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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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