The Scientific Baseline to Have an Atmosphere Sounding System Coupled to the EUSO Detector

Details The Scientific Baseline to Have an Atmosphere Sounding System Coupled to the EUSO Detector The Scientific Baseline to Have an Atmosphere Sounding System Coupled to the EUSO Detector

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....2.1101d&link_type=abstract

Proceedings of the 28th International Cosmic Ray Conference. July 31-August 7, 2003. Trukuba, Japan. Under the auspices of the I

Physics

Scientific paper

The atmosphere provides the active target for the detection of the Extreme Energy Cosmic Rays (E E C R) and Neutrinos (E E ν ), as well as for the signals induced by other physical phenomena (lightning, meteors,...), addressed by the E U S O experiment. The detection technique is based on the time and space imaging of the fluorescence, emitted in the UV wavelength range 300÷400 nm and induced, in the atmosphere, by the passage of the secondary ionizing particles which constitute the Extensive Air ˇ Showers. The EASs induced by E E C Rs and E E ν also produce an intense Cerenkov beam, collimated around the shower axis, whose reflection/diffusion can be detected as ˇ well. The transport of both the fluorescence and of the Cerenkov signal is conditioned by the atmospheric conditions. This paper addresses the issue of directly monitoring the conditions of the atmosphere, during the E U S O mission. Introduction The atmosphere is, as seen from E U S O (Extreme Universe Space Observatory" [1,7,8], an active target, whose composition, density and thermo dynamical state determines, for a given shower, the intensity of the detectable signal. The correct reconstruction of the parent EAS longitudinal profile depends on a detailed knowledge of the atmosphere's actual condition and on the capability of deconvolving the distortion intro duced by it. Since the ISS covers the whole Earth surface in the latitude range -51o+51o and moves at a speed of 7 km/sec, the variability of the scene seen by E U S O is much higher than that observed by a ground-based experiment. On the other hand, the large distance from which E U S O looks at the Earth(>˜ 400km) with respect to the thinness of the atmosphere layer where the shower develops (>˜40 km) turns out into a large advantage, together with the almost vertical direction of the line of sight(E U S O field of view F oV , ±30o around the vertical). The former feature has, as a consequence, that the proximity effect is in fact rather small (all the different segments of the shower lie approximately at the same distance (±10 %) from the detection optics, the latter ensures that the traversed depth of the

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