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One of the most powerful cosmological datasets when it comes to constrainingneutrino masses is represented by galaxy power spectrum measurements,$P_{gg}(k)$. The constraining power of $P_{gg}(k)$ is however severely limitedby uncertainties in the modeling of the scale-dependent galaxy bias $b(k)$. Inthis Letter we present a new method to constrain $b(k)$ by using thecross-correlation between the Cosmic Microwave Background (CMB) lensing signaland galaxy maps ($C_\ell^{\rm \kappa g}$) using a simple but theoreticallywell-motivated parametrization for $b(k)$. We apply the method using$C_\ell^{\rm \kappa g}$ measured by cross-correlating Planck lensing maps andthe Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 11 (DR11) CMASSgalaxy sample, and $P_{gg}(k)$ measured from the BOSS DR12 CMASS sample. Wedetect a non-zero scale-dependence at moderate significance, which suggeststhat a proper modeling of $b(k)$ is necessary in order to reduce the impact ofnon-linearities and minimize the corresponding systematics. The accomplishedincrease in constraining power of $P_{gg}(k)$ is demonstrated by determining a95% C.L. upper bound on the sum of the three active neutrino masses $M_{\nu}$of $M_{\nu}<0.19\, {\rm eV}$. This limit represents a significant improvementover previous bounds with comparable datasets. Our method will prove especiallypowerful and important as future large-scale structure surveys will overlapmore significantly with the CMB lensing kernel providing a largecross-correlation signal.

Scale-dependent galaxy bias, CMB lensing-galaxy cross-correlation, and neutrino masses