aya ishihara for the icecube ehe pwg
DESCRIPTION
1. A quest for EHE neutrinos with the IceCube detector proposal for EHE neutrino search in 2006 - 9 string sample. Aya Ishihara for the IceCube EHE pwg. 2. Introduction. Target Neutrinos of this analysis. Target Target Energy Range Log(E/GeV) > 8 Optimized for GZK neutrino. - PowerPoint PPT PresentationTRANSCRIPT
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A quest for EHEEHE neutrinoswith the IceCube detector
proposal for EHE neutrino search
in 2006 - 9 string sample
Aya Ishiharafor the IceCube EHE pwg
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Introduction
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Target Neutrinos of this analysisTarget Neutrinos of this analysis
seXp K '7.2 ννμπγ +→+→+→ ±±±GZK neutrinoGZK neutrino
The standard scenario of EHE cosmic-ray induced neutrinos The main energy range:
Eν ~ 109-11 GeV
νμ νe
μ
e
πνμEHE-CR
TargetTarget Energy Range Log(E/GeV) > 8
Optimized for GZK neutrino
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Competitors: Competitors: On-going EHE Neutrino Search On-going EHE Neutrino Search (GZK neutrino energy range (GZK neutrino energy range 108~11 GeV))
Air-shower DetectorHiRes, Auger
BG rejection based on near-horizon/upgoing young shower
reconstruction
EHE ν e
ee
CR
μ
μ
μ
Underground IceCherenkov Detector : IceCubeMain BG rejection based on
energy estimation Simple and robust
μ
EHE νμ
ν eμ
Background:Atmospheric muon
MC studies claim the target sensitivity of Auger/HiRes are almost the same as IceCube, although they are not neutrino detector!
No public results from 3 experiments yet. All claims result is coming very soon.
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EHE EHE Neutrino UndergroundNeutrino Underground
Fluxes at the IceCube depth
S. Yoshida et. al. (2004) Phys. Rev. D 69 103004
tentative
EGZK >> EAtmμ
main signalGZK neutrino induced leptonsGZK neutrino induced leptons
background Atmospheric muonAtmospheric muon
Simple energy cut works!
However, Structure of atmospheric muon flux above 106 GeV is very uncertain !
Surface Fluxes
tentative atm μ
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How uncertain ?How uncertain ?muon background in very high energy regime: NOT well-known (highly
dependent on parton distribution assumption), e.g.
charm productionbundle structure
Ord
ers
dif
fere
nce
EHE regime
Atmospheric muonModel fluxes
From charmed meson decay νμ
μ
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Need models which describe our real data in UHE background
regime
Empirical model
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Analysis
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AnalyzedAnalyzed 9-string 9-string realreal sample sample 20062006statisticsstatistics
stable filtering condition for EHE sample with Nch>80
Physics runs since 2nd June, 2006 to 20th, Nov, 2006
124.148 days of livetime after file selection (a list of files not used and used in this analysis can be found at analysis web page)
Event interval
Event FrequencyBefore file cleaning
Ch
ann
el N
>53
Hz
0.134 Hz for Channel N > 80After file cleaning
Eventinterval
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The 9-stringThe 9-string realreal sample sample 20062006
Example Bright EventsExample Bright Events
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The The 9-string9-string realreal sample sample 20062006FADC FADC Waveforms Waveforms (integral ~ NPE)
Saturated ~ 90mV
DOM#31
1 μs
90 mV
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TypicalTypical ATWD ATWD EHEEHE Waveforms Waveforms (integral ~ NPE)
DOM#36
DOM#37DOM#30
DOM#31
DOM#29
DOM#28
DOM#27
DOM#26
DOM#32
DOM#33
DOM#34
DOM#35
105 ns
402 ns
120 mV
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Looking at a Very Typical Combined EHE Waveform
String#29 – DOM#8RunID 89761- Event ID 1477531
Ch0 Ch1 Ch2
CombinedATWD FADC
105 ns0 ns 402 ns 0ns 105 ns
402 ns105 ns 1 μs
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Still have reasonable Energy vs. NPE correlationStill have reasonable Energy vs. NPE correlationup to logNPE ~ 4.5up to logNPE ~ 4.5
then, early saturation effect diffuse themthen, early saturation effect diffuse them
The 9-string simulation:The 9-string simulation:NPE and Energy CorrelationNPE and Energy Correlation
μ
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NPE corresponds to signal NPE corresponds to signal region is quite reduced region is quite reduced because of ‘reduced bin because of ‘reduced bin readout’ in 2006 datareadout’ in 2006 data
‘‘Reduced Bin#’Reduced Bin#’reduced NPE reduced NPE
Signal NPE regionbased on full readout
Signal NPE regionbased on reduced readout simulation
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The 9-string The 9-string realreal NPE distribution NPE distribution
EHE region!!
Channel N > 80 Filtering bias
Very-high energyBackground
regime
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Atmospheric Muon Bundles ModelAtmospheric Muon Bundles Model(see (see wweb pageeb page for further detail) for further detail)
cosmic-ray energy and total muon energy above Ethres in a bundle
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cos1 −
⎟⎟⎠
⎞⎜⎜⎝
⎛ −=
αμ ϑ
αα
T
Bundle
thresCR AE
EAEE
measuredcosmic-ray
flux
bundles of
atmospheric μ
Cosmic-Ray
μμ
muon bundle fluxmuon bundle flux
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Single Single μμ represents bundled represents bundled μμNPE distributions of Toy model
bundled muon events(50 muons in 100 m radius, 2*106 GeV each)
andfrom single muon (108 GeV) events in 100 m radius
μμ
μ
bundlesingle muon
Log10(event-sum NPE)
N channel
Log10(channel wise NPE)
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Flux after ice propagation (E2dF/dE [GeV/sec str cm2])
Flux at sea level (E2dF/dE [GeV/sec str cm2])
Log10(E bundle/GeV)5.4 8.2 Log10(E bundle/GeV)
5.4 8.2
Atmospheric Model Construction0.
0
0.
750.
0
0.
75 z
enit
hze
nit
h
0.0
0.7
50.
0
0
.75
cos
zen
ith
cos
zen
ith
down
horizontal
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In-ice fluxes with new modelIn-ice fluxes with new model1
1
cos1 −
⎟⎟⎠
⎞⎜⎜⎝
⎛ −=
αμ ϑ
αα
T
Bundle
thresCR AEE
AEE
Model flux#
Ethres α
1 300 GeV 1.9
2 1500 GeV 2.0
with GZK cutoff !!
#1#2
ET=14.5 GeVA=1
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NPE distribution comparison set #1 simulation and real Set #Set # EEthth αα
11 300 GeV300 GeV 1.91.9
22 1500 GeV1500 GeV 2.02.0
0.6<Cos fg-theta < 1.0-1.0<Cos fg-theta < 1.0
0.4 < Cos fg-theta < 0.6 -1.0<Cos fg-theta < 0.4
Set # 1Set # 1
Log10(NPE)
GZK μGZK atmospheric μreal data
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NPE distribution comparison set #2 simulation and real Set #Set # EEthth αα
11 300 GeV300 GeV 1.91.9
22 1500 GeV1500 GeV 2.02.0
0.6<Cos fg-theta < 1.0-1.0<Cos fg-theta < 1.0
0.4<Cos fg-theta < 0.6 -1.0<Cos fg-theta < 0.4
Set # 2Set # 2
Log10(NPE)Log10(NPE)
GZK μGZK atmospheric μreal data
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Signal and BG Simulation: NPE vs. CosSignal and BG Simulation: NPE vs. Cos((linefitlinefit))
Atmospheric muon model Atmospheric muon model
Log10(NPE)
Cos
fg-
thet
a
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Event SelectionEvent Selection
Set # 2Set # 2Set # 1Set # 1
GZK GZK μμ GZK GZK Cos
fg-
thet
a
Log10(NPE)
Cut level0 1 2 3 4 5 6
7 8 9 10 11 12
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Event Passing RateEvent Passing Rate
zoom
GZK μGZK GZK μ+GZK atmospheric μ set #1 atmospheric μ set #2
Because of uncertainty from NPE/Energy
relation, can not optimize the cut too aggressively
Cut #8 is selected
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Effective AreaEffective AreaSignal condition
Cut #8Filtering condition
Channel Number > 80
km2 km2
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Expected Sensitivity ...long journey toward GZK to be continued…
with cut #8
‘standard’GZK flux
with cut #10
Z-burst
TD
Strong ev.GZK
90 % C.L.
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Summary
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Ready to access EHE region!Ready to access EHE region!
The 9 strings provided analyzable data sample in 2006 MC shows 9 string IceCube is capable of EHE neutrino search but
early saturation and reduced bin numbers mainly has limited its capability
BG is estimated using empirical atmospheric muon bundle model Simple cut gives an event rate of ~0.02 GZK events in 124 days
and expected 10-3 background atmospheric events in the same interval.
22 string independent sample will steadily confirm any finding in 9 string data including empirical atmospheric muon model
No more bin number reduction!!
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FAQ 1FAQ 1
Q-1) CORSIKA? A-1) Use of CORSIKA for this analysis is not realistic because
of the lack of 1) reliable model (incl. bundle and prompt) in interested energy region at surface, 2) computational resources to obtain good stats at this energy and 3) very sensitive detector simulation for partially deployed partial DAQ operation to reproduce full NPE spectra
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FAQ 2FAQ 2
Q-2) Energy resolution / standard-candle? A-2) http://www.ppl.phys.chiba-u.jp/~aya/SC/gdom-1.html MC gives ~ a factor of two more NPEs. This will be put into
the systematic errors in finalizing the (unblinding) analysis. Let us also remark that GZK spectrum is so hard that the
shift of NPE (indirectly related to energy) threshold in the signal cut would not affect sensitivity in EeV regime too much.
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FAQ 3FAQ 3
Q-4) Contribution from GZK neutrino which make in-detector interaction?
A-4) There exists, but minor in the overall event rate (See S.Yoshida et al, PRD 69 (2003) 103004). We are, however, generating neutrino-induced events by JULIeT and the
event rate from the contained events are reported in the collaboration meeting.
Q-3) Baseline for NPE calculation? A-3) We have observed significant baseline shift/droop. Our
recipe to fix it was determined by looking at the baseline distribution of SC data estimated by the various algorythm.
http://www.ppl.phys.chiba-u.jp/~aya/SC/index.html
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FAQ 4FAQ 4
Q-5) IceTop to establish atmospheric muon bundle model? A-5) It is in our future plan. Insight of the mass composition
of Cosmic Rays will narrow the parameter space in the bundle model. We need more stats to realize this study.
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FAQ 5FAQ 5
Q-6) Is this analysis interfere with high energy cascade search?
A-6) No. Our study is not aimed at cascade ID but just looking for very bright events. This analysis is nothing to do with the cascade-likelihood. A (minor) contribution from EHE cascade events are just added to those from muons and taus to estimate the overall event rate. Moreover, our signal energy range (EeV) is mostly higher than that in the mainstream cascade search where you lower the energy threshold by identifying the cascade-like event topology.
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FAQ 6FAQ 6
Q-7) How the slight difference between bundle and our single muon representation in npe affects to this analysis?
A-7) It affects nothing. Our empirical formula has a flexibility in the relation between bundle energy (that determines NPE) and primary cosmic ray energy (that determines flux)
to make renormalization. The NPE/zenith angle distribution of the real data is well described by the model.
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ExtraExtra
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MC truth and LineFit MC truth and LineFit
with Atm. Mu weight with Atm. Mu weight
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Angular ResolutionAngular Resolution
Atm. Mu weight Atm. Mu weight
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Memorandum for atmospheric muon fit using 9 string data
CR
CRCRIB
CR
CR
T
IB
IBthIB
dE
dJE
E
dE
dJ
AE
E
E
AEEFAll
3,
11
3,
3,3,
1
1
1
cos1
1
1),(cos
μ
αμ
μμ
α
ϑα
αα
ϑ
−=
⎟⎟⎠
⎞⎜⎜⎝
⎛ −−
=−
γκ −= )( CRCR FEJ
)(3, NPEfE IB =μ
)(coscos FGf ϑϑ =
11
min cos1 −
⎟⎟⎠
⎞⎜⎜⎝
⎛ −=
αμ ϑ
αα
T
Bundle
CR AEE
AEE
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Event Properties