from 28 June 2015 to 3 July 2015 (Africa/Johannesburg)
SAIP2015 Proceeding published on 17 July 2016
Rotation Curves and Bars: Accounting for non-circular motions in barred spiral galaxies
Presented by Mr. Toky RANDRIAMAMPANDRY on 2 Jul 2015 from 16:30 to 16:50
Type: Oral Presentation
Track: Track D1 - Astrophysics
The rotation curves (RCs) of disk galaxies are a tool for studying their mass distribution and the dark matter content. The assumption underlying this type of work is that galaxies are axisymmetric and the rotational velocity of their gas traces the gravitational potential. Unfortunately, this is surely not the case for barred galaxies since the measured velocities depend on both the gravitational potential and the gas' streaming motion along the bar. The so-called “tilted-ring method” is commonly adopted when deriving RCs of galaxies, but it can produce erroneous values for the derived parameters of galaxies with large non-circular motions. There are methods used to correct for the non-circular motion which are based on harmonic decomposition and Fourier analysis of the velocity field. However, these methods do not work when the bar is aligned or perpendicular to the major axis because of degenerate velocity components. Using the case of NGC 3319, we show the importance of properly accounting for these non-circular motions. We use snapshots of N-body/hydrodynamic simulations with similar bar properties to adjust the observed RC of NGC 3319. The mass models of the adjusted RCs vary greatly from those obtained using the observed RC. These lead to wildly different conclusions about the dark matter concentration and domination. These results demonstrate that future studies of barred spiral galaxies must include careful corrections for the non-circular motions.
Prof. Claude Carignan; email@example.com; Department of Astronomy, University of Cape Town