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They could be formed in orbits with a small inclination (with respect to the stellar spin) via disk migration, or in more highly inclined orbits via high-eccentricity migration, where gravitational interactions with a companion and tidal dissipation are at play. Here we target hot Jupiter systems where the misalignment $\\lambda$ has been inferred observationally and we investigate whether their properties are consistent with high-eccentricity migration. 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