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HERD is the High Energy cosmic-Radiation Detection instrument proposed to operate onboard Chinas space station in the 2020s. It is designed to detect energetic cosmic ray nuclei, leptons and photons with a high energy resolution ($sim1%$ for electrons and photons and $20%$ for nuclei) and a large geometry factor ($>3,{ m^2,sr}$ for electrons and diffuse photons and $>2,{ m^2,sr}$ for nuclei). In this work we discuss the capability of HERD to detect monochromatic $gamma$-ray lines, based on simulations of the detector performance. It is shown that HERD will be one of the most sensitive instruments for monochromatic $gamma$-ray searches at energies between $sim10$ to a few hundred GeV. Above hundreds of GeV, Cherenkov telescopes will be more sensitive due to their large effective area. As a specific example, we show that a good portion of the parameter space of a supersymmetric dark matter model can be probed with HERD.
Many theoretical works have predicted the existence of very high energy ($rm VHE:>100 GeV$) $gamma$-ray emission from Gamma-Ray Bursts (GRBs) in both the prompt and the afterglow phases. Observation of such high energy emission, especially in the pro
In August 2015, the CALorimetric Electron Telescope (CALET), designed for long exposure observations of high energy cosmic rays, docked with the International Space Station (ISS) and shortly thereafter began tocollect data. CALET will measure the cos
Results will be shown from the ASTRONEU array developed and operated in the outskirts of Patras, Greece. An array of 9 scintillator detectors and 3 antennas were deployed to study Extensive Air Showers (EAS) as a tool for calibrating an underwater ne
The energetic pulsar PSR B1706-44 and the adjacent supernova remnant (SNR) candidate G 343.1-2.3 were observed by H.E.S.S. during a dedicated observational campaign in 2007. A new source of very-high-energy (VHE; E > 100 GeV) gamma-ray emission, HESS
We measure the energy emitted by extensive air showers in the form of radio emission in the frequency range from 30 to 80 MHz. Exploiting the accurate energy scale of the Pierre Auger Observatory, we obtain a radiation energy of 15.8 pm 0.7 (stat) pm