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Description
The Latin American Giant Observatory (LAGO) is composed by a network of water Cherenkov detectors installed in the Andean region at various latitudes, from Sierra Negra in M\'exico 18$^{\circ}$ 59' N to the Antarctic Peninsula 64$^{\circ}$ 14'S 56$^{\circ}$ 38' O and altitudes from Lima, Peru at 20 m a.s.l. to Chacaltaya, Bolivia at 5400 m a s.l. The detectors of the network are built on the basis of commercial water tanks, so they have several geometries (cylindrical in general) and different methods of water purification. LAGO's network of detectors also spans over a wide range of geomagnetic rigidity cut offs and atmospheric absorption depths. This, together with its manufacturing differences, generates different structures in the atmospheric radiation spectra measured by our detectors.
One of the main scientific goals of LAGO is to measure the temporal evolution of the flow of secondary particles at ground. This atmospheric flux is produced by the interaction of cosmic rays with the atmosphere at different sites to study the solar modulation of galactic cosmic rays. So, to integrate, monitor and share the data of the detectors, a web monitor is being developed, which is based on a novel semi-analytical method that combines simulations of the total cosmic ray spectrum and the detectors response to estimate the signals left by secondary particles at the detector.
In the present work we give details of the detector calibration method, applied on four detectors of the network and including the one operated in the Base Machu Picchu, ($62^{\circ} 05'S 58^{\circ} 28'O$) during the last Peruvian scientific campaign to Antarctica (January 2018). We also review some candidates for Forbush decrease measured in the detectors under this calibration and present the functionalities of the web monitor.
