ASTR 610 Theory of Galaxy Formation Lecture 16
ASTR 610 Theory of Galaxy Formation Lecture 16
ASTR 610 Theory of Galaxy Formation Lecture 16
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Three Succesful Models with Scatter<br />
Source: Dutton, vdBosch, Dekel & Courteau, 2007, ApJ, 654, 27<br />
Model ν η Δ IMF<br />
I 0.8 0.8 -0.4<br />
II 1.0 0.5 -0.2<br />
III 0.0 0.8 -0.2<br />
AC parameter<br />
c(M) parameter<br />
All three models match slopes, zero-points and scatter <strong>of</strong> the observed TF and RL<br />
relations. However, the scatter in the observed RL relation requires σ ln λ ≤ 0.25<br />
σ ln λ 0.5<br />
For comparison, simulations predict that<br />
; Hence, disk galaxies may only<br />
form in a subset <strong>of</strong> all haloes, preferably those with smaller spin parameter (which<br />
are the ones that experienced a more quiescent formation history)...<br />
<strong>ASTR</strong> <strong>610</strong>: <strong>Theory</strong> <strong>of</strong> <strong>Galaxy</strong> <strong>Formation</strong> © Frank van den Bosch: Yale 2012
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