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Table 1.

Summary of the differences between the SCHOol (FC17) and the COllege simulations.

SCHOol (FC17) COllege (this work)
Input distributions Input quantities (size, morphology etc.) correspond to the lensfit priors and a power law magnitude distribution Input quantities are taken from Griffith et al. (2012) based on HST ACS observations
Analytical models Bulge+Disc models, with scalelengths coupled Sérsic models
Object detection SEXTRACTOR is run on one rotation and the same detection catalogue is used in all four rotations SEXTRACTOR is run on all rotations and corresponding detection catalogues are used
Correlations Ellipticity is uncorrelated with size, magnitude, morphology, etc. The dependence between ellipticity, size, morphology, etc., is automatically included by using the measurements from Griffith et al. (2012) on HST data
Coaddition SWARP is run with pixel resampling turned off SWARP is run with pixel resampling turned on
Depth: Extends to 29th magnitude Relatively shallow and somewhat incomplete beyond the detection limit
Sample variance The input catalogue changes for each shear and PSF realisation The input galaxy catalogue is identical for all shear and PSF realisations
Clustering Galaxies are placed randomly on the sky Galaxies are placed at their true locations
Intrinsic alignment Galaxies have random orientation Observed complex ellipticities from Griffith et al. (2012) are used
Redshifts No explicit redshift information for galaxies A nine-band photo-z is assigned to every simulated galaxy based on matching to the KiDS observations of the COSMOS field
Weight bias correction Separately calculated for each shear and each rotation Calculated for a combined catalogue for every PSF set

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