Search for Large-Scale Cosmic-Ray Anisotropy with the First Detection Units of KM3NeT/ARCA

AbstraktAbstract

Although KM3NeT/ARCA was primarily built to detect high-energy neutrinos from astrophysical sources, it also provides a valuable opportunity to study cosmic rays in the TeV to PeV energy range. This is made possible by the detection of down-going atmospheric muons produced in cosmic-ray air showers, the same particles that usually represent background in neutrino searches. In this study, we focus on identifying large-scale anisotropies in the arrival directions of these cosmic rays, using data from ARCA’s first detection units. To separate true anisotropies signals from instrumental effects, the East-West method, which correctly removes the count variations not associated with real anisotropies, has been applied. The distribution of event counts in 20-minute sidereal time bin is analyzed to search for a dipole component. The amplitude of the first harmonic shows a significance of 1.7 σ, hence, an upper limit on the dipole amplitude at 2.0 × 10−3 is set at 99% confidence level. The corresponding phase of the dipole is found to be −40◦ ± 26◦.

Although KM3NeT/ARCA was primarily built to detect high-energy neutrinos from astrophysical sources, it also provides a valuable opportunity to study cosmic rays in the TeV to PeV energy range. This is made possible by the detection of down-going atmospheric muons produced in cosmic-ray air showers, the same particles that usually represent background in neutrino searches. In this study, we focus on identifying large-scale anisotropies in the arrival directions of these cosmic rays, using data from ARCA’s first detection units. To separate true anisotropies signals from instrumental effects, the East-West method, which correctly removes the count variations not associated with real anisotropies, has been applied. The distribution of event counts in 20-minute sidereal time bin is analyzed to search for a dipole component. The amplitude of the first harmonic shows a significance of 1.7 σ, hence, an upper limit on the dipole amplitude at 2.0 × 10−3 is set at 99% confidence level. The corresponding phase of the dipole is found to be −40◦ ± 26◦.