Absolute calibration and monitoring of a spectrometric channel using a photomultiplier

A new instrument, a camera obscura with a number of light apertures (or slits), is suggested for observation of EAS images in Cerenkov light. Its advantages (over mirror-imaging telescopes) are a low night-sky light noise, a wide field of view and absence of aberrations. This camera is effective for measurements of bright objects such as EAS of energies higher than 103 TeV. Analysis of EAS images in the 'knee' region of the primary cosmic-ray energy spectrum (E0 approximately=3*103 TeV) could give new information on the expected variation of cosmic-ray composition in this energy region.

https://iopscience.iop.org/article/10.1088/0954-3899/20/12/013/pdf

Camera obscura for observation of EAS in Cerenkov light

An Antarctic balloon experiment for measuring the energy spectrum and elemental composition of cosmic rays in the ultrahigh-energy range (1018–1020) eV is proposed. Scientific equipment will measure fluorescence caused by an extensive air shower formed in the atmosphere by an ultrahigh energy particle and Cherenkov light of this shower reflected from a snow surface. It is assumed that the balloon will fly in the circumpolar orbit in Antarctica at a height of ~25 km for (2–3) winter (in the Southern Hemisphere)months. For this time, ~3000 events caused by particles with energies above 1018 eV and (200–300) events caused by particles with energies above 1019 eV will be detected.

Study of the energy spectrum and mass composition of primary cosmic rays in the energy range of 1018–1020 eV using a balloon setup in antarctica (SPHERE-antarctica project)

The status of high energy gamma ray astronomy above 2×1011 eV will be reviewed. In this energy range earth bound detectors can be used. Recently new large area detectors with a significant increase in sensitivity became operational. We compare the performance and the preliminary results from the leading experiments. Also an outlook for the next generation detectors will be given.

High energy gamma astronomy above 200 GeV

The main purpose of the Sphere–Antarctica project is connected to the fundamental problems of the cosmic ray physics and general astrophysics - the determination of the energy and mass composition of cosmic ray particles of ultra high and extremely high energies 1018 − 1020 eV. In the energy region above 6 1019 eV modern experiments (Telescope Array and Pierre Auger Observatory) observed anisotropy and the clustering of arrival directions of cosmic rays in some areas. The scientific importance of this problem stems from the lack of generally accepted acceleration mechanism of the CR particles above 3 1018 eV, the unknown nature of the sources of such particles, the inconsistencies of the results of major experiments in the part of the mass of CR composition and the discrepancy of experimental and model data. Scientific novelty of this project is in the methodology registration of the extensive air showers over a large area ~ 600 km2 from an altitude 30 km, that allows to measure the two optical components of the shower Vavilov–Cherenkov radiation and fluorescence light by the same SiPM sensitive elements of the detector simultaneously.

Detector for the ultrahigh energy cosmic rays composition study in Antarctica

We are presently building an array of angle integrating air Cherenkov counters for the study of VHE and UHE cosmic rays. The new array will be sensitive to extended air showers of energies > 5 × 1013 meV and of zenith angles up to 35°. The determination of the incident shower direction will be performed by fast timing measurements with an angular resolution of 0.5–5 mrad. The Cherenkov counters will allow us to obtain information on the shower energy and structure higher up in the atmosphere. The array will be combined with the existing HEGRA scintillation counter matrix on La Palma. The combination of the Cherenkov data and the data from the ground level scintillator matrix will provide a powerful tool for γ/hadron discrimination. We expect to achieve hadron rejection ratios of > 103 when adding the proposed muon detectors, thereby making possible the detection of the diffuse γ radiation presumed to be coming predominantly from the galactic plane.

A new air Cherenkov counter concept for the observation of extended air showers

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A new air Cherenkov counter concept for the observation of extended air showers