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Forthcoming large-scale surveys will soon attempt to measure cosmic shear toan unprecedented level of accuracy, requiring a similarly high level ofaccuracy in the shear measurements of galaxies. Factors such as pixelisation,imperfect point-spread function (PSF) correction, and pixel noise can alldirectly or indirectly lead to biases in shear measurements, and so it can benecessary for shear measurement methods to be calibrated against internal,external, or simulated data to minimize bias. It is thus important tounderstand the nature of this calibration. In this paper, we show that atypical calibration procedure will on average leave no residual additive bias,but will leave a residual multiplicative bias. Additionally, the errors on thepost-calibration bias parameters will be changed, and on average increased,from the errors on the pre-calibration measurements of these parameters, butthat this is generally worth the benefit in decreasing the expected value ofthe multiplicative bias. We find that in most typical cases, it is worthwhileto apply a first-order bias correction, while a higher-order bias correction isonly worthwhile for methods with intrinsically high multiplicative bias ($>10$per cent) or when the simulation size is very small ($<10^6$ simulatedgalaxies).

The Effects of Calibration on the Bias of Shear Measurements