Stéphane Courteau
Stéphane Courteau
Stéphane Courteau
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Comparison With Models<br />
• Simple exponential disk embedded in a DM halo<br />
• Use density profile for collisionless CDM<br />
simulations of halo formation (NFW)<br />
• Assume adiabatic invariance (Blumenthal etal)<br />
• Use stellar disks of various M/L ratios and<br />
R exp = 3 kpc, and compute the disk-halo<br />
contributions to the rotation curve.<br />
– Get ∂ logV 2.2 / ∂ logR exp for each value of V disk/ V tot<br />
• Test with bulge and isothermal halos
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