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-c04-5<br />
<strong>4.</strong>2 Comparison to observations<br />
The easiest test to make, is to compare <strong>the</strong> density<br />
pr<strong>of</strong>iles <strong>of</strong> clusters to those <strong>of</strong> <strong>the</strong> simulations (<strong>the</strong><br />
NFW pr<strong>of</strong>iles, and variants).<br />
Below <strong>we</strong> show <strong>the</strong> comparison <strong>of</strong> mass pr<strong>of</strong>iles derived<br />
from X-ray data to those <strong>of</strong> NFW pr<strong>of</strong>iles:<br />
It is remarkable how good <strong>the</strong> fit is, and <strong>the</strong> concentration<br />
index is <strong>we</strong>ll within <strong>the</strong> limits expected for <strong>the</strong><br />
clusters.<br />
Ano<strong>the</strong>r (simpler) way to do this, is by looking at <strong>the</strong><br />
distribution <strong>of</strong> <strong>the</strong> galaxies within <strong>the</strong> clusters. Again,<br />
a good fit is found:<br />
6-4-10see http://www.strw.leidenuniv.nl/˜ franx/college/galaxies10 10-c04-6
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