Maximum feedback and dark matter profiles of dwarf galaxies

Authors

  • Oleg Y. Gnedin,

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    • †Present address: Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA.

  • HongSheng Zhao

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    • ‡Visiting Professor at the Institute of Theoretical Astrophysics, National Astronomical Observatory, Beijing 100012, China.


ognedin@stsci.eduOYG

hsz@ast.cam.ac.ukHSZ

Abstract

The observed rotation curves of dark matter-dominated dwarf galaxies indicate low-density cores, contrary to the predictions of CDM models. A possible solution of this problem involves stellar feedback. A strong baryonic wind driven by vigorous star formation can remove a large fraction of the gas, causing the dark matter to expand. Using both numerical and analytical techniques, we explore the maximum effect of the feedback with an instantaneous removal of the gaseous disc. The energy input depends on the compactness of the disc, hence the specific angular momentum of the disc. For the plausible cosmological parameters and a wide range of the disc angular momenta, the feedback is insufficient to destroy the central halo cusp, while the inner density is lowered only by a modest factor of 2 to 6. Any realistic modelling of the feedback would have even lesser impact on dark matter. We find that no star formation effect can resolve the problems of CDM cusps.

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