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Using data from the Pantheon SN Ia compilation and the Sloan Digital SkySurvey (SDSS), we propose an estimator for weak lensing convergenceincorporating positional and photometric data of foreground galaxies. Thecorrelation between this and the Hubble diagram residuals of the supernovae has$3.6\sigma$ significance, and is consistent with weak lensing magnification dueto dark matter halos centered on galaxies. We additionally constrain theproperties of the galactic haloes, such as the mass-to-light ratio $\Gamma$ andradial profile of the halo matter density $\rho(r)$. We derive a newrelationship for the additional r.m.s. scatter in magnitudes caused by lensing,finding $\sigma_{\rm lens} = (0.06 \pm 0.017) (d_{\rm C}(z)/ d_{\rmC}(z=1))^{3/2}$ where $d_{\rm C}(z)$ is the comoving distance to redshift $z$.Hence the scatter in apparent magnitudes due lensing will be of the same sizeas the intrinsic scatter of SN Ia by $z \sim 1.2$. We propose a modification ofthe distance modulus estimator for SN Ia to incorporate lensing, which can beeasily calculated from observational data. We anticipate this will improve theaccuracy of cosmological parameter estimation for high-redshift SN Ia data.

Weak lensing magnification of Type Ia Supernovae from the Pantheon sample