Context. Feedback from accreting supermassive black holes is often identified as the main mechanism responsible for regulating star-formation in AGN host galaxies. However, the relationships between AGN activity, radiation, winds, and star-formation are complex and still far from being understood. Aims. We study scaling relations between AGN properties, host galaxy properties and AGN winds. We then evaluate the wind mean impact on the global star-formation history, taking into account the short AGN duty cycle with respect to that of star-formation. Methods. We first collect AGN wind observations for 94 AGN with detected massive winds at sub-pc to kpc spatial scales. We then fold AGN wind scaling relations with AGN luminosity functions, to evaluate the average AGN wind mass-loading factor as a function of cosmic time. Results. We find strong correlations between the AGN molecular and ionised wind mass outflow rates and the AGN bolometric luminosity. The power law scaling is steeper for ionised winds (slope 1.29±0.38) than for molecular winds (0.76±0.06), meaning that the two rates converge at high bolometric luminosities. The molecular gas depletion timescale and the molecular gas fraction of galaxies hosting powerful AGN driven winds are 3-10 times shorter and smaller than those of main-sequence galaxies with similar star-formation rate, stellar mass and redshift. These findings suggest that, at high AGN bolometric luminosity, the reduced molecular gas fraction may be due to the destruction of molecules by the wind, leading to a larger fraction of gas in the atomic ionised phase. The AGN wind mass-loading factor η =ṀOF /SFR is systematically higher than that of starburst driven winds. Conclusions. Our analysis shows that AGN winds are, on average, powerful enough to clean galaxies from their molecular gas only in massive systems at z < ∼ 2, i.e. a strong form of co-evolution between SMBHs and galaxies appears to break down for the least massive galaxies.

We present a Chandra study of mass profiles in 7 elliptical galaxies, of which 3 have galaxy-scale and 4 group-scale halos, demarcated at 10 13 M ⊙ . These represent the best available data for nearby objects with comparable X-ray luminosities. We measure ∼flat mass-to-light (M/L) profiles within an optical half-light radius (R eff ), rising by an order of magnitude at ∼10R eff , which confirms the presence of dark matter (DM). The data indicate hydrostatic equilibrium, which is also supported by agreement with studies of stellar kinematics in elliptical galaxies. The data are well-fitted by a model comprising an NFW DM profile and a baryonic component following the optical light. The distribution of DM halo concentration parameters (c) versus M vir agrees with ΛCDM predictions and our observations of bright groups. Concentrations are slightly higher than expected, which is most likely a selection effect. Omitting the stellar mass drastically increases c, possibly explaining large concentrations found by some past observers. The stellar M/L K agree with population synthesis models, assuming a Kroupa IMF. Allowing adiabatic compression (AC) of the DM halo by baryons made M/L more discrepant, casting some doubt on AC. Our best-fitting models imply total baryon fractions ∼0.04-0.09, consistent with models of galaxy formation incorporating strong feedback. The groups exhibit positive temperature gradients, consistent with the "Universal" profiles found in other groups and clusters, whereas the galaxies have negative gradients, suggesting a change in the evolutionary history of the systems around M vir ≃ 10 13 M ⊙ .

Mrk 231 is a nearby ultra-luminous IR galaxy exhibiting a kpc-scale, multi-phase AGN-driven outflow. This galaxy represents the best target to investigate in detail the morphology and energetics of powerful outflows, as well as their still poorly-understood expansion mechanism and impact on the host galaxy. In this work, we present the best sensitivity and angular resolution maps of the molecular disk and outflow of Mrk 231, as traced by CO(2−1) and (3−2) observations obtained with the IRAM/PdBI. In addition, we analyze archival deep Chandra and NuSTAR X-ray observations. We use this unprecedented combination of multi-wavelength data sets to constrain the physical properties of both the molecular disk and outflow, the presence of a highly-ionized ultra-fast nuclear wind, and their connection. The molecular CO(2−1) outflow has a size of ∼1 kpc, and extends in all directions around the nucleus, being more prominent along the south-west to north-east direction, suggesting a wide-angle biconical geometry. The maximum projected velocity of the outflow is nearly constant out to ∼1 kpc, thus implying that the density of the outflowing material must decrease from the nucleus outwards as ∼r −2 . This suggests that either a large part of the gas leaves the flow during its expansion or that the bulk of the outflow has not yet reached out to ∼1 kpc, thus implying a limit on its age of ∼1 Myr. Mapping the mass and energy rates of the molecular outflow yieldsṀ OF = [500−1000] M yr −1 andĖ kin,OF = [7−10] × 10 43 erg s −1 . The total kinetic energy of the outflow is E kin,OF is of the same order of the total energy of the molecular disk, E disk . Remarkably, our analysis of the X-ray data reveals a nuclear ultrafast outflow (UFO) with velocity −20 000 km s −1 ,Ṁ UFO = [0.3−2.1] M yr −1 , and momentum loadṖ UFO /Ṗ rad = [0.2−1.6]. We finḋ E kin,UFO ∼Ė kin,OF as predicted for outflows undergoing an energy conserving expansion. This suggests that most of the UFO kinetic energy is transferred to mechanical energy of the kpc-scale outflow, strongly supporting that the energy released during accretion of matter onto super-massive black holes is the ultimate driver of giant massive outflows. The momentum fluxṖ OF derived for the large scale outflows in Mrk 231 enables us to estimate a momentum boostṖ OF /Ṗ UFO ≈ [30−60]. The ratiosĖ kin,UFO /L bol,AGN = [1−5]% anḋ E kin,OF /L bol,AGN = [1−3]% agree with the requirements of the most popular models of AGN feedback.

We present radial mass profiles within $0:3r vir for 16 relaxed galaxy groups-poor clusters (kT range 1Y3 keV ) selected for optimal mass constraints from the Chandra and XMM-Newton data archives. After accounting for the mass of hot gas, the resulting mass profiles are described well by a two-component model consisting of dark matter, represented by an NFW model, and stars from the central galaxy. The stellar component is required only for eight systems, for which reasonable stellar mass-to-light ratios (M/L K ) are obtained, assuming a Kroupa IMF. Modifying the NFW dark matter halo by adiabatic contraction does not improve the fit and yields systematically lower M /L K . In contrast to previous results for massive clusters, we find that the NFW concentration parameter (c vir ) for groups decreases with increasing M vir and is inconsistent with no variation at the 3 level. The normalization and slope of the c vir -M vir relation are consistent with the standard ÃCDM cosmological model with 8 ¼ 0:9 (considering a 10% bias for early forming systems). The small intrinsic scatter measured about the c vir -M vir relation implies that the groups represent preferentially relaxed, early forming systems. The mean gas fraction ( f ¼ 0:05 AE 0:01) of the groups measured within an overdensity Á ¼ 2500 is lower than for hot, massive clusters, but the fractional scatter ( f /f ¼ 0:2) for groups is larger, implying a greater impact of feedback processes on groups, as expected.