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In addition to the intrinsic clustering of galaxies themselves, the spatialdistribution of galaxies observed in surveys is modulated by the presence ofweak lensing due to matter in the foreground. This effect, known asmagnification bias, is a significant contaminant to analyses of galaxy-lensingcross-correlations and must be carefully modelled. We present a method toestimate the magnification bias in spectroscopically confirmed galaxy samplesbased on finite differences of galaxy catalogues while marginalizing overerrors due to finite step size. We use our estimator to measure themagnification biases of the CMASS and LOWZ samples in the SDSS BOSS galaxysurvey, analytically taking into account the dependence on galaxy shape forfiber and PSF magnitudes, finding $\alpha_{\rm CMASS} = 2.71 \pm 0.02$ and$\alpha_{\rm LOWZ} = 2.45 \pm 0.02$ and quantify modelling uncertainties inthese measurements. Finally, we quantify the redshift evolution of themagnification bias within the CMASS and LOWZ samples, finding a difference ofup to a factor of three between the lower and upper redshift bounds for theformer. We discuss how to account for this evolution in modelling and itsinteraction with commonly applied redshift-dependent weights. Our method shouldbe readily-applicable to upcoming surveys and we make our code publiclyavailable as part of this work.

Magnification Bias Estimators for Realistic Surveys: an Application to the BOSS Survey