Measurement of the Cosmic Ray Energy Spectrum above 4TeV Using Two Cherenkov Telescopes at YBJ in Tibet
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Two air shower Cherenkov telescopes, as prototype detector of a wide field of view (FOV) Cerenkov/fluorescence telescope array (WFCA), are operated at the ARGO-YBJ experiment site in Tibet. Using the Cherenkov signal in the shower images recorded by the Cherenkov telescopes and shower geometry measured by the ARGO-YBJ detector, shower energy can be reconstructed. With the help of such Coincident events an absolute calibration of the energy scale for the ground based experiment will be established by comparing with the balloon borne experimental results.Keywords:
Air shower
Cherenkov detector
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Gamma-Ray Astronomy
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The Large High Altitude Air Shower Observatory project is proposed to study high energy gamma ray astronomy ( 40 GeV-1 PeV ) and cosmic ray physics ( 20 TeV-1 EeV ). The wide field of view Cherenkov telescope array, as a component of the LHAASO project, will be used to study energy spectrum and compositions of cosmic ray by measuring the total Cherenkov light generated by air showers and shower maximum depth. Two prototype telescopes have been in operation since 2008. The pointing accuracy of each telescope is crucial to the direction reconstruction of the primary particles. On the other hand the primary energy reconstruction relies on the shape of the Cherenkov image on the camera and the unrecorded photons due to the imperfect connections between photomultiplier tubes. UV bright stars are used as point-like objects to calibrate the pointing and to study the optical properties of the camera, the spot size and the fractions of unrecorded photons in the insensitive areas of the camera.
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This report presents an cherenkov telescope prototype, observation method of cherenkov light from extensive air showers (EAS) generated by cosmic rays (CRs) above $10^{16}$eV and preliminary observations. The interest in cherenkov light differential detectors of EAS is caused by the possibility to measure the depth of cascade maximum, Xmax, and/or the shower age via angular and temporal distributions of the cherenkov signal. In particular, it was shown using EAS model simulations that the pulse width measured at the periphery of the shower, r > 300 m, at sea level is pronouncedly connected with Xmax. cherenkov detector is a wide-angle telescope working in coincidence with scintillation detectors, integral and differential cherenkov detectors Yakutsk complex EAS.
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Telescopes, designed with semi-conductor based photo sensors, have the potential to detect Cherenkov or fluorescence light emitted by cosmic-rays in the atmosphere.Such telescopes promise a high duty cycle and efficiency in remote harsh environments.Given the relatively low costs and robustness of these instruments, this technology could prove interesting especially if deployed in large numbers with existing and future extended cosmic-ray and gamma ray detectors, including the Pierre Auger observatory, HAWC, IceCube and CTA.They may have the potential to enhance the sensitivity of these instruments for the detection of high-energy gamma rays and cosmic-ray air showers.In addition, for neutrino telescopes such a technology could prove to be an efficient cosmic-ray veto on the surface.In this contribution the current motivation, design, and development of a prototype SiPM based air Cherenkov telescope is described.The results of initial sensitivity studies, and the readiness of the system for first tests, including those proposed for the South Pole are shown.
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The ARGO‐YBJ detector, located in Tibet at 4300 m a.s.l., is a full‐coverage Extensive Air‐Shower Array consisting of a single layer of Resistive Plate Chambers. The main scientific goals of the experiment are the study of cosmic rays and the detection of astrophysical γ radiation at few hundreds GeV energy threshold. About 30% of the foreseen active area is in stable data taking since December 2004. The analysis of first data shows that the detector is working properly and that ARGO‐YBJ has the capability to image extensive air showers with unprecedented granularity and to monitor continuously the Northern Sky searching for steady and transient sources of γ‐rays. In this paper we report some results about the air shower detection and the first sky map covering the declination band −20°< δ <80°.
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