,100,1000 PeV– Cutoff: 1,10,100,1000 GeV– Composition p & Fe
• Explore– Particle content rad - meson - baryon - mu
– Radial profiles Esh vs r
– Shower development dN/dE, ancestry
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Ground level particles
e-
n,p
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Radial distributions by particle ID
radiatingmesonsbaryonsmuons
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
E vs r (AIRES)
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
E vs r (CORSIKA)
Fraction of available energy approaches 10% by 100 PeV
Scaling allows use of high cutoff
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Synthesis of Askaryan pulses
• Many ground level particles– Superposition
• Individual RF pulses– Event: (id, te, xe, n, E)
– SubShower: (ts, xs, n, (r,l,s))
– Resolve geometry to antenna– Launch EM pulse (scaled AVZ)– Propagation effects (1/r, attenuation)– Adjust phase to common time basis
• Response– CoAdd spectra (t, n, pol, (complex spectrum))– Antenna/DAQ
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Subshowers & Coherence of RF pulses
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Time Domain Waveforms
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
RF: (Ep = 1 EeV, Ecut = 1 TeV )
20 10 0 10 20600
400
200
0
200
400
t nsm
V
Simulat ed p ulse in a R ice ant enna ch 6
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
EeV/TeV again
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
RF Cerenkov Rings
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
RF vs Core Size
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Determining Cosmic Ray Composition
• AIRES showers (from S. Seunarine)
• Esh(r<20 cm) as proxy for radio
• High-lite: 10 PeV, True iron
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Comparison of Fe/p
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Scaling & Rates
• Rate independent of D• Threshold increases with D• True for E-3
– But not for E-2
• Rate for 30m*30m @ 3PeV = 1/hour
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Shallow Array Concepts
• Drill 16 x 30m holes – 1 dom per hole– 4 antennas per dom
• 2 x 50m cables to each of four nearby strings & SJB• 2 doms per cable
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
AURA geometry
255 0 260 0 265 0 270 0
0 .0
0 .5
1 .0
1 .5
2 .0
2 .5
3 .0
3 .5
t ns after impact V
offset
Simulat ed R IC E resp onse w A U R A t iming
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
ANITA (A. Javaid)
• Rate– A 1.5 106 km2 sr– 1400/day E>1019 – ? /day E>1020
• High, Thin, Ice
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Summary
• Test beam for radio sure would be nice
• Air Shower Cores: Eeff ~ 10% Ep (at EeV)
• Synthetic RF looks usable• CR Composition Measurement
– Core energy anti-correlated with deep- – p-Fe separation
• Three scenarios– Small subsurface array w/IceTop– AURA– ANITA
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
END
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Radial distributions by energy
-1.5 -1 -0.5 0 0.5 1 1.5 2xm
-1.5
-1
-0.5
0
0.5
1
1.5
2
ym
x,yfor rad : Log EGeV 10. , 17.7828 , 31.6228 , 56.2341 , 100.
-0.1 0 0.1 0.2xm
-0.1
0
0.1
0.2
ym
x,yfor rad : Log EGeV 100. , 177.828 , 316.228 , 562.341 , 1000.
-1.5 -1 -0.5 0 0.5 1 1.5 2xm
-1.5
-1
-0.5
0
0.5
1
1.5
2
ym
x,yfor rad : Log EGeV 10. , 17.7828 , 31.6228 , 56.2341 , 100.
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Askaryan pulses from air shower cores, Merida, 30th ICRC, July 10 2007 (Seckel)
Sample the Cerenkov Ring