Left side: the sensitivity of the SHMR to the assumed value of ﹩{\sigma }_{\mathrm{log}M* }﹩. The solid curves show the SHMR for each value of scatter indicated in the key. The dashed curves show the mean ﹩{M}_{\mathrm{halo}}﹩ in bins of ﹩{M}_{* }﹩. This figure explains why the bias in Figure 8, ﹩b({M}_{* })﹩, decreases as the scatter increases. Right side: comparison of the SHMR derived here to other measurements in the literature. There are few measurements at z = 0.5, so we show values at z = 0 and z = 1 from the same works, with the expectation that the z = 0.5 value should lie somewhere in between. Estimates of the SHMR from abundance matching, such as Behroozi et al. (2013a) and Moster et al. (2013), lie significantly below the relation here. Values derived from cluster samples appear to be in much better agreement with BOSS. Lastly, we are in good agreement with the results of Rodríguez-Torres et al. (2016), who also analyze the CMASS sample but using a different stellar mass estimate and abundance matching technique.