Atmospheric Neutrino Fluxes Giles Barr XXIst International Conference on Neutrino Physics and Astrophysics Neutrino 2004 Paris.

Slides:

Advertisements

Similar presentations

Stefan Roesler SC-RP/CERN on behalf of the CERN-SLAC RP Collaboration

Advertisements

Soudan 2 Peter Litchfield University of Minnesota For the Soudan 2 collaboration Argonne-Minnesota-Oxford-RAL-Tufts-Western Washington  Analysis of all.

Super-Kamiokande Introduction Contained events and upward muons Updated results Oscillation analysis with a 3D flux Multi-ring events  0 /  ratio 3 decay.

Atmospheric neutrino fluxes Teresa Montaruli, Paolo Desiati, Aya Ishihara, UW, IceCube Meeting, Mar 2005 A background and an interesting measurement How.

Searching for the footprint of prompt atmospheric neutrino flux and beyond Guey-Lin Lin National Chiao-Tung U. Taiwan With N. Tung and F.-F. Lee KEKPH.

Cosmic Rays Basic particle discovery. Cosmic Rays at Earth – Primaries (protons, nuclei) – Secondaries (pions) – Decay products (muons, photons, electrons)

TeVPA, July , SLAC 1 Cosmic rays at the knee and above with IceTop and IceCube Serap Tilav for The IceCube Collaboration South Pole 4 Feb 2009.

Tom Gaisser October 29, 2002 Oxford Atmospheric neutrinos from decay of , K and  produced by interactions of cosmic rays in the atmosphere Up-down symmetric.

An accelerator beam of muon neutrinos is manufactured at the Fermi Laboratory in Illinois, USA. The neutrino beam spectrum is sampled by two detectors:

Presented by Steve Kliewer Muon Lifetime Experiment: A Model.

Gravitational waves LIGO (Laser Interferometer Gravitational-Wave Observatory ) in Louisiana. A laser beam is.

Counting Cosmic Rays through the passage of matter By Edwin Antillon.

May 26, 2002Thomas K. Gaisser Atmospheric neutrino fluxes Status of the calculations based on work with M. Honda.

Chiba, July 29, 2003Tom Gaisser Comments on atmospheric muon and neutrino backgrounds in neutrino telescopes Use semi-analytic estimates to display some.

First energy estimates of giant air showers with help of the hybrid scheme of simulations L.G. Dedenko M.V. Lomonosov Moscow State University, Moscow,

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.

EHE Search for EHE neutrinos with the IceCube detector Aya Ishihara for the IceCube collaboration Chiba University.

Constraints of hadronic interaction models from the cosmic muon observations. L.G. Dedenko, A.V. Lukyashin, G.F. Fedorova, T.M. Roganova M.V. Lomonosov.

Size and Energy Spectra of incident cosmic radiation obtained by the MAKET - ANI surface array on mountain Aragats. (Final results from MAKET-ANI detector)‏

The FLUKA high energy cosmic ray generator: predictions for the charge ratio of muons detected underground G. Battistoni, A. Margiotta, S. Muraro, M. Sioli.

Final results on atmospheric  oscillations with MACRO at Gran Sasso Bari, Bologna, Boston, Caltech, Drexel, Frascati, Gran Sasso, Indiana, L’Aquila, Lecce,

Atmospheric shower simulation studies with CORSIKA Physics Department Atreidis George ARISTOTLE UNIVERSITY OF THESSALONIKI.

Flux calculation results and systematic errors from Bartol calculation presented by Giles Barr, Oxford with considerable help from Simon Robbins ICRR-Kashiwa.

Geomagnetic Spectroscopy: An Estimation of Primary Mass of Cosmic Rays Rajat K Dey 1,2 Arunava Bhadra 2 Jean-No ë l Capdevielle 3 1 Department of Physics.

Cosmic Rays GNEP Teacher Workshop Steve Shropshire, July 2007.

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

Atmospheric neutrinos

XXXI International Cosmic Ray Conference, ICRC 2009 Lodz, Poland, July 7-15, 2009 Time structure of the Extensive Air Shower front with the ARGO-YBJ experiment.

The muon component in extensive air showers and its relation to hadronic multiparticle production Christine Meurer Johannes Blümer Ralph Engel Andreas.

Mumbai, August 1, 2005 Tom Gaisser Atmospheric neutrinos Primary spectrum Hadronic interactions Fluxes of muons and neutrinos Emphasis on high energy.

Cosmic rays at sea level. There is in nearby interstellar space a flux of particles—mostly protons and atomic nuclei— travelling at almost the speed of.

Charged Kaon Production Yield Studies with Stretcher Sergei Striganov Fermilab Future of Kaon Physics at Fermilab August 21, Fermilab.

Study of the Atmospheric Muon and Neutrinos for the IceCube Observatory Ryan Birdsall Paolo Desiati, Patrick Berghaus,

Nucleon Decay Search in the Detector on the Earth’s Surface. Background Estimation. J.Stepaniak Institute for Nuclear Studies Warsaw, Poland FLARE Workshop.

“The Cosmic Ray composition in the knee region and the hadronic interaction models” G. Navarra INFN and University, Torino, Italy For the EAS-TOP Collaboration.

Study of high energy cosmic rays by different components of back scattered radiation generated in the lunar regolith N. N. Kalmykov 1, A. A. Konstantinov.

Bartol Flux Calculation presented by Giles Barr, Oxford ICRR-Kashiwa December 2004.

QCD at Cosmic Energies Erice, Aug 30, 2004 Thomas K. Gaisser Hadronic interactions in modeling atmospheric cascades The atmospheric cascade equation Heavy.

School of Cosmic-ray Astrophysics, Erice, July 4, 2004 Thomas K. Gaisser Role of particle interactions in high-energy astrophysics Uncorrelated fluxes.

QUARKS-2014 Suzdal 7 June 2014 Testing High Energy Cosmic Ray Interaction Models with the Atmospheric Muon Data L.G. Dedenko, G.F. Fedorova, T.M. Roganova.

Cosmic ray physics in ALICE Katherin Shtejer Díaz For the ALICE Collaboration LatinoAmerican Workshop on High Energy Physics: Particles and Strings, Havana,

Hadron Production Measurements presented by Giles Barr, Oxford ICRR-Kashiwa December 2004.

The Hybrid Scheme of Simulations of the Electron- photon and Electron-hadron Cascades In a Dense Medium at Ultra-high Energies L.G. Dedenko M.V. Lomonosov.

March 3, 2009Tom Gaisser1 Neutrino oscillations Review of particle physics, neutrino interactions and neutrino oscillations.

8/15/2011ICRC Beijing1 PRODUCTION OF SECONDARY COSMIC RAYS IN THE UPPER ATMOSPHERE D. Müller P.J. Boyle 1 J.R. Hörandel 2 A. Obermeier 2 THE UNIVERSITY.

Atmospheric Neutrinos Phenomenology and Detection p 00 ++  e+e+ e-e- ++  Michelangelo D’Agostino Physics C228 October 18, 2004.

Workshop on AstroParticle Physics, WAPP 2009 Bose Institute, Darjeeling, December 2009 Extensive Air Showers and Astroparticle Physics Observations and.

Influence of diffractive interactions on cosmic rays air showers ABSTRACT: A comparative study of commonly used hadronic collision simulation packages.

QUARKS-2010, Kolomna1 Study of the Energy Spectrum and the Composition of the Primary Cosmic Radiation at Super-high Energies.

All lepton generation and propagation with MMC Dmitry Chirkin, UCB/LBNL AMANDA meeting, Uppsala, 2004.

On the Prospect of Tau Neutrino Astronomy in GeV Energies and Beyond G.-L. Lin National Chiao-Tung U. Taiwan Moriond 2005.

Search for a Diffuse Flux of TeV to PeV Muon Neutrinos with AMANDA-II Detecting Neutrinos with AMANDA / IceCube Backgrounds for the Diffuse Analysis Why.

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.

Review of experimental results on atmospheric neutrinos Introduction Super-Kamiokande MACRO Soudan 2 Summary Univ. of Tokyo, Kamioka Observatory.

Bartol Atmospheric Neutrino Fluxes Giles Barr, Thomas K. Gaisser, Todor Stanev 1 st Atmospheric Neutrino Workshop Garching, Germany 7 February 2016 Presented.

1 Cosmic Ray Physics with IceTop and IceCube Serap Tilav University of Delaware for The IceCube Collaboration ISVHECRI2010 June 28 - July 2, 2010 Fermilab.

Measurement of high energy cosmic rays by the new Tibet hybrid experiment J. Huang for the Tibet ASγCollaboration a a Institute of high energy physics,

Atmospheric neutrinos with Deep Core

Muons in IceCube PRELIMINARY

IceCube Collaboration Meeting

Giles Barr Cosener’s House 19 Feb 2005

Direct Measurement of the Atmospheric Muon Spectrum with IceCube

Systematic uncertainties in MonteCarlo simulations of the atmospheric muon flux in the 5-lines ANTARES detector VLVnT08 - Toulon April 2008 Annarita.

Comparison Of High Energy Hadronic Interaction Models

Measurement of the Atmospheric Muon Charge Ratio by Using a Cosmic Ray Telescope Soheila Abdollahi (Imam Khomeini International University, Sharif University.

08/27/04 Strategies for the search for prompt muons in the downgoing

Comparison Of High Energy Hadronic Interaction Models

Fluxes of atmosperic leptons

Presentation transcript:

Atmospheric Neutrino Fluxes Giles Barr XXIst International Conference on Neutrino Physics and Astrophysics Neutrino 2004 Paris

Synopsis Section 1: Features of atmospheric neutrino fluxes –Cosmic ray cascades –3D effects –Fluxes, flux ratios Section 2: Systematics –Primary fluxes –Hadron production –Other effects

Section 1: Features of Atmospheric neutrino fluxes

Neutrinos produced from a shower Primary cosmic ray: proton or heavier nucleus Interacts in ~90g/cm 2 Atmosphere depth 1050 g/cm 2 Cascade Most hadrons don’t reach ground. Primary cosmic ray N N K π π μ ν π

E ν (GeV) Contained Partially C Through Going ν induced μ

E ν (GeV) Osc Max Down Osc Max Horizontal Osc Max Up Contained Partially C Through Going ν induced μ Δm 2 =2.5 x eV 2

Vertical μ reach Earth’s surface Pions Interact Kaons Interact 3D effects E ν (GeV) Osc Max Down Osc Max Horizontal Osc Max Up Contained Partially C Through Going ν induced μ

Summary of Atmospheric Neutrino Calculations Zatsepin, Kuz’minSP JETP 14:1294(1961)1D E. V. Bugaev and V. A. Naumov,PL B232:391 (1989)1D Agrawal, Gaisser, Lipari, StanevPRD 53:1314 (1996)1DTarget D. PerkinsAsp.Phys. 2:249 (1994)Mu Honda, Kajita, Kasahara, MidorikawaPRD 52:4985 (1995)1DFRITIOF Battistoni et alAsp.Phys 12:315 (2000) Asp.Phys 19:269 (2003) 3DFLUKA P. LipariAsp.Phys 14:171 (2000)3D V. Plyaskin PL B516:213 (2001) hep-ph/ D GHEISHA Tserkovnyak et alAsp.Phys 18:449 (2003)3D CALOR-FRITIOF GFLUKA/GHEISHA Wentz et alPRD (2003)3D Corsika: DPMJET VENUS, UrQMD Liu, Derome, BuénerdPRD (2003)3D Favier, Kossalsowski, ViallePRD (2003)3DGFLUKA Barr, Gaisser, Lipari, Robbins, StanevPRD (July 2004)3DTarget Honda, Kajita, Kasahara, MidorikawaPRD (2001) PRD submitted (2004) 3DDPMJET

Shower graphic Detector No energy threshold 80km altitude Earth’s surface

Shower graphic Detector No energy threshold 80km altitude Earth’s surface

dφ/d ln(E) (m -2 s -1 sr -1 )

Path length distributions From Honda et. al. astro-ph/ Solid 3D at Kamioka, Dashed 1D at Kamioka, Dot 3D at Soudan

Azimuth angle distribution East-West effect NESWNNESWN E ν >315 MeV p p π+π+ π-π- μ+μ+ μ-μ-

Ratios Flavour ratio NM=3D with no bending of secondaries in Earth’s mag field

Section 2: Systematics

Primary fluxes Protons = 75% of all nucleon fluxes Helium = 15% of all nucleons = 60% of all nuclei. αKbc H He CNO Ne-Si Fe(56) Primary Kinetic Energy (GeV/n) dN/dE K /m 2 /s/sr/n Protons Helium Flux of primaries at top of atmosphere

Residuals: Oldest measurements (Data-Fit)/Fit 100%

Residuals: Newer measurements (Data-Fit)/Fit 100%

Residuals: Newest measurements (Data-Fit)/Fit 100%

Effect on neutrino fluxes (Data-Fit)/Fit 100% This includes helium uncertainty shown on next slide

Helium Fluxes (Data-Fit)/Fit 100%

Barton et. al. Atherton et. al. SPY Serpukov Allaby et. al. Abbott et. al. Eichten et. al. Cho et. al. 1 GeV TeV Parent energy 10 Population of hadron- production phase-space for pA → πX interactions. ν μ flux (represented by boxes) as a function of the parent and daughter energies. Measurements. 1-2 p T points 3-5 p T points >5 p T points Can attempt fit all the data simultaneously. Antiproton example: Duperray, Huang, Protasov, Buénerd astro-ph/ GeV TeV 10 Daughter energy Hadron production measurements

Hadron production: From: Wentz et al PRD (2003) Corsika models (Sea level muon fluxes) x p E ν (GeV) Muon fluxes MC comparison

Associative production Effect of a 15% reduction in ΛK + production

Future hadron- production experiments HARP 3-15 GeV at CERN PS MIPP GeV at FNAL MI NA49 100,160 GeV at SPS

Cross section change Effect of artificial increase in total cross section of 15%

Other effects: Atmospheric Density

Other effects: Magnetic field (negligible, but perhaps include a plot from Favier et. al.) From: Favier, Kossakowski and Vialle. PRD (2003) Method A: Generate far from Earth Earth, propagate in (Circles) Method B: Generate near earth and propagate charge- reversed out. Latitude cos(Zenith)

Return to 3D: Is it important? SuperKamiokande Collaboration hep-ex/ D bigger >30% 10%-30% 3%-10% <3% 1D bigger 3%-10% 10%-30%

SuperKamiokande Collaboration hep-ex/ D bigger >30% 10%-30% 3%-10% <3% 1D bigger 3%-10% 10%-30% Return to 3D: Is it important?

Conclusions Since early days of nucleon decay expts and the atmospheric neutrino ‘anomaly’: –Large increase in calculation sophistication –Much improved primary fluxes –Hadron production data still needed 3D effects now well understood.