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We present cosmological parameter measurements from the Deep Lens Survey(DLS) using galaxy-mass and galaxy-galaxy power spectra in the multipole range$\ell=250\sim2000$. We measure galaxy-galaxy power spectra from two lens binscentered at $z\sim0.27$ and $0.54$ and galaxy-mass power spectra bycross-correlating the positions of galaxies in these two lens bins with galaxyshapes in two source bins centered at $z\sim0.64$ and $1.1$. We marginalizeover a baryonic feedback process using a single-parameter representation and asum of neutrino masses, as well as photometric redshift and shear calibrationsystematic uncertainties. For a flat $\Lambda$CDM cosmology, we determine$S_8\equiv\sigma_8\sqrt{\Omega_m/0.3}=0.810^{+0.039}_{-0.031}$, in goodagreement with our previous DLS cosmic shear and the Planck Cosmic MicrowaveBackground (CMB) measurements. Without the baryonic feedback marginalization,$S_8$ decreases by $\sim0.05$ because the dark matter-only power spectrum lacksthe suppression at the highest $\ell$'s due to Active Galactic Nuclei (AGN)feedback. Together with the Planck CMB measurement, we constrain the baryonicfeedback parameter to $A_{baryon}=1.07^{+0.31}_{-0.39}$, which suggests aninteresting possibility that the actual AGN feedback might be stronger than therecipe used in the OWLS simulations. The interpretation is limited by thevalidity of the baryonic feedback simulation and the one-parameterrepresentation of the effect.

Constraints on Cosmology and Baryonic Feedback with the Deep Lens Survey Using Galaxy-Galaxy and Galaxy-Mass Power Spectra