Calculation of atmospheric neutrino flux using the interaction model calibrated with atmospheric muon data

By Mitsuhiko Honda, T. Kajita, K. Kasahara, S. Midorikawa, T. Sanuki. 2006

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Using the ``modified DPMJET-III'' model explained in the previous paper [T. Sanuki et al., preceding Article, Phys. Rev. D 75, 043005 (2007).], we calculate the atmospheric neutrino flux. The calculation scheme is almost the same as HKKM04 [M. Honda, T. Kajita, K. Kasahara, and S. Midorikawa, Phys. Rev. D 70, 043008 (2004).], but the usage of the ``virtual detector'' is improved to reduce the error due to it. Then we study the uncertainty of the calculated atmospheric neutrino flux summarizing the uncertainties of individual components of the simulation. The uncertainty of $K$-production in the interaction model is estimated using other interaction models: FLUKA'97 and FRITIOF 7.02, and modifying them so that they also reproduce the atmospheric muon flux data correctly. The uncertainties of the flux ratio and zenith angle dependence of the atmospheric neutrino flux are also studied.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/564b9d2859750e391c85061ebf97e8c8baa26769

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Citations in the corpus

Letter of Intent: The Precision IceCube Next Generation Upgrade (PINGU) (2014, methodology): “Events are generated isotropically from a user-defined power law distribution (normally E−2) and can be reweighted to reproduce the atmospheric neutrino spectrum [35].”
KM3MeT 2.0 Letter of intent for ARCA and ORCA (2016, methodology): “Additionally, CORSIKA underestimates the expected atmospheric neutrino flux at high energies [18,19], and this is corrected for as per [35].”
Letter of intent for KM3NeT 2.0 (2016, methodology): “The background of atmospheric neutrinos assumed in these analyses corresponds to the so-called Honda flux [18] with a prompt component as calculated by Enberg [19].”
OBSERVATION AND CHARACTERIZATION OF A COSMIC MUON NEUTRINO FLUX FROM THE NORTHERN HEMISPHERE USING SIX YEARS OF ICECUBE DATA (2016, methodology): “In addition, nuisance parameters are introduced to take into account systematic uncertainties, e.g., the conventional atmospheric neutrino flux is described by the prediction taken from Honda et al. (2007) and the flux normalization Fconv is taken as a nuisance parameter.”
Extending the Search for Muon Neutrinos Coincident with Gamma-Ray Bursts in IceCube Data (2017, background): “As such, the background energy PDF can be artificially extended to very high energies by using simulated neutrino events with an atmospheric spectrum(Honda et al. 2007).”
Invited review: Physics potential of the ICAL detector at the India-based Neutrino Observatory (INO) (2015, background): “[5], based on the analysis of cosmic ray neutrino fluxes from [92], [93] and [94].”
A COMBINED MAXIMUM-LIKELIHOOD ANALYSIS OF THE HIGH-ENERGY ASTROPHYSICAL NEUTRINO FLUX MEASURED WITH ICECUBE (2015, methodology): “For the conventional atmospheric neutrinos, we use the HKKMS model by Honda et al. (2007) and for the prompt atmospheric neutrinos, we use the ERS model by Enberg et al. (2008).”
AN INDIRECT SEARCH FOR WEAKLY INTERACTING MASSIVE PARTICLES IN THE SUN USING 3109.6 DAYS OF UPWARD-GOING MUONS IN SUPER-KAMIOKANDE (2011, methodology): “We use the neutrino flux calculated by ( Honda et al. (2007) ; Eν <10 TeV) and ( Volkova (1980) ; Eν >10 TeV) for this simulation.”
IceCube high-energy starting event sample: Description and flux characterization with 7.5 years of data (2020, background): “[101] and the latter is given in the BERSS flux calculations [103].”
All-sky Search for Time-integrated Neutrino Emission from Astrophysical Sources with 7 yr of IceCube Data (2016, background): “In the northern sky (θ> 85°), the sample is dominated by atmospheric neutrinos produced in the decays of kaons and pions in cosmic-ray air showers(Honda et al. 2007) and is well described by Monte Carlo simulation.”
Global fit to three neutrino mixing: critical look at present precision (2012, methodology): “For the sake of comparison with the results of the analysis of the Super-Kamiokande collaboration, in our atmospheric analysis with phases SK1–4 the no-oscillation expectations have been normalized to those obtained with the new Honda fluxes [95], while the analysis from SK1–3 is done with the previ”