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tokens: et al. 2011 ), was required to have an overall completeness (the fraction of spectroscopic targets that were observed) over 70 per cent and a redshift completeness (the fraction of observed galaxies with good spectra) over 80 per cent. We use these galaxies to construct an overdensity map , where i denotes the pixel on the sky. n i = ∑ j ∈ pixel i w j , where w j is the systematic weight (Anderson et al. 2014 ) of galaxy j . The map is given a healp ix pixelization with N side = 1024. Note that we do not weigh the pixels by their observed area because the healp ix pixels are much smaller than the observed sectors for which the completeness is computed, and we did not want to introduce extra power due to possible errors in the completeness on small scales. We also confirm (see Section 7 ) that including pixel weights have only a small effect on the final result. 4 ANGULAR POWER SPECTRA 4.1 Theory We model the theoretical galaxy-CMB lensing convergence angular cross-power spectrum and the galaxy clustering angular auto-power spectrum using standard methods. We assume ΛCDM with parameters consistent with Planck 2013 (Planck Collaboration XVI et al. 2014a ) and BOSS Data Release 11 (Anderson et al. 2014 ). We use these models to estimate statistical errors from mocks and systematic corrections to E G (see Section 5 ). However, our measurement of E G along with errors from jackknife resampling, which we use in our final result, does not use our power spectrum models and is independent of ΛCDM. In addition, the corrections we determine from these models are well within statistical error bars. Using the Limber approximation for small scales (l ≳ 10) and assuming the ΛCDM model, the galaxy-CMB lensing convergence angular cross-power spectrum can be written as where f g ( z ) is the galaxy redshift distribution, W ( z ) = χ(1 − χ( z )/χ CMB ) is the CMB lensing kernel, χ( z ) (χ CMB ) is the comoving distance out to redshift z (the CMB surface-of-last-scattering redshift z CMB = 1100), and P mg ( k, z ) is the matter–galaxy 3D cross-power spectrum as a function of z and wavenumber k (Hirata et al. 2004 ). The cosmological parameters present are the Hubble parameter today H 0 and the current matter density parameter Ω m, 0 . The galaxy redshift distribution for CMASS is shown in fig. 1 of Anderson et al. ( 2014 ). The galaxy clustering angular auto-power spectrum can be written as where H ( z ) is the Hubble parameter at redshift z and P gg ( k, z ) is the galaxy 3D auto-power spectrum. Figure 1. An equatorial map of the CMASS survey divided into 37 regions used for jackknife resampling. 4.2 Mock galaxy catalogues from <italic>N</italic>-body simulations We compute the power spectra P mg ( k, z ) and P gg ( k, z ) using N -body simulations in order to model both non-linearities and the occupation of haloes with galaxies. The N -body simulation runs using the TreePM method (Bagla 2002 ; White, Hernquist Springel 2002 ; Reid et al. 2014 ). We use 10