the kickoff in Brazil. In 2011, MinCyT ranked LLAMA as its astronomical project and in 2012, FAPESP approved a €7 M grant. The final agreement, between MinCyT, FAPESP and Universidade de São Paulo (USP), was signed in June 2014, and on July 9, it was formally presented to the public. Measurements of the electrical characteristics of the site were carried out in late 2016, and construction of the road to the summit began in December 2016. Assembly of the antenna is planned to take place in 2022, with testing beginning in 2023. Origin of the name The observatory acronym comes from the Quechuan word llama that designates the South American camelid that lives in the region where the telescope is being installed. There is some confusion with the word array, since LLAMA will consist of a single dish antenna, but the instrument will have VLBI technology and can therefore be part of an antenna array with telescopes of other observatories. Moreover, the LLAMA observatory can be expanded in the future by installing other antennas in different sites. In different official documents the acronym LLAMA may be found expanded as Long Latin American Millimeter Array rather than Large. It is also possible to read Millimetric instead of Millimeter. After some debate, the LLAMA Executive Committee stated that Large Latin American Millimeter Array is the right expansion for the LLAMA acronym. The observatory logo has as symbols the Southern Cross (upper right), a telescope sketch (bottom right), the acronym (upper left) and a llama profile (bottom left). Although it changed with time, these symbols are present since the beginning. The image illustrating this page is the official logo since August 2014. Science LLAMA is a multipurpose instrument, with the capacity to both observe bright sources like the Sun, and very weak sources very far from Earth. The following is a list of different subjects that will be addressed with LLAMA observations. The Sun In the unperturbed solar atmosphere, the shorter the wavelength the deeper the observation. Frequencies near the submillimeter range are produced in the lower chromosphere or the photosphere. Therefore, LLAMA observations will bring new information about the structure of the lower Solar Atmosphere, the active and quiescent filaments and the dynamics of the chromosphere and its magnetic field. The possibility to observe Solar Flares at high frequencies with a high sensitive instrument will give clues about the acceleration of the