4. Structure of Dark Matter halos Obviously, we cannot observe the ...

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6-4-10see http://www.strw.leidenuniv.nl/˜ franx/college/galaxies10 10-c04-11 Fits with NFW profiles are hard. The rise of the rotation curve is too slow: However, it is possible that other processes play a role. For example, rotation may not dominate the gas kinematics. 6-4-10see http://www.strw.leidenuniv.nl/˜ franx/college/galaxies10 10-c04-12 • Substructure The halos from simulations look smooth - but are not as smooth as might be. Many show subhalos. An example is : (e.g., Springel et al. 2008, arxiv 0809.0898)
6-4-10see http://www.strw.leidenuniv.nl/˜ franx/college/galaxies10 10-c04-13 6-4-10see http://www.strw.leidenuniv.nl/˜ franx/college/galaxies10 10-c04-14 The mass fraction in subhalos as a function of radius is given by the following plot
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4. Structure of Dark Matter halos Obviously, we cannot observe the ...

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