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The tumbling pattern of a bar is the main parameter characterising itsdynamics. From numerical simulations, its evolution since bar formation istightly linked to the dark halo in which the bar is formed through dynamicalfriction and angular momentum exchange. Observational measurements of the barpattern speed with redshift can restrict models of galaxy formation and barevolution. We aim to determine, for the first time, the bar pattern speedevolution with redshift based on morphological measurements. We have selected asample of 44 low inclination ringed galaxies from the SDSS and COSMOS surveyscovering the redshift range 0 <z< 0.8 to investigate the evolution of the barpattern speed. We have derived morphological ratios between the deprojectedouter ring radius (R_{ring}) and the bar size (R_{bar}). This quantity isrelated to the parameter {\cal R}=R_{CR}/R_{bar} used for classifiying bars inslow and fast rotators, and allow us to investigate possible differences withredshift. We obtain a similar distribution of $R$ at all redshifts. We do notfind any systematic effect that could be forcing this result. The resultsobtained here are compatible with both, the bulk of the bar population (~70%)being fast-rotators and no evolution of the pattern speed with redshift. Weargue that if bars are long-lasting structures, the results presented hereimply that there has not been a substantial angular momentum exchange betweenthe bar and halo, as predicted by numerical simulations. In consequence, thismight imply that the discs of these high surface-brightness galaxies aremaximal.

Bar pattern speed evolution over the last 7 Gyr