Abstract
We discuss the calibration scheme and the resulting acceptance of the Guane Array (GA) of Water Cherenkov Detectors (WCD). This array is part of the Latin American Giant Observatory (LAGO) project, having singles and small arrays particle detectors, covering a huge range of geomagnetic rigidity cutoffs and atmospheric absorption/reaction levels. GA is compose of three WCDs placed at the vertices of an equilateral triangle (∼ 105 meters), at Bucaramanga, Colombia, (N 7° 8' 40.1959'', W 73° 7' 30'', 956 m a.s.l.). It is designed to study the flux of Cosmic Rays between ∼ 10 GeV to ∼ 106 GeV and their modulation by Space Weather phenomena. GA is thought to operate in two modes simultaneously: Single Particle Mode and Cascade Mode. The calibration of GA is based on two steps: The first step is based on Geant4 simulations, to estimate the response of each WCD to the background radiation and the second step is related to the response in coincidence as an array, through simulations of secondary particle flux and their modulation using CORSIKA and MAGNETOCOSMICS codes. As a result of these calibration steps we have characterized the response of each WCD in terms of the Vertical Equivalent Muon -Energy deposited by a Muon entering at the top and exiting from the bottom of the detector- and estimate the response of the GA for different background fluctuations.
