1 INTRODUCTION
2 GENERAL METHODOLOGY FOR GALAXY GALAXY LENSING
2.1 From $\gamma$ to ∆Σ
2.2 Correction terms due to imperfect knowledge of source redshifts
3 METHODOLOGY
3.1 General approach and limitations
3.2 Computation of $\Delta\Sigma$
3.3 Blinding strategy
3.4 Aspects of tests agreed to before analysis
3.5 Amplitude fitting
3.6 Searching for trends caused by correlated systematic errors
3.7 Estimate of global systematic error
3.8 Effective redshift weighting of lens samples
4 FOREGROUND LENS DATA
4.1 BOSS survey
4.2 Lens samples
5 WEAK LENSING DATA
5.1 SDSS
5.2 HSC
5.3 CS82
5.4 CFHTLenS
5.5 KiDS
5.6 DES
6 COMPUTATION OF $\Delta\Sigma$
6.1 Computation of $\Delta\Sigma$ and notation
6.2 SDSS
6.3 HSC
6.4 CS82
6.5 CFHTLenS
6.6 KiDS
6.7 DES
7 HOMOGENEITY OF BOSS SAMPLES
7.1 Overall homogeneity
7.2 Galactic hemisphere
7.3 Stellar density and seeing
8 RESULTS
8.1 Comparison of $\Delta\Sigma$ and computation of amplitudes
8.2 Effective lens redshift
8.3 Tests related to homogeneity of lens samples
8.4 Scaling of amplitudes with mean source redshift
8.5 Trends including systematic errors
8.6 Empirical estimates of the systematic error
8.7 Comparison with statistical error
9 DISCUSSION
9.1 Amplitude of $\Delta\Sigma$ versus source redshift
9.2 On the possibility of underestimated statistical errors
9.3 Considerations for future implementations of these tests
9.4 Connection with cosmic shear
9.5 Implication for the “Lensing is Low” effect
10 SUMMARY AND CONCLUSIONS