NuTel Video Conference 6/13/2003 M.A. Huang

Slides:

Advertisements

Similar presentations

Antonis Leisos KM3NeT Collaboration Meeting the calibration principle using atmospheric showers the calibration principle using atmospheric showers Monte.

Advertisements

JNM Dec Annecy, France The High Resolution Fly’s Eye John Matthews University of Utah Department of Physics and High Energy Astrophysics Institute.

Atmospheric Neutrinos Barry Barish Bari, Bologna, Boston, Caltech, Drexel, Indiana, Frascati, Gran Sasso, L’Aquila, Lecce, Michigan, Napoli, Pisa, Roma.

Results from the Telescope Array experiment H. Tokuno Tokyo Tech The Telescope Array Collaboration 1.

Alignment study 19/May/2010 (S. Haino). Summary on Alignment review Inner layers are expected to be kept “almost” aligned when AMS arrives at ISS Small.

VHENTW, 4/25/206M.A. Huang SHENIE: Simulation of High Energy Neutrino Interacting with the Earth M.A. Huang a, Y.L. Hong b, C.H. Iong bc, G.L. Lin b (a)

George W.S. Hou & M.A. Huang Center for Cosmology and Particle Astrophysics Department of Physics, National Taiwan University, 1, Sec. 4, Roosevelt Rd.,Taipei,

M. Kowalski Search for Neutrino-Induced Cascades in AMANDA II Marek Kowalski DESY-Zeuthen Workshop on Ultra High Energy Neutrino Telescopes Chiba,

Reconstruction of neutrino interactions in PEANUT in general scanning (unbiased) mode Giovanni De Lellis on behalf of Andrea Russo Naples University.

Frictional Cooling MC Collaboration Meeting June 11-12/2003 Raphael Galea.

Tampa APS Meeting April 2004 P. Gorham 1 UH ANITA monte carlo Peter Gorham University of Hawaii A N I T A.

First Observations of Separated Atmospheric  and  Events in the MINOS Detector. A. S. T. Blake* (for the MINOS collaboration) *Cavendish Laboratory,

Detecting Earth-Skimming and Mountain-Penetrating Tau Neutrinos G.-L.Lin National Chiao-Tung University, Taiwan ISMD04.

P. Gorham, SLAC SalSA workshop1 Saltdome Shower Array: Simulations Peter Gorham University of Hawaii at Manoa.

EHE Lepton Propagation in the Earth and Its Implications to the IceCube EHE  Propagation in the Earth EHE  Propagation in the Earth What is the.

GLAST background review dec Simulating rates: the big picture Incoming rate into the 6 m 2 sphere: is it right? Corresponding trigger rate: implies.

Study of e + e  collisions with a hard initial state photon at BaBar Michel Davier (LAL-Orsay) for the BaBar collaboration TM.

MPBACH MultiPixel Balloon-borne Air CHerenkov Detection of Iron Cosmic Rays Using Direct Cherenkov Radiation Imaged with a High Resolution Camera 1.

Atmospheric Neutrino Oscillations in Soudan 2

MP BACH MultiPixel Balloon-borne Air CHerenkov Detection of Iron Cosmic Rays Using Direct Cherenkov Radiation Imaged with a High Resolution Camera University.

Computational Lab in Physics: Final Project Monte Carlo Nuclear Collisions: Glauber Model.

Experiment Rosen07: Measurement of R =  L /  T on Deuterium in the Nucleon Resonance Region. 1  Physics  Data Analysis  Cross Section calculation.

The showers Induced be e with LPM effect included (red stars) look very different from showers without LPM effect (blue stars).The showers are more elongated.

1/8-10/2007M.A. Huang CRTNT Experiment Status  Introduction  Two prototype telescopes  Test run on ARGO-YBJ site, Tibet  Full scale experiment: 2008.

EAS Reconstruction with Cerenkov Photons Shower Simulation Reconstruction Algorithm Toy MC Study Two Detector Configuration Summary M.Z. Wang and C.C.

Latest Results from the MINOS Experiment Justin Evans, University College London for the MINOS Collaboration NOW th September 2008.

NESTOR SIMULATION TOOLS AND METHODS Antonis Leisos Hellenic Open University Vlvnt Workhop.

Humberto Salazar (FCFM-BUAP) for the Pierre Auger Collaboration, CTEQ- Fermilab School Lima, Peru, August 2012 Ultrahigh Cosmic Rays: The highest energy.

AGASA Results Masahiro Teshima for AGASA collaboration

Detection of electromagnetic showers along muon tracks Salvatore Mangano (IFIC)

3/22/2002M.A. Huang George W.S. Hou & M.A. Huang Center for Cosmology and Particle Astrophysics Department of Physics, National Taiwan University.

Detection of UHE Shower Cores by ANITA By Amir Javaid University Of Delaware.

RICE: ICRC 2001, Aug 13, Recent Results from RICE Analysis of August 2000 Data See also: HE228: Ice Properties (contribution) HE241: Shower Simulation.

Update on Rolling Cascade Search Brennan Hughey UW-Madison

6/27/2003 Event Rate Estimation -2 NuTel Video Conference 6/27/2003 M.A. Huang.

Interactions with Rest Gas – Typical Case Interactions with Rest Gas – ELENA Quantitative analysis for ELENA Evaluations at 100 keV Ejection Energy Evaluations.

Current Physics Results Gordon Thomson Rutgers University.

OUTGOING NEUTRONS IN CALET CALET AIMS AT DETECTING UHE CR ELECTRONS HIGH REJECTION FACTOR FOR PROTONS/NUCLEI NEEDED POSSIBLE IMPROVEMENT RESPECT ‘STANDARD’

31/03/2008Lancaster University1 Ultra-High-Energy Neutrino Astronomy From Simon Bevan University College London.

Olivier Deligny for the Pierre Auger Collaboration IPN Orsay – CNRS/IN2P3 TAUP 2007, Sendai Limit to the diffuse flux of UHE ν at EeV energies from the.

A New Upper Limit for the Tau-Neutrino Magnetic Moment Reinhard Schwienhorst      ee ee

Search for UHE Neutrinos with AMANDA Stephan Hundertmark University of California, Irvine Methodical Aspects of Underwater/Ice Neutrino Telescopes Hamburg,

AGASA Results Masahiro Teshima Max-Planck-Institut für Physik, München, Germany for AGASA collaboration.

IC40 Spectrum Unfolding 7/1/2016Warren Huelsnitz1 SVD Method described in A. Höcker and V. Kartvelishvili, NIM A 372 (1996) 469NIM A 372 (1996) 469 Implemented.

SADE ANITA Monte Carlo(SAM) Test Results Amir Javaid University of Delaware.

SADE ANITA Monte Carlo(SAM) Test Results Amir Javaid University of Delaware.

ICARUS T600: low energy electrons

Neutral Current Interactions in MINOS Alexandre Sousa, University of Oxford for the MINOS Collaboration Neutrino Events in MINOS Neutrino interactions.

Muons in IceCube PRELIMINARY

Development of the 21CMA radio-detection array (Xinjiang/China) for the observation of UHE neutrinos showers Didier Charrier1, Pascal Lautridou1, Olivier.

(Xin-Heng Guo, Bing-Lin Young) Beijing Normal University

A.Smirnov, A.Sidorin, D.Krestnikov

Primary estimation of CEPC beam dilution and beam halo

Gamma Ray Constraints on New Physics Interpretations of IceCube Data

Calculation of detector characteristics for KM3NeT

Event Rates vs Cross Sections

Relativistic Magnetic Monopole Flux Constraints from RICE

MUPAGE: A fast muon generator

CRTNT Project & Cosmic RayτNeutrino (>1 PeV) Measurement

Nonequilibrium Green’s Function with Electron-Phonon Interactions

Using Single Photons for WIMP Searches at the ILC

Unfolding performance Data - Monte Carlo comparison

Estimation of Sensitivity to Gamma Ray point Sources above 30TeV

Study of e+e collisions with a hard initial state photon at BaBar

NKS2 Meeting with Bydzovsky NKS2 Experiment / Analysis Status

ICRC2011, 32ND INTERNATIONAL COSMIC RAY CONFERENCE, BEIJING 2011

Ultra-high energy upward going muons in Super-Kamiokande II

ANITA simulations P. Gorham 5/12/2019 P. Gorham.

Update on POLA-01 measurements in Catania

Hellenic Open University

Presentation transcript:

NuTel Video Conference 6/13/2003 M.A. Huang Event Rate Estimation NuTel Video Conference 6/13/2003 M.A. Huang 6/13/2003

Monte Carlo simulation Uniform and isotopic distribution of neutrino trajectory. Interaction of mountain/sea/atmosphere Cross-section Inelasticity Tau energy loss and decay Tau decay and initiate shower Shower simulation Detector simulation 6/13/2003

Progress report Individual event simulation is not finish yet! No shower and photon information. No exact trigger condition. Preliminary estimation of event rate by Trigger simulation  photo-electron density Shower simulation  maximum detectable distance MC simulation  triggered events  acceptance Tau flux  Event rate 6/13/2003

Monte-Carlo simulation Ntot =106 Neutrino trajectories are simulated Uniform distribution in impact points Isotropic distribution in arrival directions Rp V D Detector - Neutrino plane Rp V Detector Rp : impact parameter D : distance to impact point 6/13/2003

Uniform Distribution Uniform distribution in impact points number density  = Ntot / total volume dN/dR = 4R2 Rp=Rmax* P1/3 ; P: random probability cos: -1 to +1 : -180 º to +180º 6/13/2003

Isotropic Vz Rp V Vy Vx Detector Select random vector on plane perpendicular to Rp vector, then rotate it back to detector coordinate. Rp V Detector Vy Vx 6/13/2003

Simulated Acceptance Generated acceptance AMC = 2 3 R 2 For R = 5 km, AMC  1550 km2 sr r Detector R   6/13/2003

Trigger conditions 1015 eV electron showers, injected from 20, 30, 40 km from detector plan. Two types of Trigger 50 /m2 200 /m2 Details see S.C. Hsu’s talk D 200 /m2 50 /m2 Rp 6/13/2003

Range of impact parameter Event can be triggered if Rp-D inside phase space of trigger region shown above. D must be greater than 5 km, to allow shower development Rp V D Detector - Neutrino plane 6/13/2003

Field of View Loa (8º32º) : :90º - 98º ; : 114º -146º Peak of Loa and Kea disappear! Too far! Loa (8º32º) : :90º - 98º ; : 114º -146º Kea (8º32º) : :91º - 99º ; : 54º - 86º Loa + Kea (12º100º) : :89º - 101º ; : 50º - 150º 6/13/2003

Triggered events Earth skimming events dominate, most events coming from bottom of valley. 6/13/2003

Acceptance Ntr: # of events pass trigger conditions Atr: Triggered acceptance Ntot: # of events in simulation = 106 AMC: Simulate acceptance = 1550 km2 sr 6/13/2003

Acceptance Trigger at 50 /m2 6/13/2003

Acceptance Trigger at 200 /m2 6/13/2003

Tau flux Tau flux at 1-30 PeV ~ 2-51034 (cm2 sr s eV)1 1 to 30 PeV Tau flux at 1-30 PeV ~ 2-51034 (cm2 sr s eV)1 Consistent fluxes from calculations of La Babara and G.L. Lin. Integrated flux from 1 to 30 PeV,  ~ 30. (km2 sr yr) 1 45.7 (km2 sr yr) 1 if use peak value 5 1034 (cm2 sr s eV)1 6/13/2003

Event Rate Event rate R = A0.1 Assume 10% duty time Number of trigger event per year 6/13/2003

Discussion Based on 1015 eV shower, E 2.51015 eV Expect higher acceptance at higher energy, Event rate could be higher than estimated value. Average distance to impact point ~ 10 km, Best site should have valley width  25 Km For AGN-, NuTel could detect several events per year at E=1-30 PeV. 6/13/2003