We have used the capability of the MUSE instrument to explore the impact ofstellar feedback at large scales in Haro 11, a galaxy under extreme starburstcondition and one of the first galaxies where Lyman continuum (LyC) has beendetected. Using Ha, [OIII] and [OI] emission lines from deep MUSE observations,we have constructed a sequence of velocity-dependent maps of the Ha emission,the state of the ionised gas and a tracer of fast shocks. These allowed us toinvestigate the ionisation structure of the galaxy in 50 kms^2 bins over avelocity range of -400 to 350 kms. The ionised gas in Haro 11 is assembled by arich arrangement of structures, such as superbubbles, filaments, arcs andgalactic ionised channels, whose appearances change drastically with velocity.The central star forming knots and the star forming dusty arm are the mainengines that power the strong mechanical feedback in this galaxy, although withdifferent impact on the ionisation structure. Haro 11 appears to leak LyCradiation in many directions. We found evidence of a kpc-scale fragmentedsuperbubble, that may have cleared galactic-scale channels in the ISM.Additionally, the southwestern hemisphere is highly ionised in all velocities,hinting at a density bound scenario. A compact kpc-scale structure of lowlyionised gas coincides with the diffuse Lya emission and the presence of fastshocks. Finally, we find evidence that a significant fraction of the ionisedgas mass may escape the gravitational potential of the galaxy.

We present the first spatially resolved analysis of rest-frame optical and UVimaging and spectroscopy for a lensed galaxy at z = 2.39 hosting a Seyfertactive galactic nucleus (AGN). Proximity to a natural guide star has enabledhigh signal-to-noise VLT SINFONI + adaptive optics observations of rest-frameoptical diagnostic emission lines, which exhibit an underlying broad componentwith FWHM ~ 700 km/s in both the Balmer and forbidden lines. Measured lineratios place the outflow robustly in the region of the ionization diagnosticdiagrams associated with AGN. This unique opportunity - combining gravitationallensing, AO guiding, redshift, and AGN activity - allows for a magnified viewof two main tracers of the physical conditions and structure of theinterstellar medium in a star-forming galaxy hosting a weak AGN at cosmic noon.By analyzing the spatial extent and morphology of the Ly-alpha anddust-corrected H-alpha emission, disentangling the effects of star formationand AGN ionization on each tracer, and comparing the AGN induced mass outflowrate to the host star formation rate, we find that the AGN does notsignificantly impact the star formation within its host galaxy.

We report high spatial resolution (~0.076", 410pc) ALMA imaging of the dustcontinuum and the ionised carbon line [CII] in a luminous quasar host galaxy atz=6.6, 800 million years after the Big Bang. Based on previous studies, thisgalaxy hosts a ~1x10^9 M_sun black hole and has a star-formation rate of ~1500M_sun/yr. The unprecedented high resolution of the observations reveals acomplex morphology of gas within 3kpc of the accreting central black hole. Thegas has a high velocity dispersion with little ordered motion along theline-of-sight, as would be expected from gas accretion that has yet to settlein a disk. In addition, we find the presence of [CII] cavities in the gasdistribution (with diameters of ~0.5kpc), offset from the central black hole.This unique distribution and kinematics cannot be explained by a simple model.Plausible scenarios are that the gas is located in a truncated or warped disk,or the holes are created by interactions with nearby galaxies or due to energyinjection into the gas. In the latter case, the energy required to form thecavities must originate from the central active galactic nucleus, as therequired energy far exceeds the energy output expected from supernovae. Thisenergy input into the gas, however, does not inhibit the high rate ofstar-formation. Both star-formation and black-hole activity could have beentriggered by interactions with satellite galaxies: our data reveal threeadditional companions detected in [CII] emission around the quasar.

(Abridged) We explore the massive cluster XMMXCSJ2215.9-1738 at z~1.5 withKMOS spectroscopy of Halpha and [NII] covering a region that corresponds toabout one virial radius. Using published spectroscopic redshifts of 108galaxies in and around the cluster we computed the location of galaxies in theprojected velocity vs. position phase-space to separate our cluster sample intoa virialized region of objects accreted longer ago (roughly inside half R200)and a region of infalling galaxies. We measured oxygen abundances for tencluster galaxies with detected [NII] lines in the individual galaxy spectra andcompared the MZR of the galaxies inside half R200 with the infalling galaxiesand a field sample at similar redshifts. We find that the oxygen abundances ofindividual z~1.5 star-forming cluster galaxies inside half R200 are comparable,at the respective stellar mass, to the higher local SDSS metallicity values.The metallicities of these galaxies in the inner part of the cluster are higherby 0.1-0.2dex, at a given mass, than those of infalling galaxies and of fieldgalaxies at z~1.5. This effect is more pronounced when using the O3N2metallicity calibration compared to the N2 calibration, which can be explainedby the different locations of cluster and field galaxies in the [OIII]/Hbetavs. [NII]/Halpha diagram involving two line ratios compared to one line ratioinformation in the case of the N2 relation. The enhanced metallicities ofcluster galaxies at z~1.5 inside half R200 indicate that the density of the ICMin this massive cluster becomes high enough toward the cluster center such thatthe ram pressure exceeds the restoring pressure of the hot gas reservoir ofcluster galaxies and can remove this gas reservoir initiating quenching,although the galaxies continue to form stars, at slightly lower rates, usingthe available cold gas in the disk which is not stripped.

The stellar initial mass function (IMF) regulates the baryonic cycle withingalaxies, and is a key ingredient to translate observations into physicalquantities. Although for decades it was assumed to be universal, there is nowgrowing observational evidence showing that the center of massive early-typegalaxies host an enhanced population of low-mass stars compared to theexpectations from the Milky Way. Moreover, these variations in the IMF havebeen found to be related to the radial metallicity variations in massivegalaxies. We present here a two-dimensional stellar population analysis of themassive lenticular galaxy FCC 167 (NGC 1380) as part of the Fornax3D project.Using a newly developed stellar population fitting scheme, we derive a fulltwo-dimensional IMF map of an early-type galaxy. This two-dimensional analysisallows us go further than a radial analysis, showing how the metallicitychanges along a disc-like structure while the IMF follows a distinct, lessdisky distribution. Thus, our findings indicate that metallicity cannot be thesole driver of the observed radial IMF variations. In addition, a comparisonwith the orbital decomposition shows suggestive evidence of a coupling betweenstellar population properties and the internal dynamical structure of FCC 167,where metallicity and IMF maps seem to track the distribution of cold and warmorbits, respectively.