Summary
We give a brief description of a new model for non-circular motions in disk galaxy velocity fields, that does not invoke epicycles. We assume non-circular motions to stem from a bar-like or oval distortion to the potential, as could arise from a triaxial halo or a bar in the mass distribution of the baryons. We apply our model to the high-quality CO and Hα kinematics of NGC 2976 presented by [5]; it fits the data as well as their model with unrealistic radial flows, but yields a steeper rotation curve. Our analysis and other evidence suggests that NGC 2976 hosts a bar, implying a large baryonic contribution to the potential and thus limiting the allowed dark matter halo density.
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© 2008 Springer Science+Business Media B.V.
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Spekkens, K., Sellwood, J. (2008). Modeling Non-Circular Motions in Disk Galaxies: A Bar in NGC 2976. In: Jerjen, H., Koribalski, B. (eds) Galaxies in the Local Volume. Astrophysics and Space Science Proceedings. Springer, Dordrecht. https://doi.org/10.1007/978-1-4020-6933-8_35
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DOI: https://doi.org/10.1007/978-1-4020-6933-8_35
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