2009/08/05 by Ruslan Gabbasov, R. F. Gabbasov, P. Repetto +1 · 1 citation
Chemistry · Mathematics · Physics and Astronomy · #Adaptive optics and wavefront sensing #Additive white Gaussian noise #Algorithm #Artificial intelligence #Astronomy and Astrophysical Research #Astrophysics #Bar (unit) #Chemistry #Computer science #Galaxies: Formation, Evolution, Phenomena #Galaxy #Gaussian #Gaussian noise #Image (mathematics) #Mathematics #Noise (video) #Physics #Robustness (evolution) #Spiral galaxy #Statistics #White noise #astro-ph.GA
paper · pdf · doi:10.1088/0004-637x/702/1/392
published as 2009 ApJ 702, 392 · Accepted for publication in ApJ. 16 pages, 16 figures
arxiv created 2009/08/05 · openalex publication_date 2009/08/12 · arxiv updated 2010/08/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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 −1 kpc −1 for this galaxy.