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< \title{Search for ultra-high-energy cosmic neutrinos with the IceCube neutrino observatory}
---
> \title{Search for Ultra-high energy cosmic neutrinos with the IceCube neutrino observatory}
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< A search for extremely-high-energy (EHE) neutrinos with energies greater than $10^6$~GeV
---
> A search for extremely-high energy (EHE) neutrinos with energies greater than $10^6$~GeV
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< between May 2010 and May 2012. Two neutrino-induced cascade events are
---
> between May 2010 and May 2012. Two neutrino induced cascade events are
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< An upper limit on the neutrino flux in the energy range above $10^6$~GeV is obtained from the observations.
---
> An upperlimit on the neutrino flux in the energy above $10^6$~GeV is obtained from the observations.
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< ultra-high-energy cosmic-ray sources such as AGNs associated with radio-loud jets.
---
> ultra-high energy cosmic-ray sources such as AGNs associated with radio-loud jets.
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< The origin of the ultra-high-energy cosmic-rays (UHECRs) has been a long-standing
---
> The origin of the ultra-high energy cosmic-rays (UHECRs) has been a long-standing
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< propagation of ultra-high-energy cosmic-rays (UHECRs) with energies reaching up
---
> propagation of ultra-high energy cosmic-rays (UHECRs) with energies reaching up
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< A measurement of the cosmogenic neutrinos probes the yet-unknown UHECR origin
---
> A measurement of the cosmogenic neutrinos probes yet-unknown UHECR origin
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< The main energy-emission range of the GZK cosmogenic neutrinos
< is predicted to be around EeV ($10^{18}$~eV)~\cite{yoshida93,ESS}.
< The cosmogenic production has been considered as a main source to emit extremely-high-energy (EHE)
---
> The main energy emission range of the GZK cosmogenic neutrinos
> are predicted to be around EeV ($10^{18}$~eV)~\cite{yoshida93,ESS}.
> The cosmogenic production has been considered as a main source to emit extremely-high energy (EHE)
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< as well as the omni-directional neutrino-detection capability
< have extended the sensitivity into energy regimes even beyond EeV
---
> as well as the omni-directional neutrino detection capability
> have extended the sensitivity into energy regime even beyond EeV
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< satellite when the NPE of the event is larger than 1000. A total of 4.5$\times 10^7$ and 6.3$\times 10^7$
---
> satellite when NPE of the event is larger than 1000. A total of 4.5$\times 10^7$ and 6.3$\times 10^7$
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< For a blind analysis we used approximately 10\% of the total experimental sample
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> For a blind analysis we used approximately 10\% of total experimental sample
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< The dominant class by event number is that containing muon bundles, made up of a large
< number of muons produced by high energy cosmic-ray interactions in the atmosphere.
< The other class is that containing atmospheric neutrinos. The muon bundle was simulated with the CORSIKA
---
> Dominated in the event number are muon bundles made up of a large
> number of muons produced by high energy cosmic-ray interactions in the atmosphere, and
> the other are atmospheric neutrinos. The muon bundle was simulated with the CORSIKA
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< with the pure-iron primary-cosmic-ray composition.
---
> with the pure-iron primary cosmic-ray composition.
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< In this analysis-level sample, a total of $5.0\times 10^5$ and $6.3\times 10^5$
---
> In this analysis level sample, a total of $5.0\times 10^5$ and $6.3\times 10^5$
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< event rates at the final selection level are given as asymmetric errors.
---
> event rates at the final selection level are given as asymmetric error.
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< \caption{Event number distributions in the plane of NPE and energies of neutrino-induced muons (left)
---
> \caption{Event number distributions in the plane of NPE and energies of neutrino-induced muon (left)
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< The particle-energy distribution is assumed to follow $E^{-1}$ in these plots for illustrative purposes.
< The muon and neutrino energies are given when a particle intersects a radius of 880~m from the IceCube center.
---
> The particle energy distribution is assumed to follow $E^{-1}$ in these plots for illustrative purposes.
> The muon and neutrino energies are given when particle intersects a radius of 880~m from the IceCube center.
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< \includegraphics[width=1.50in]{figure/NPEVsEnergyMuE1.pdf}
< \includegraphics[width=1.50in]{figure/NPEVsEnergyCascadeE1.pdf}
---
> \includegraphics[width=1.50in]{figure/NPEVsEnergyMuE1.eps}
> \includegraphics[width=1.50in]{figure/NPEVsEnergyCascadeE1.eps}
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< \includegraphics[width=1.85in]{figure/AnalysisLevelIC86NPE.pdf}
< \includegraphics[width=1.85in]{figure/AnalysisLevelIC86CosTheta.pdf}
< \caption{Event-number distributions are shown as functions of NPE
---
> \includegraphics[width=1.85in]{figure/AnalysisLevelIC86NPE.eps}
> \includegraphics[width=1.85in]{figure/AnalysisLevelIC86CosTheta.eps}
> \caption{Event number distributions are shown as functions of NPE
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< for the livetime of the test samples of the experimental data (20.8 days).
---
> for livetime of the test samples of the experimental data (20.8 days).
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< Each component of the background (single and coincident atmospheric muons, conventional
< and prompt atmospheric neutrinos) is also shown separately.}
---
> Each component of the background, single and coincident atmospheric muon, conventional
> and prompt atmospheric neutrinos are also shown separately.}
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< As the energy spectrum of background atmospheric muons and neutrinos falls steeply with energy,
< cosmogenic neutrino fluxes dominate over background in the high-energy region.
---
> As the energy spectrum of background atmospheric muon and neutrinos falls steeply with energy,
> cosmogenic neutrino fluxes dominate over background in the high energy region.
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< Figure~\ref{fig:energyNPE} presents the simulated analysis-level distribution of NPE recorded by IC86 as a
---
> Figure~\ref{fig:energyNPE} presents the simulated analysis level distribution of NPE recorded by IC86 as
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< Figure~\ref{fig:analysislevel} displays the NPE and reconstructed zenith-angle distributions
---
> Figure~\ref{fig:analysislevel} displays the NPE and reconstructed zenith angle distributions
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< IC79 and IC86, the resultant anglar resolution is approximately $\sim 1$ degree
---
> IC79, and IC86, the resultant anglar resolution is approximately $\sim 1$ degree
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< which is sufficient to remove atmospheric muon-bundle background events in the current analysis.
---
> which is sufficient to remove atmospheric muon bundle background events in the current analysis.
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< \includegraphics[width=1.7in]{figure/AnalysisLevel2D_IC86Data.pdf}
< \includegraphics[width=1.7in]{figure/AnalysisLevel2D_IC86AtmMuSingleCoinc.pdf}
< \includegraphics[width=1.7in]{figure/AnalysisLevel2D_IC86AtmNu.pdf}
< \includegraphics[width=1.7in]{figure/AnalysisLevel2D_IC86AllSignal.pdf}
---
> \includegraphics[width=1.7in]{figure/AnalysisLevel2D_IC86Data.eps}
> \includegraphics[width=1.7in]{figure/AnalysisLevel2D_IC86AtmMuSingleCoinc.eps}
> \includegraphics[width=1.7in]{figure/AnalysisLevel2D_IC86AtmNu.eps}
> \includegraphics[width=1.7in]{figure/AnalysisLevel2D_IC86AllSignal.eps}
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< \caption{Event-number distributions on the plane of NPE and reconstructed zenith angle
---
> \caption{Event number distributions on the plane of NPE and reconstructed zenith angle
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< distributions include atmospheric muons from the CORSIKA package with SIBYLL high-energy
---
> distributions include atmospheric muons from the CORSIKA package with SIBYLL high energy
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< \includegraphics[height=2.1in, width=2.1in]{figure/EffectiveAreaEachFlavor_IC79.pdf}
< \includegraphics[height=2.1in, width=2.1in]{figure/EffectiveAreaEachFlavor_IC86.pdf}
< \includegraphics[height=2.1in, width=2.1in]{figure/EffectiveArea3FlavorSum_3years.pdf}
---
> \includegraphics[height=2.1in, width=2.1in]{figure/EffectiveAreaEachFlavor_IC79.canvas.eps}
> \includegraphics[height=2.1in, width=2.1in]{figure/EffectiveAreaEachFlavor_IC86.canvas.eps}
> \includegraphics[height=2.1in, width=2.1in]{figure/EffectiveArea3FlavorSum_3years.canvas.eps}
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< In Fig.~\ref{fig:final}, the event-number distributions of the Monte Carlo simulations and
---
> In Fig.~\ref{fig:final}, the event number distributions of the Monte Carlo simulations and
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< The signal distributions add all three flavors of neutrinos.
---
> The signal distributions adds all three flavors of neutrinos.
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< can be separated with a zenith-angle-independent NPE threshold value.
---
> can be separated with a zenith angle independent NPE threshold value.
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< The effective neutrino-detection areas of the analysis
---
> The effective neutrino detection areas of the analysis
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< The right panel in Fig.~\ref{fig:effarea} shows the three-neutrino-flavor sum of
---
> The right panel in Fig.~\ref{fig:effarea} shows the three neutrino flavor sum of
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< $1.75\times10^{-3}$, equivalent to a 2.9$\sigma$ deviation,
---
> $1.75\times10^{-3}$ equivalent to a 2.9$\sigma$ deviation,
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< \includegraphics[width=1.55in, height=1.55in]{figure/Aug_EventView.pdf}
< \includegraphics[width=1.55in, height=1.55in]{figure/EventViewJan2012_3.pdf}
---
> \includegraphics[width=1.55in, height=1.55in]{figure/Aug_EventView.eps}
> \includegraphics[width=1.55in, height=1.55in]{figure/EventViewJan2012_3.eps}
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< \includegraphics[height=3.0in]{figure/FinalLevelIC86IC79NPE.pdf}
---
> \includegraphics[height=3.0in]{figure/FinalLevelIC86IC79NPE.eps}
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< We examine models predicting ultra-high-energy neutrino productions
---
> We examine models predicting ultra-high energy neutrino productions
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< that a neutrino generation mechanism other than the GZK interactions
< is responsible for the PeV neutrino sky including the observed two neutrino events.
---
> that neutrino generation mechanism other than the GZK interactions
> is responsible for PeV neutrino sky including the observed two neutrino events.
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< the present constraints from the limit on the ultra-high-energy neutrino flux are compatible
< with those from the photon-flux measurement by Fermi in the 10 GeV region~\cite{fermilimit}.
---
> the present constraints from the limit on the ultra-high energy neutrino flux are compatible
> with those from the photon flux measurement by Fermi in 10 GeV region~\cite{fermilimit}.
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< \includegraphics[width=0.45\textwidth]{./figure/EvolutionContourIC40-79-86_1yr.pdf}
---
> \includegraphics[width=0.45\textwidth]{./figure/EvolutionContourIC40-79-86_1yr.eps}
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< \includegraphics[width=0.45\textwidth]{./figure/UpdatedUpperlimt_withoutGR_withSys_v2.pdf}
---
> \includegraphics[width=0.45\textwidth]{./figure/UpdatedUpperlimt_withoutGR_withSys_v2.eps}
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< widely assumed in the models mentioned here while a predominance of heavier nuclei
---
> widely assumed in the models mentioned here while predominance of heavier nuclei
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< We analyzed the 2010--12 data sample collected by the 79 and 86-string IceCube
< detector to search for extremely-high-energy neutrinos with energies exceeding $10^6$~GeV\null.
---
> We analyzed the 2010-12 data sample collected by the 79 and 86-string IceCube
> detector to search for extremely-high energy neutrinos with energies exceeding $10^6$~GeV\null.
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< The energy profiles of the two events indicate that these events are cascades of which the energy deposited was $\sim$1~PeV.
< An upper limit on the neutrino rate in the energy region above 100 PeV
< puts constraints on the distribution of UHECR emitters in redshift space.
---
> The energy profiles of the two events indicates that these events are cascades of which the energy deposited $\sim$1~PeV.
> An upperlimit on the neutrino rate in the energy region above 100 PeV
> puts constraints on distribution of UHECR emitters in redshift space.
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< the parameter region where some leading UHECR-source candidates are expected to be distributed.
< The bound---significantly upgraded from our previous publication~\cite{icecubeEHE2011}---was
< brought about by both the enlarged instrumentation volume and
< the refined Monte Carlo simulations with improved agreements with the experimental data.
---
> the parameter region where some UHECR source leading candidates are expected to be distributed.
> The bound significantly upgraded from our previous publication~\cite{icecubeEHE2011}
> was brought by both the enlarged instrumentation volume and
> the refined Monte Carlo simulations with improved agreements to the experimental data.
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< driving the IceCube program to search for extremely-high-energy cosmic neutrinos.
< I also deeply acknowledge the entire IceCube collaboration for their enthusiastic support
< in the data analysis, simulations, as well as the stable operations of the detector.
---
> driving the IceCube program to search for extremely-high energy cosmic neutrinos.
> I also deeply acknowledge the entire IceCube collaboration for their enthusiastic supports
> on the data analysis, simulations, as well as the stable operations of the detector.