Model-based pattern speed estimates for 38 barred galaxies

2008/06/03 by P. Rautiainen, H. Salo, E. Laurikainen · 109 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Barred spiral galaxy #Bulge #Disc #Elliptical galaxy #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy rotation curve #Halo #Lenticular galaxy #Luminous infrared galaxy #Photometry (optics) #Physics #Spiral galaxy #Stars #Stellar, planetary, and galactic studies #astro-ph

paper · pdf · doi:10.1111/j.1365-2966.2008.13522.x

published in Monthly Notices of the Royal Astronomical Society 388(4), 1803-1818 (Oxford University Press) · 18 pages, 13 figures, accepted for publication in MNRAS

arxiv created 2008/06/03 · openalex publication_date 2008/07/14 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06

Abstract

We have modelled 38 barred galaxies by using near-infrared and optical data from the Ohio State University Bright Spiral Galaxy Survey. We constructed the gravitational potentials of the galaxies from H-band photometry, assuming a constant mass-to-light ratio. The halo component we choose corresponds to the so-called universal rotation curve. In each case, we used the response of gaseous and stellar particle disc to rigidly rotating potential to determine the pattern speed. We find that the pattern speed of the bar depends roughly on the morphological type. The average value of corotation resonance radius to bar radius, ⁠, increases from 1.15 ± 0.25 in types SB0/a–SBab to 1.44 ± 0.29 in SBb and 1.82 ± 0.63 in SBbc–SBc. Within the error estimates for the pattern speed and bar radius, all galaxies of type SBab or earlier have a fast bar ⁠, whereas the bars in later type galaxies include both fast and slow rotators. Of 16 later type galaxies with a nominal value of ⁠, there are five cases, where the fast-rotating bar is ruled out by the adopted error estimates. We also study the correlation between the parameter and other galactic properties. The clearest correlation is with the bar size: the slowest bars are also the shortest bars when compared to the galaxy size. A weaker correlation is seen with bar strength in a sense that slow bars tend to be weaker. These correlations leave room for a possibility that the determined pattern speed in many galaxies corresponds to actually that of the spiral, which rotates more slowly than the bar. No clear correlation is seen with either the galaxy luminosity or the colour.

Citations

• The gravitational potential of the bar in NGC 4314
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• Polygonal structures in a gaseous disk: Numerical simulations
• SDSS-IV MaNGA: Bar pattern speed estimates with the Tremaine-Weinberg method and their error sources
• The impact of spiral density waves on the distribution of supernovae
• Stellar mass distribution of S4G disk galaxies and signatures of bar-induced secular evolution
• Gravitational torques imply molecular gas inflow towards the nucleus of M 51
• The dynamical state of bars in cluster dwarf galaxies: The cases of NGC 4483 and NGC 4516