Primary Energy Reconstruction Method for Air Shower Array Experiments
This study presents an event-by-event method for unfolding the all-particle energy spectrum in air shower array experiments. It introduces an inverse problem solution through analytical or numerical integration. The advantages include simplicity and a general formulation, with solutions like a regularized unfolding iterative algorithm and parameterization of the inverse problem with a priori spectral information. However, there are challenges such as pseudo solutions for elemental spectra and undefined systematic errors. The work addresses an ill-posed problem due to a wide range of primary particle types and redefines the inverse problem. A multi-parametric energy estimator is developed using CORSIKA EAS simulation and ICETOP detector response, with a focus on minimizing errors in the reconstructed spectrum. Validation is done by comparing expected and reconstructed spectra for different particle types like proton, helium, oxygen, and iron.
Primary Energy Reconstruction Method for Air Shower Array Experiments
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Primary Energy Reconstruction Method for Air Shower Array Experiments SamvelTer-Antonyanand Ali Fazely
Inverse Problem for All-particle energy spectrum Event-by-event method Unfolding Advantage: simplicity Solution: analytical or numerical integration [J. Phys. G: Nucl. Part. Phys. 35 (2008) 115] Disadvantage: ? The most experiments ignore the methodic errors. Advantage: general formulation Solutions: a) regularized unfolding iterative algorithm [KASCADE Collaboration , Astropart.Phys. 24 (2005) 1] b) parameterization of inverse problem + + a priory spectral info. [GAMMA Collaboration, Astropart.Phys. 28 (2007) 169] Disadvantage: Pseudo solutions for elemental spectra and undefined systematic errors for unfolding algorithms (KASCADE). [S. Ter-Antonyan, Astropart.Phys. 28 (2007) 321]
Event-by-eventanalysis [GAMMA_09] [KASCADE-GRANDE] Energy estimator: [ICETOP_09] This work is ill-posed problem for F(E0)due to A H, He, … Fe Redefinition of inverse problem: =2.9 0.25 for 1 PeV E0 < 500 PeV • a priori: • Let and and , for , - constant
Solution for primary spectrum 2% , and |a|<< 0.1 where • Spectral errors: Statistic Errors Methodic Errors
Multi-parametric energy estimator for ICETOP Array: • CORSIKA EAS SIMULATION • + • ICETOP DETECTOR RESPONSE • + • LDF RECONSTRUCTION min{2(a1,a2,…a6,(Ei)| E0,i)} i=1,…104, AH, He, O, Fe
Expected biases and uncertainties of primary energy ICETOP • GAMMA Experiment <Ln(E1/E0)> if then Log(E0/GeV) (Ln(E1/E0)) Log(E0/GeV)
Verification of method Expected reconstructed all-particle spectrum for ICETOP Primary energy spectra for p, He, O, Fefrom GAMMA Experiment data [GAMMA Collaboration, Astropart.Phys. 28 (2007) 169]
Expected (red symbols) all-particle spectrum for ICETOP
