Soon the number of type Ia supernovae (SNe) measurements should surpass 10^5. Understanding weaklensing effects in these objects will then be more important than ever. Although SNe lensing is usually seen as a source of systematic noise in this talk I will show how this noise can be in fact turned into signal. I will thus first describe how we were able to accurately model the lensing effects. I will then use these fits to show that the SNe Hubble diagram dispersion is basically modulated by Omega_m0 and sigma_8. I will argue that the modelling of this dispersion allows for an independent measurement also of sigma_8 with supernova data. I will finally show some results using real data.