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The bar pattern speed ($\Omega_{\rm b}$) is defined as the rotationalfrequency of the bar, and it determines the bar dynamics. Several methods havebeen proposed for measuring $\Omega_{\rm b}$. The non-parametric methodproposed by Tremaine \& Weinberg (1984; TW) and based on stellar kinematics isthe most accurate. This method has been applied so far to 17 galaxies, most ofthem SB0 and SBa types. We have applied the TW method to a new sample of 15strong and bright barred galaxies, spanning a wide range of morphological typesfrom SB0 to SBbc. Combining our analysis with previous studies, we investigate32 barred galaxies with their pattern speed measured by the TW method. Theresulting total sample of barred galaxies allows us to study the dependence of$\Omega_{\rm b}$ on galaxy properties, such as the Hubble type. We measured$\Omega_{\rm b}$ using the TW method on the stellar velocity maps provided bythe integral-field spectroscopy data from the CALIFA survey. Integral-fielddata solve the problems that long-slit data present when applying the TWmethod, resulting in the determination of more accurate $\Omega_{\rm b}$. Inaddition, we have also derived the ratio $\cal{R}$ of the corotation radius tothe bar length of the galaxies. According to this parameter, bars can beclassified as fast ($\cal{R}$ $< 1.4$) and slow ($\cal{R}$>1.4). For all thegalaxies, $\cal{R}$ is compatible within the errors with fast bars. We cannotrule out (at 95$\%$ level) the fast bar solution for any galaxy. We have notobserved any significant trend between $\cal{R}$ and the galaxy morphologicaltype. Our results indicate that independent of the Hubble type, bars have beenformed and then evolve as fast rotators. This observational result willconstrain the scenarios of formation and evolution of bars proposed bynumerical simulations.

Bar pattern speeds in CALIFA galaxies: I. Fast bars across the Hubble sequence