2009ApJ...702..392G

An important dynamic parameter of barred galaxies is the bar pattern speed, Ω_P. Among several methods that are used for the determination of Ω_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 Ω_ P_. We found that a signal to noise ratio in surface density ∼5 introduces errors of ∼20% for the Gaussian noise, while for the white noise the corresponding errors reach ∼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 Hα Fabry-Pérot interferometry data. We found Ω_P= 43±6 km/s/kpc for this galaxy.