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We examine the importance of baryonic feedback effects on the matter powerspectrum on small scales, and the implications for the precise measurement ofneutrino masses through gravitational weak lensing. Planned large galaxysurveys such as the Large Synoptic Sky Telescope (LSST) and Euclid are expectedto measure the sum of neutrino masses to extremely high precision, sufficientto detect non-zero neutrino masses even in the minimal mass normal hierarchy.We show that weak lensing of galaxies while being a very good probe of neutrinomasses, is extremely sensitive to baryonic feedback processes. We use publiclyavailable results from the Overwhelmingly Large Simulations (OWLS) project toinvestigate the effects of active galactic nuclei feedback, the nature of thestellar initial mass function, and gas cooling rates, on the measured weaklensing shear power spectrum. Using the Fisher matrix formalism and priors fromCMB+BAO data, we show that when one does not account for feedback, the measuredneutrino mass may be substantially larger or smaller than the true mass,depending on the dominant feedback mechanism, with the mass error |\Delta m_nu|often exceeding the mass m_nu itself. We also consider gravitational lensing ofthe cosmic microwave background (CMB) and show that it is not sensitive tobaryonic feedback on scales l < 2000, although CMB experiments that aim forsensitivities sigma(m_nu) < 0.02 eV will need to include baryonic effects inmodeling the CMB lensing potential. A combination of CMB lensing and galaxylensing can help break the degeneracy between neutrino masses and baryonicfeedback processes. We conclude that future large galaxy lensing surveys suchas LSST and Euclid can only measure neutrino masses accurately if the matterpower spectrum can be measured to similar accuracy.

Systematic errors in the measurement of neutrino masses due to baryonic feedback processes: Prospects for stage IV lensing surveys