The pattern speed of the bar in NGC 936

We have used the Tremaine-Weinberg method to measure the angular speed of rotation for the bar in the SB0 galaxy NGC 936. With this technique, the bar's pattern speed, Ω_p, can be derived from the luminosity and stellar-kinematic information in long-slit spectral observations taken parallel to the major axis of the galaxy. The kinematic measurement required is the mean line-of-sight velocity of all stellar light entering the slit. This quantity can only be calculated reliably if any asymmetry in the shape of the broadening function of the spectral lines is also measured, and so we present a method which allows for such asymmetry. The technique also returns a true measure of the rms uncertainty in the estimate. Application of the analysis to a set of long-slit spectra of NGC936 returns four separate measures of Ω_p which are mutually consistent. Combination of these data produces a best estimate for the bar pattern speed of $$\Omega_p = 60\pm14\text {km s}^{-1}\text {kpc}^{-1}$$ (assuming a distance of 16.6 Mpc). This result refines the only previous attempt to make this measurement, which yielded an estimate for Ω_p in NGC936 of $$104\pm37\text {km s}^{-1} \text {kpc}^{-1}$$. The new measurement places the co-rotation radius just beyond the end of the bar, in agreement with theoretical calculations