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We have investigated, using both a theoretical and an empirical approach, thefrequency of low redshift galaxy-galaxy lensing systems in which the signatureof weak lensing might be directly detectable. We find good agreement betweenthese two approaches. In order to make a theoretical estimate of the weaklensing shear, $\gamma$, for each galaxy in a catalogue, we have made anestimate of the asymptotic circular velocity from the stellar mass using threedifferent approaches: from a simulation based relation, from anempirically-derived relation, and using the baryonic Tully-Fisher relation.Using data from the Galaxy and Mass Assembly redshift survey we estimate thefrequency of detectable weak lensing at low redshift. We find that to aredshift of $z\sim 0.6$, the probability of a galaxy being weakly lensed by atleast $\gamma = 0.02$ is $\sim 0.01$. A scatter in the $M_*-M_h$ relationresults in a shift towards higher measured shears for a given population ofgalaxies. Given this, and the good probability of weak lensing at lowredshifts, we have investigated the feasibility of measuring the scatter in the$M_*-M_h$ relation using shear statistics. This is a novel measurement, and ismade possible because DSM is able to make individual \itshape direct~\upshapeshear measurements, in contrast to traditional weak lensing techniques whichcan only make statistical measurements. We estimate that for a shearmeasurement error of $\Delta\gamma = 0.02$ (consistent with the sensitivity ofDSM), a sample of $\sim$50,000 spatially and spectrally resolved galaxies wouldallow a measurement of the scatter in the $M_*-M_h$ relation to be made. Whilethere are no currently existing IFU surveys of this size, there are upcomingsurveys which will provide this data (e.g The Hobby-Eberly Telescope DarkEnergy Experiment (HETDEX), surveys with Hector, and the Square Kilometre Array(SKA)).

Direct Shear Mapping: Prospects for weak lensing studies of individual galaxy-galaxy lensing systems