Abstract
We present the analysis method used to search for an anisotropy in the high energy Cosmic Rays arrival distribution using data collected by the ANTARES telescope. ANTARES is a neutrino detector, where the collected data are dominated by a large background of cosmic ray muons. Therefore, the background data are suitable for high-statistics studies of cosmic rays in the Northern sky. The main challenge for this analysis is accounting for those effects which can mimic an apparent anisotropy in the muon arrival direction: the detector exposure asymmetries, non-uniform time coverage, diurnal and seasonal variation of the atmospheric temperature. Once all these effects have been corrected, a study of the anisotropy profiles along the right ascension can be performed.
Highlights
Cosmic Rays (CRs) in the TeV to PeV range are mainly charged particles, believed to originate in our Galaxy, possibly in local astrophysical accelerators such as supernova remnants
We present the analysis method used to search for an anisotropy in the high energy Cosmic Rays arrival distribution using data collected by the ANTARES telescope
ANTARES is a neutrino detector, where the collected data are dominated by a large background of cosmic ray muons
Summary
Cosmic Rays (CRs) in the TeV to PeV range are mainly charged particles, believed to originate in our Galaxy, possibly in local astrophysical accelerators such as supernova remnants. The recostruction strategy of the events is based on a maximum likelihood method in which the best set of parameters describing the track is estimated through a recursive fit procedure used to maximise the likelihood function This function is the probability distribution function of time residuals defined as the difference between theoretical and measured arrival times of the hits on the PMTs. The following cuts have been applied in order to keep only events that are suitable for the analysis. Data - Montecarlo comparison The Montecarlo (MC) sample of events used in this analysis is performed with the MUPAGE [7] package which simulates the propagation of the muons produced after the interaction of cosmic rays in the atmosphere It is a run-by-run simulation: using the measured optical background rates, optical modules conditions and run duration, a realistic simulation of the physics and data taking process for each run is obtained. In the analysis method used in this work, the MC distributions are not used to correct real data but the two samples are treated separately and compared at the end of the analysis
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