For Omega=0.3 Lambda=0.7: In the LCDM03 mocks we used

We assume a mean k+e correction of the form K+E = (z+6.0*z**2)/(1.0+20.0*z**3)

The adopted biasing parameters were alpha=0.45 and beta=-0.18

These parameters are as described the MNRAS paper Norberg etal (2002) "The 2dFGS: Galaxy Luminosity Function and Survey Selection Function"

While in LCDM04 and LCDM04r we made very small tweaks to be consistent with the final 2dFGRS calibration and instead adopted

We assume a mean k+e correction of the form K+E = (z+6.0*z**2)/(1.0+8.9*z**2.5)

The adopted biasing parameters were alpha=0.45 and beta=-0.14

Estimates of the resulting galaxy (ansd masss) power spectra obtained from the full Hubble Volume cube can be found in the following files

These parameters are as described the MNRAS paper Cole etal (2005) "The 2dFGS: Power-spectrum analysis of the final dataset and cosmological implications"

The magnitude limit of all the catalogues is uniform and considerably deeper than that of the 2dFGRS redshift survey essentially as deep as the photometric APM survey. Thus to make mocks of the redshift catalogues one should view these catalogues through the 2dF magnitude limit and redshift completeness masks or ask Shaun.Cole@durham.ac.uk for catalogues that have been processed this way.

For Omega=1.0:

For Omega=0.3 Lambda=0.7:

We assume a mean k+e correction of the form K+E = 0.03*z/(0.01+z^4)

These models both produce 164.5 gals per square degree brighter than the 2dF limit of B_J=19.45. This is in good agreement with the most recently calibrated APM catalogue after dust extinction corrections based on the published SFD dust maps.

The magnitude limit we have taken for the APM and 2dF catalogues is B_J=20.5. IE this is deeper than the 2dF redshift survey and essentially as deep as the photometric APM survey.

We assume a mean k+e correction of the form K+E = -2.5*z .

The magnitude limit we have taken for the 6dF catalogues is B_J=13.5 . IE this is deeper than the planned redshift survey.

ftp://ftp-astro.physics.ox.ac.uk/pub/users/wjs/pscz/psi.f

It is defined by:

c Model of PSCZ selection function r in Mpc/h taken from c ftp://ftp-astro.physics.ox.ac.uk/pub/users/wjs/pscz/psi.f c but boosted in number density by 25% to match actual number c in PSCz redshift catalogue c c r -- distance in units of Mpc/h c real function sel(r) c************************************************************************ implicit none real r,psistar,alpha,alrstar,beta,gamma,eps,alr,del,fudge data psistar,alpha,alrstar,beta,gamma/ & 0.0077115800,1.81726,1.93673,4.42847,1.56137/ data eps/1e-5/ data fudge/1.25188/ c************************************************************************ alr=alog10(max(r,eps)) del = alr-alrstar sel = fudge*psistar * 10**((1-alpha)*del) / & (1 + (10**(gamma*del)))**(beta/gamma) return end

In the catalogue file fluxes in mJ replace the magnitudes used in the other catalogues.