I've populated the ghsmc_800 simulation (8003 particles,
480Mpc/h, σ8=0.74, Ωm=0.236,
ΩΛ=0.764, n=0.95) with output from the
new version of Galform, using the models of Cole et al. (2000), Baugh
et al. (2005) and Bower et al. (2006), and with output from the old
version of Galform, using the models of Cole et al. (2000), Cole et
al. (2000) with a higher baryon fraction, and 'Model M'. The plots
below compare the clustering in these models and the clustering of the
dark matter to clustering from the SDSS and 2dFGRS.
The projected correlation function (actually rpwp(rp)) for samples with a space density ng/(h3 Mpc-3) of 0.00117, 0.00308 (the fiducial space density from Harker, Cole & Jenkins 2007) and 0.01015:
Old Galform | New Galform |
---|---|
0.00117 | 0.00117 |
0.00308 | 0.00308 |
0.01015 | 0.01015 |
rξ(r) for samples with the following space density:
Old Galform | New Galform |
---|---|
0.00117 | 0.00117 |
0.00249 | 0.00249 |