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Abstract

M dwarfs are the most numerous type of stars in the Universe. Their low masses and their large planet-to-star size ratios offer big advantages to study orbiting exoplanets around these stars. On one hand, the radial velocities signals have greater amplitudes and are easier to identify than in FGK stars. On the other, the small size of M dwarfs leads to transiting planets leaving a stronger imprint in the light curve. Additionally, their low temperatures places their habitable zone close to the host star, which makes them excellent targets to search for temperate or habitable worlds. Despite the advantages that M dwarfs offer, these do not come for free. Typically they are active entities, and most of the M-dwarfs have strong magnetic fields, which can heat their stellar chromospheres, creating magnetic activity which drives the occurrence of stellar spots in their photosphere. Consequently, stellar activity can mimic the signal of an orbiting planet which is one of the most problematic sources of noise. This thesis is focused on the discovery and characterization of exoplanets around M dwarfs, where I highlight the importance of careful modeling of the intrinsic stellar noise present in the data for to avoid false planet claims