Abstract
We discuss two aspects of the core–cusp problem in spiral galaxies. The first is observational. In deriving rotation curves from HI data cubes it is essential to take into account projection effects,non-circular motions due to bars and other deviations from axisymmetry, and the effect of pressure gradients on the gas rotation velocity. While these effects may be individually small in themselves, the combined effect is significant as we demonstrate from our analysis of the galaxy NGC 6822. The second issue concerns the effect of gas flows on the survival of density cusps. Winds created by multiple supernova explosions selectively remove low angular momentum baryons from the center of galaxies. Recent simulations show that supernova winds acting throughout the history of a dwarf galaxy can substantially reduce the baryonic and dark matter density in the centers of dwarf galaxies.
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Acknowledgments
G.R. acknowledges support from the NSF AST-04-07072 grant to the University of Nevada, Las Vegas. The research presented here is the result of collaborations with O. Valenzuela, A. Klypin, F. Governato, C. Brook, L. Mayer, A. Brooks, J. Wadsley, P. Jonsson, B. Willman, G. Stinson, T. Quinn, and P. Madau. We are grateful to E. Brinks for help with the data and to E. de Blok for making the data available to us.
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Rhee, G. (2010). Behind the Mask: Resolving the Core–Cusp Problem in Spiral Galaxies. In: Block, D., Freeman, K., Puerari, I. (eds) Galaxies and their Masks. Springer, New York, NY. https://doi.org/10.1007/978-1-4419-7317-7_32
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DOI: https://doi.org/10.1007/978-1-4419-7317-7_32
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