Galaxy Formation, Theory and Modelling. Shaun Cole (ICC, Durham). Collaborators: Geraint Harker John Helly Adrian Jenkins Hannah Parkinson. ICC Photo: Malcolm Crowthers. 25 th October 2007. Outline. An Introduction to the Ingredients of Galaxy Formation Models
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ICC Photo: Malcolm Crowthers
Parkinson, Cole and Helly 2007
Insert an empirically motivated factor into this merger rate equation
Thus we require:
Very nearly consistent with the universal Sheth-Tormen/Jenkins Mass Function
NFW profiles, but with what concentration
Neto et al 2007
Helly et al. (2002)
Galaxy orbits decay due to dynamical friction
Bower et al 2006
Gas cooling rates
DM and Gas density profile
Galaxy merger rates
Dark Matter Merger Trees
Positions and velocities
Star formation rate, ages, metallicities
Structure & Dynamics
Harker, Cole & Jenkins 2007
Particles in 300 Mpc/h box
Two grids of models with
Achieved by rescaling particle masses and velocities (Zheng et al 2002)
-- Grid 1
-- Grid 2
For each (scaled) N-body output we have two variants of each of three distinct GALFORM models.
Low baryon fraction (Cole et al 2000)
Superwinds (Baugh et al 2005 aka M)
AGN-like feedback (C2000hib)
Each model is adjusted to match the
observed r-band LF.
Compare clustering and determine best fit.
Zehavi et al 2005
Clustering strength primarily dependent on
I.E. Galaxy bias predicted by the GALFORM model is largely independent of model details.
The constraint on
from b-band 2dFGRS data
More modelling work required.