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Atmospheric neutrino fluxes

This article discusses the background and measurement of atmospheric neutrino fluxes, as well as the accuracy of current predictions. It also introduces a C++ class and library for simulating and analyzing neutrino fluxes. The article highlights the importance of accurate flux measurements for experiments like AMANDA (IceCube) and the potential contribution of FLUKA simulations.

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Atmospheric neutrino fluxes

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  1. Atmospheric neutrino fluxes • A background and an interesting measurement • How well do we know the atmospheric neutrino fluxes? • The primary CR spectrum • Can we have a muon and neutrino flux from the same code? • A tool for simulation and analysis: a C++ class and a library • for fluxes (suitable for ANIS and IceTray) • It is a beautiful measurement with the largest data • sample AMANDA (IceCube) have since K physics and prompt • Fluxes are poorly constrained by accelerator data Teresa Montaruli, Paolo Desiati, Aya Ishihara, UW, IceCube Meeting, Mar 2005

  2. MACRO final data  Honda 2001  Honda 1995  Bartol 1996  SK Data Bartol 96 HKKM (2001 CR) FLUKA (2001 CR) FLUKA (1996 CR) ~20% predictions no oscill. Em>1 GeV predictions Dm2=2.5 10-3eV2 SK and MACRO through-going muon data pointed out that the CR assumed after ICRC2001 by HKKM and Bartol was too steep and that a better agreement was achieved with the previous Agrawal et al. 1996 CR flux Moreover ATIC data preferred E-2.7 to steeper spectra Super-Kamiokande and MACRO TM, ICRC2003 HE rapporteur talk

  3. p He Primary CRs 5% agreement between AMS and Bess98 < 100 GeV BUT CAPRICE -20% ICRC2001 assumes AMS-Bess The region relevant for AMANDA/IceCube is higly uncertain due to large errors of Jacee and RunJob data Moreover He and heavy components are worse known and their relevance increases Primary spectra: ICRC2001 (softer), Agrawal or Old Bartol (harder)

  4. The inputs: primary CRs in most recent calculations Main difference between ICRC2001/Gaisser-Honda 2002: CNO+Si-Mg+Fe E-2.7/harder Main difference between ICRC2001/HKKM 2004: He [average of E-2.74+E-2.64]/E-2.64] + protons [E-2.74/ E-2.74+E-2.71 (E>100 GeV)] Results: HKKM 2004 is closer to previous Agrawal et al, 1996, harder than ICRC2001 and Gaisser-Honda fit resulting in more through-going muons Gaisser-Honda 2002

  5. These results agree with: Gaisser astro-ph/0502380 Theoretical Errors Though HKKM 2004 uses a harder spectrum than Bartol, it is lower! Interaction models are different (Target 2/DPMJET-III – to be updated 15% lower than L3 m data) Lots of comparisons between Bartol, HKKM and FLUKA groups resulted in uncertainty reduction also thanks to muon data in the atmosphere. These groups published their results in 2003-2004. Can AMANDA data help? How does Lipari flux (used in AMANDA) compare to the more recent calculations?

  6. AMANDA DATA hep-ex/0501064 SK data prefer higher fluxes by 12% and harder spectra than HKKM2004 +0.05 >100 GeV AMANDA works in a higher E region where oscillations play a small role BUT in the region where hadronic models are worsely known (K physics, prompts…) Systematics need to be reduced – Paolo’s talk!!!!

  7. Atmospheric ns and ms with FLUKA FLUKA (http://www.fluka.org) new runs extending up to 106 GeV/nucleon started at UW. The goal is to have neutrinos from 4p and atmospheric muons from the same interaction and transport code (first 3D code, Astr.Phys.19, 2003) Prompt neutrinos and muons will be addressed when DPMJET-III interface will be ready FLUKA yet poor statistics L3 m data can help reducing systm at HE

  8. The inputs: primary CR for VHE spectrum NEW FLUKA generation: CR suitable for VHE

  9. The AtmosphericFlux Class • The constructor: AtmosphericFlux mymodel(model); • Class Methods: Init: Read Tables in prepared in common format Flux: returns the flux at a given energy, angle and for a flavor eg: double flux = mymodel.Flux(1,1.e3,0.1); returns: flux in GeV-1 cm-2 sr-1 s-1 given: • Neutrino type: ne, anti-ne, nm, anti-nm • Neutrino Energy • Cos(zenith) Average flux: returns averaged over lower hemisphere Compatible with ANIS Usable by IceTray (A. Hishihara) Usable in analysis stage with ROOT as a shareable library Extensible to ANY FLUX (can become a library of fluxes to be used for event reweighting purposes)

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