4. Structure of Dark Matter halos Obviously, we cannot observe the ...
4. Structure of Dark Matter halos Obviously, we cannot observe the ...
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<br />
Fits with NFW pr<strong>of</strong>iles are hard. The rise <strong>of</strong> <strong>the</strong> rotation<br />
curve is too slow:<br />
Ho<strong>we</strong>ver, it is possible that o<strong>the</strong>r processes play a role.<br />
For example, rotation may not dominate <strong>the</strong> gas kinematics.<br />
6-4-10see http://www.strw.leidenuniv.nl/˜ franx/college/galaxies10 10-c04-12<br />
• Substructure<br />
The <strong>halos</strong> from simulations look smooth - but are not<br />
as smooth as might be. Many show sub<strong>halos</strong>. An example<br />
is : (e.g., Springel et al. 2008, arxiv 0809.0898)
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