Bars are ellipsoidal-like structures that appears in the inner regions of a large fraction of discs of galaxies. Bars universal features present at all galactic masses, morphological types and across the Hubble time. Stars forming bars follow elongated orbits aligned with the bar major-axis. These barred structures rotate as a coherent structure around the galactic center with a fixed angular frequency called pattern speed. The rotation of the bar have important dynamic implications for the galaxy evolution. In particular, the bar rotation produce important redistributions of the angular momentum, energy and mass in the disc of the galaxies, producing important changes in the galactic structure. Therefore, both morphology and dynamics of the barred galaxies depend on their pattern speed. Measuring the bar pattern speed is the most difficult amongst the observational parameters characterizing bars. Several methods have been used during decades to determine this dynamical parameter of barred galaxies. In this talk we will give a summarize about the different methods used in the literature to determine the bar pattern speed in barred galaxies. In addition, we will summarize the relation between different galaxy properties such as mass, morphology, or size and the measured pattern speeds. We will also compared the observations with state of the art cosmological simulations of barred galaxies.