EHE MC Check K. Mase* on behalf of EHE penguins, Chiba university*

Collaboration Meeting Oxford Keiichi Mase ■ Simulated Chiba  Muons are simulated with JULIeT.  JULIeT → photonics → ROMEO → DOM simulator and calibrator → weighting- module  6 < log 10 E < 9 [GeV]  dF/dE = E -1  The direction is uniform (default)  The position is uniform within 880 m radius.  The interaction of pair creation, brems. and photo-nuclear, and the decay is switched on. (default)  bulk ice photonics table ■ The purpose of this study  To check the MC for the Extremely High Energy (EHE) nutrinos (muons). ■ Test data  generated at Madison (Aya, Paolo) and Chiba (Keiichi, Shigeru)

10 16 eV10 15 eV eV10 18 eV10 20 eV eV

Collaboration Meeting Oxford Keiichi Mase ■ Primary Particle Log 10 (Primary energy) [GeV] cos(theta) [rad.] # ## Azimuth [rad.]  This is fine!

Collaboration Meeting Oxford Keiichi Mase ■ The highest energy cascade along a muon track X [m] Log 10 (Primary energy) [GeV] ## ## Z [m] Y [m]

Collaboration Meeting Oxford Keiichi Mase ■ The highest energy cascade along a muon track Log 10 (Primary energy) [GeV] Log 10 (highest cascade energy) Pair creation+brems.+photo-nuclear Only pair creation

Collaboration Meeting Oxford Keiichi Mase ■ The z position of the highest energy cascade upgoing uniform downgoing  Strange  even only pair creation case  Need debug

Collaboration Meeting Oxford Keiichi Mase Log 10 (Primary energy) [GeV] Log 10 (dF/dLog 10 E) [/cm 2 /s/sr] downgoing Log 10 (Primary energy) [GeV] Log 10 (dF/dLog 10 E) [/cm 2 /s/sr] upgoing ■ Weight module for JULIeT (Aya) JULIeT numerical calc. Log 10 (Simulated Flux) [/cm 2 /sr] Log 10 (Primary energy) [GeV] upgoing Log 10 (Primary energy) [GeV] Log 10 (Simulated Flux) [/cm 2 /sr] downgoing Simulated flux → weight

Collaboration Meeting Oxford Keiichi Mase ■ Detector response Log 10 (Primary energy) [GeV] log 10 (Total Np.e.) log 10 (OM Hits) Log 10 (Primary energy) [GeV]  There are correlation.

Collaboration Meeting Oxford Keiichi Mase ■ Consuming time  It takes too much time for high energy (log 10 E > 9 GeV). Only 1 big event  Xeon 2.4GHz  Used Project I3DefaultPhysicsSource I3DefaultDetectorStatusSource I3DefaultCalibrationSource I3TextFileGeometrySource I3MCCalibrationFiller I3MCRawDOMStatusFiller I3CalibrateStatusModule I3JulietPrimaryParticleSource I3Juliet I3HitConstructor I3NoiseGeneratorModule I3RomeoInterfaceModule I3DOMsimulator I3DOMcalibrator I3BoostPhysicsWriter I3BoostGeometryWriter I3BoostCalibrationWriter Averaged over 100 events Acceptable level (1000 events/week) 5.36 s/event 289 s/event 501 s/event 383 s/event ← 1 hour

Collaboration Meeting Oxford Keiichi Mase ■ Summary and future plan  The MC software to study EHE neutrinos are almost ready.  However, there are several problems.  strange distribution of the maximum cascade z position  It takes too much time to simulate high energy events (log 10 E > 9 GeV).  Other parameters and the waveform should be checked.  We will start mass production of MC events after fixing the above problems.  We will develop a reconstruction method for the EHE neutrino events.

Collaboration Meeting Oxford Keiichi Mase Backup

Collaboration Meeting Oxford Keiichi Mase ■ Technical problem  When I run large number of events, I got a error. > private/dataclasses/I3DOMCalibration.cxx:84 Invalid ATWD channel in I3DOMCalibration > private/root-icetray/RootI3Tray.cxx:443 Invalid ATWD channel in I3DOMCalibration > private/root-icetray/RootI3Tray.cxx:457 Fatal exception caught: Invalid ATWD channel in I3DOMCalibration

Collaboration Meeting Oxford Keiichi Mase Neutrino-Induced Cascades: Signature of  e and  are hadronic and electro-magnetic cascades. Neutral Current interactions of all neutrino flavors produce hadronic cascades Background consists of atmospheric muons, emitting energetic secondaries S Signal and Background ~ 5 m

Collaboration Meeting Oxford Keiichi Mase Bartol 2004 Angular Spectrum 1400 m 2800 m 11000m UpDown

Collaboration Meeting Oxford Keiichi Mase Events in Energy-direction plane By Monte Carlo GZK domain Atm  domain

Collaboration Meeting Oxford Keiichi Mase Energy deposit profile in km 3 By the JULIeT Monte Carlo function

Collaboration Meeting Oxford Keiichi Mase IceCube EHE Sensitivity 90% C.L. for 10 year observation

Collaboration Meeting Oxford Keiichi Mase Particle identification IceCube Solid: particle ID, direction, and energy Shaded: energy only (Supernova detection)

Collaboration Meeting Oxford Keiichi Mase ■ Software for EHE neutrinos JULIeT Photonics ROMEODOM Sim EHE propagator Cherenkov Detector Electronics  2D absolute sensitivity included  saturation included  Speed improved → need more. Now, the software is almost ready.

Collaboration Meeting Oxford Keiichi Mase ■ Consuming time  It takes too much time for high energy (log 10 E > 9 GeV). Only 1 big event  Xeon 2.4GHz  Used Project I3DefaultPhysicsSource I3DefaultDetectorStatusSource I3DefaultCalibrationSource I3TextFileGeometrySource I3MCCalibrationFiller I3MCRawDOMStatusFiller I3CalibrateStatusModule I3JulietPrimaryParticleSource I3Juliet I3HitConstructor I3NoiseGeneratorModule I3RomeoInterfaceModule I3DOMsimulator I3DOMcalibrator I3BoostPhysicsWriter I3BoostGeometryWriter I3BoostCalibrationWriter 100 events 21.45s/4events 1154s/4events 2003s/4events 3015s/4events 1533s/4events

Collaboration Meeting Oxford Keiichi Mase amanda-core dataclasses dataio examples-offline icetray offline-mk phys-services root-icetray ithon eventviewer eventviewer-modules I3Db analysis-tree monolith-reader triggerUtil-C++ DOMcalibrator ICETRAY-APP OFFLINE-SOFTWARE DOMsimulator PSInterface c2j-icetray corsika++ hit-constructor mmc mmc-icetray noise-generator romeo romeo-amanda romeo-interface i3anis simple-muon juliet juliet-interface ucr-icetray TWRSimulator cascade-generator examples-simulation topsim weighting-module FeatureExtractor atmo-flux fat-reader