The HEAT instrument has detected cosmic-ray electrons and positrons in two balloon ights, at energies between 1 and 50 GeV. The combined data set indicates that the positron fraction does not increase with energy above 10 GeV. However, our results suggest a slight overabundance of positrons at all energies compared with published predictions from secondary production sources, and possibly the h...

The Fermi Large Area Telescope has provided the measurement of the high energy (20 GeV to 1 TeV) cosmic ray electrons and positrons spectrum with unprecedented accuracy. This measurement represents a unique probe for studying the origin and diffusive propagation of cosmic rays as well as for looking for possible evidences of Dark Matter. In this contribution we focus mainly on astrophysical sou...

We employ the Monte Carlo particle collision code DPMJET3.04 to determine the multiplicity spectra of various secondary particles (in addition to π 0 's) with γ's as the final decay state, that are produced in cosmic-ray (p's and α's) interactions with the interstellar medium. We derive an easy-to-use γ-ray production matrix for cosmic rays with energies up to about 10 PeV. This γ-ray productio...

Recently different experiments mention to have observed a large scale cosmic-ray anisotropy at TeV energies, e.g. Milagro, Tibet and SuperKamiokande. For these energies the cosmic-rays are expected to be nearly isotropic. Any measurements of cosmic-rays anisotropy could bring some information about propagation and origin of cosmic-rays. Though the primary aim of the ANTARES neutrino telescope i...

BLANCA is a new, large non-imaging Cerenkov detector located at the CASA-MIA experiment it Dugway, Utah. Using 144 individual Cerenkov detectors, BLANCA covers an area of approximately 0.2 km and has an energy threshold of 300 TeV. The lateral density function (LDF) of the Cerenkov light in air showers is measured. Since the LDF depends on the primary particle species, a change in composition a...

A high significance observation of two muon signals, the shadow of the sun and moon, have been seen by the 5.4 kt MINOS Far Detector, at a depth of 2070 mwe. The distribution of angular separation of muons near the moon was well described by a Gaussian, which was used to determine the angular resolution (0.34◦ ± 0.07◦) and pointing (0.3◦ ± 0.05◦) of the detector. Introduction & Motivation The M...

After a short review of the ultrahigh energy cosmic ray puzzle – the apparent observation of cosmic rays originating from cosmological distances with energies above the expected Greisen-Zatsepin-Kuzmin cutoff 4 × 10 19 eV – we consider strongly interacting neutrino scenarios as an especially interesting solution. We show that all features of the ultrahigh energy cosmic ray spectrum from 10 17 e...

The GALPROP cosmic-ray (CR) propagation model has been extended to three dimensions including the effects of stochastic SNR sources, a comprehensive cross-section database, and nuclear reaction networks. A brief description of the new code is given and some illustrative results for the distribution of CR protons presented. Results for electrons and γ-rays are given in an accompanying paper.