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We present observations of ionized gas outflows in 11 z = 1.39â€"2.59 radio-loud quasar host galaxies. Data were taken with the integral field spectrograph OSIRIS and the adaptive optics system at the W.M. Keck Observatory targeting nebular emission lines (H β, [O III ], H α, [N II ], and [S II ]) redshifted into the near-infrared (1â€"2.4 ÎĽ m). Outflows with velocities of 500â€"1700 km sâˆ'1 are detected in 10 systems on scales ranging from <1 kpc to 10 kpc with outflow rates from 8â€"2400 M ⊙ yrâˆ'1. For five sources, the outflow momentum rates are 4â€"80 times L AGN/c, consistent with outflows being driven by an energy-conserving shock. The five other outflows are either driven by radiation pressure or an isothermal shock. The outflows are the dominant source of gas depletion, and we find no evidence for star formation along the outflow paths. For eight objects, the outflow paths are consistent with the orientation of the jets. Yet, given the calculated pressures, we find no evidence of the jets currently doing work on these galactic-scale ionized outflows. We find that galactic-scale feedback occurs well before galaxies establish a substantial fraction of their stellar mass, as expected from local scaling relationships. [ABSTRACT FROM AUTHOR]

We present detailed observations of photoionization conditions and galaxy kinematics in 11 z = 1.39–2.59 radio-loud quasar host galaxies. Data were taken with the OSIRIS integral field spectrograph and the adaptive optics system at the W. M. Keck Observatory that targeted nebular emission lines (Hβ, [O iii ], Hα, [N ii ]) redshifted into the near-infrared (1–2.4 μm). We detect extended ionized emission on scales ranging from 1 to 30 kpc photoionized by stars, shocks, and active galactic nuclei (AGN). Spatially resolved emission-line ratios indicate that our systems reside off the star formation and AGN-mixing sequence on the Baldwin, Phillips, & Terlevich diagram at low redshift. The dominant cause of the difference between line ratios of low-redshift galaxies and our sample is due to lower gas-phase metallicities, which are 2–5× less compared to galaxies with AGN in the nearby universe. Using gas velocity dispersion as a proxy to stellar velocity dispersion and dynamical mass measurement through inclined disk modeling, we find that the quasar host galaxies are undermassive relative to their central supermassive black hole mass, with all systems residing off the local scaling (M•–σ, M•–M*) relationship. These quasar host galaxies require substantial growth, up to an order of magnitude in stellar mass, to grow into present-day massive elliptical galaxies. Combining these results with part I of our sample paper, we find evidence for winds capable of causing feedback before the AGN host galaxies land on the local scaling relation between black hole and galaxy stellar mass, and before the enrichment of the interstellar medium to a level observed in local galaxies with AGN. [ABSTRACT FROM AUTHOR]

We present a three-dimensional data cube of the K-band continuum and the Br γ, H2 S(0), and S(1) lines within the central 18.″5 × 13.″8 (520 pc × 390 pc) region of NGC 6946. Data were obtained using OSIRIS, a near-infrared Integral Field Spectrograph at Keck Observatory, with Laser Guide Star Adaptive Optics. The 0.″3 resolution allows us to investigate the stellar bulge and the forming star clusters in the nuclear region on 10 pc scales. We detect giant H II regions associated with massive young star clusters in the nuclear spiral/ring (R ∼ 30 pc) and in the principal shocks along the nuclear bar. Comparisons of the Br γ fluxes with Pa α line emission and radio continuum indicate AK ∼ 3, AV ∼ 25 for the nuclear star-forming regions. The most luminous H II regions are restricted to within 70 pc of the center, despite the presence of high gas columns at larger radii (R ∼ 200 pc). H2 emission is restricted to clouds within R ∼ 60 pc of the center, resembling the distribution of HCN line emission. We propose that gas-assisted migration of the young star clusters is contributing to the buildup of the nuclear bar and nuclear star cluster (R < 30 pc) in this galaxy. [ABSTRACT FROM AUTHOR]

We present stellar kinematics and orbit superposition models for the central regions of four brightest cluster galaxies, based upon integral-field spectroscopy at Gemini, Keck, and McDonald Observatories. Our integral-field data span radii from <100 pc to tens of kiloparsecs, comparable to the effective radius of each galaxy. We report black hole masses, M•, of 2.1+1.6–1.6 × 1010M☼ for NGC 4889, 9.7+3.0–2.5 × 109M☼ for NGC 3842, and 1.3+0.5–0.4 × 109M☼ for NGC 7768, with errors representing 68% confidence limits. For NGC 2832, we report an upper limit of M• < 9.0 × 109M☼. Our models of each galaxy include a dark matter halo, and we have tested the dependence of M• on the model dark matter profile. Stellar orbits near the center of each galaxy are tangentially biased, on comparable spatial scales to the galaxies’ photometric cores. We find possible photometric and kinematic evidence for an eccentric torus of stars in NGC 4889, with a radius of nearly 1 kpc. We compare our measurements of M• to the predicted black hole masses from various fits to the relations between M• and stellar velocity dispersion (σ), luminosity (L), or stellar mass (M⋆). Still, the black holes in NGC 4889 and NGC 3842 are significantly more massive than all σ-based predictions and most L-based predictions. The black hole in NGC 7768 is consistent with a broader range of predictions. [ABSTRACT FROM AUTHOR]