Constraints on Cosmology and Baryonic Feedback with the Deep Lens Survey
  Using Galaxy-Galaxy and Galaxy-Mass Power Spectra
  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 bins
centered at $z\sim0.27$ and $0.54$ and galaxy-mass power spectra by
cross-correlating the positions of galaxies in these two lens bins with galaxy
shapes in two source bins centered at $z\sim0.64$ and $1.1$. We marginalize
over a baryonic feedback process using a single-parameter representation and a
sum of neutrino masses, as well as photometric redshift and shear calibration
systematic 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 good
agreement with our previous DLS cosmic shear and the Planck Cosmic Microwave
Background (CMB) measurements. Without the baryonic feedback marginalization,
$S_8$ decreases by $\sim0.05$ because the dark matter-only power spectrum lacks
the suppression at the highest $\ell$'s due to Active Galactic Nuclei (AGN)
feedback. Together with the Planck CMB measurement, we constrain the baryonic
feedback parameter to $A_{baryon}=1.07^{+0.31}_{-0.39}$, which suggests an
interesting possibility that the actual AGN feedback might be stronger than the
recipe used in the OWLS simulations. The interpretation is limited by the
validity of the baryonic feedback simulation and the one-parameter
representation of the effect.
