ON THE BAR PATTERN SPEED DETERMINATION OF NGC 3367

An important dynamic parameter of barred galaxies is the bar pattern speed, {omega} {sub P}. Among several methods that are used for the determination of {omega} {sub P}, the Tremaine-Weinberg method has the advantage of model independence and accuracy. In this work, we apply the method to a simulated bar including gas dynamics and study the effect of two-dimensional spectroscopy data quality on robustness of the method. We added white noise and a Gaussian random field to the data and measured the corresponding errors in {omega} {sub P}. We found that a signal to noise ratio in surface density {approx}5 introduces errors of {approx}20% for the Gaussian noise, while for the white noise the corresponding errors reach {approx}50%. At the same time, the velocity field is less sensitive to contamination. On the basis of the performed study, we applied the method to the NGC 3367 spiral galaxy using H{alpha} Fabry-Perot interferometry data. We found {omega} {sub P} = 43 {+-} 6 km s{sup -1} kpc{sup -1} for this galaxy.