Observation of the Anisotropy of 10 TeV Primary Cosmic Ray Nuclei Flux with the Super-Kamiokande-I Detector release_fih6djuza5g6tot562nflwrq7a

Abstract

The relative sidereal variation in the arrival direction of primary cosmic ray nuclei of median energy 10 TeV was measured using downward, through-going muons detected with the Super-Kamiokande-I detector. The projection of the anisotropy map onto the right ascension axis has a first harmonic amplitude of (6.64 ± 0.98 stat.± 0.55 syst.) × 10^-4 and a phase at maximum at (33.2^∘± 8.2^∘stat.± 5.1^∘syst.) right ascension. A sky map in equatorial coordinates indicates an excess region in the constellation of Taurus and a deficit region toward Virgo. The excess region is centered at (α_T, δ_T) = (75^∘± 7^∘, -5^∘± 9^∘) with a half opening angle χ_T = (39 ± 7)^∘; the excess flux is (0.104 ± 0.020) parameters for the deficit region are (α_V, δ_V) = (205^∘± 7^∘, 5^∘± 10^∘), χ_V = (54 ± 7)^∘, and (-0.094 ± 0.014) anisotropy (allowed at 13 excess and deficit cones described above. We explored the implications under the assumption that the true anisotropy is not distorted too much by the analysis filter so that it is well-described by the observed excess and deficit cones.
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