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tokens: pointings (what we will call translational dithering), and with multiple angles due to offsets of the camera rotational angles (what we will call rotational dithering). These aspects of the observing strategy can be used in addition to traditional methods to mitigate WL systematics. Related studies that explore possible translational dithers to determine how the LSST observing strategy can be used to reduce systematic errors in measurements of the LSS have already been conducted (Carroll et al. 2014 ; Awan et al. 2016 ; LSST Science Collaboration et al. 2017 ). In this paper, we study how different aspects of the observing strategy help mitigate the additive shear bias, and rank a set of simulated strategies based on their performance for WL systematics (while the statistical trade-offs are not addressed here). In Section 2 , we explain WL and its systematics in more detail; in Section 3 , we present a representative set of LSST survey strategies and separately the three translational dithering strategies that are studied in this paper, although our method can be easily applied to new observing strategies in the future as they are released. In Section 4 , we present our methodology, using both a direct effect on the cosmic shear bias, and simpler statistical tests of uniformity; and in Section 5 , we analyse the results, and discuss them in the context of the 2018 call 2 for proposals on optimizing the LSST observing strategy for different science cases. 2 BACKGROUND This section includes background information on WL, the observable quantities that are measured and used to constrain cosmological parameters, and the observational systematics that can be affected by different choices in observing strategy. 2.1 WL measurements WL is a ubiquitous statistical effect that modifies the light profiles of galaxies as the light rays from those galaxies pass by other mass along the line of sight before they are observed. WL by the LSS of the universe distorts the shapes and sizes of galaxies according to the distortion matrix: where κ is the convergence, a measure of the magnification due to WL, and γ 1 , γ 2 are spin-2 shear, a measure of the shape distortion due to WL (Bartelmann Schneider 2001 ). The distortion matrix can be used to transform lensed coordinates into unlensed coordinates, such that for unlensed and lensed positions on the sky and , (Mandelbaum et al. 2015 ). The cosmic shear signal can be measured using shear–shear correlation functions between pairs of galaxies, as follows: where t and × are the tangential and cross components of the shear, θ is the angular separation on the sky, φ is the polar angle (Kilbinger 2015 ), refers to the expected value, and R () refers to the real component. We only consider ξ + in our analysis because the biases on ξ − are much closer to 0, and so not much work is needed to mitigate them (Jarvis et al. 2016 ). It is clear from the definition of these correlation functions that any bias in the measured