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The Cherenkov Telescope Array (CTA) is the next generation facility ofImaging Atmospheric Cherenkov Telescopes. It will reach unprecedentedsensitivity and energy resolution in very-high-energy gamma-ray astronomy. CTAwill detect Cherenkov light emitted within an atmospheric shower of particlesinitiated by cosmic-gamma rays or cosmic rays entering the Earth's atmosphere.From the combination of images the Cherenkov light produces in the telescopes,one is able to infer the primary particle energy and direction. A correctenergy estimation can be thus performed only if the local atmosphere is wellcharacterized. The atmosphere not only affects the shower development itself,but also the Cherenkov photon transmission from the emission point in theparticle shower, at about 10-20 km above the ground, to the detector. Cherenkovlight on the ground is peaked in the UV-blue region, and therefore molecularand aerosol extinction phenomena are important. The goal of CTA is to controlsystematics in energy reconstruction to better than 10%. For this reason, acareful and continuous monitoring and characterization of the atmosphere isrequired. In addition, CTA will be operated as an observatory, with data madepublic along with appropriate analysis tools. High-level data quality can onlybe ensured if the atmospheric properties are consistently and continuouslytaken into account. In this contribution, we concentrate on discussing theimplementation strategy for the various atmospheric monitoring instrumentscurrently under discussion in CTA. These includes Raman lidars and ceilometers,stellar photometers and others available both from commercial providers andpublic research centres.

Strategy Implementation for the CTA Atmospheric Monitoring Program