We investigate the shape of the Rotation Curves (RCs) of $z\sim 1$star-forming galaxies and compare them with the local star-forming galaxies.For this purpose, we have used $409$ galaxies from the K-band Multi-ObjectSpectrograph (KMOS) for Redshift One Spectroscopic Survey (KROSS). This samplecovers the redshift range $0.57\leq z \leq 1.04$, effective radii $0.69 \leqR_e \left[kpc \right] \leq 7.73$, absolute H-band magnitude $-24.46 \leq M_H\leq -18.85$ with median stellar mass $log\left(M_* \ \left[M_\odot\right]\right)=9.95$ and median total star-formation rate $log\left(SFR_{tot} \\left[M_\odot \ yr^{-1} \right]\right)=1.49$. Using $^{3D}$BAROLO (Barolo), weextract $H\alpha$ kinematic maps and corresponding Rotation Curves (RCs). Themain advantage of Barolo is that it incorporates the beam smearing in the 3Dobservational space, which provide us with the intrinsic rotation velocity evenin the low spatial resolution data. Using Asymmetric Drift Correction (ADC), wehave corrected the RCs for the pressure gradient effect, which seems to be amore dominant effect than beam smearing in high-z galaxies. Nearly all objects($0.1 <v/ \sigma< 15$) are affected by the pressure gradient, and we noticedthat ADC improves the rotation velocity of these systems by $\sim 10-87\%$.Only a combination of the three techniques (3D-kinematic modelling +3D-Beamsmearing correction + ADC ) yields the intrinsic RC of an individualgalaxy. Further, we present the co-added RCs constructed out of 237high-quality objects to obtain intrinsic RC shapes out to 6.4 $\times$ diskscale length. We do not see any change in the shape of RCs with respect to thelocal star-forming disk-type galaxies. In contrast, we do find a significantevolution in the stellar-disk length ($R_D$) of the galaxies. Therefore, weconclude stellar disk evolves over cosmic time while total mass distributionstays constant.

A prediction of the classic active galactic nuclei (AGN) unification model isthe presence of ionisation cones with different orientations depending on theAGN type. Confirmations of this model exist for present times, but it is lessclear in the early Universe. Here, we use the morphology of giant Ly$\alpha$nebulae around AGNs at redshift z$\sim$3 to probe AGN emission and thereforethe validity of the AGN unification model at this redshift. We compare thespatial morphology of 19 nebulae previously found around type I AGNs with a newsample of 4 Ly$\alpha$ nebulae detected around type II AGNs. Using twoindependent techniques, we find that nebulae around type II AGNs are moreasymmetric than around type I, at least at radial distances $r>30$~physical kpc(pkpc) from the ionizing source. We conclude that the type I and type II AGNsin our sample show evidence of different surrounding ionising geometries. Thissuggests that the classical AGN unification model is also valid forhigh-redshift sources. Finally, we discuss how the lack of asymmetry in theinner parts (r$\lesssim$30 pkpc) and the associated high values of the HeII toLy$\alpha$ ratios in these regions could indicate additional sources of (hard)ionizing radiation originating within or in proximity of the AGN host galaxies.This work demonstrates that the morphologies of giant Ly$\alpha$ nebulae can beused to understand and study the geometry of high redshift AGNs oncircum-nuclear scales and it lays the foundation for future studies using muchlarger statistical samples.

We investigate the disc-halo connection in massive (Mstar/Msun>5e10) discgalaxies from the cosmological hydrodynamical simulations EAGLE andIllustrisTNG, and compare it with that inferred from the study of HI rotationcurves in nearby massive spirals from the Spitzer Photometry and AccurateRotation Curves (SPARC) dataset. We find that discrepancies between the thesimulated and observed discs arise both on global and on local scales.Globally, the simulated discs inhabit halos that are a factor ~4 (in EAGLE) and~2 (in IllustrisTNG) more massive than those derived from the rotation curveanalysis of the observed dataset. We also use synthetic rotation curves of thesimulated discs to demonstrate that the recovery of the halo masses fromrotation curves are not systematically biased. We find that the simulationspredict dark-matter dominated systems with stellar-to-total enclosed massratios that are a factor of 1.5-2 smaller than real galaxies at all radii. Thisis an alternative manifestation of the `failed feedback problem', since itindicates that simulated halos hosting massive discs have been too inefficientat converting their baryons into stars, possibly due to an overly efficientstellar and/or AGN feedback implementation.

We present interferometric HI observations of six double-disc stellarcounterrotator ("2$\sigma$") galaxies from the Atlas3D sample. Three aredetected in HI emission; two of these are new detections. NGC 7710 shows amodestly asymmetric HI disc, and the atomic gas in PGC 056772 is centrallypeaked but too poorly resolved to identify the direction of rotation. IC 0719,the most instructive system in this study, shows an extended, strongly warpeddisc of 43 kpc diameter, with a faint tail extending towards its neighbor IC0718. The gas has likely been accreted from this external source during anencounter whose geometry directed the gas into misaligned retrograde orbits(with respect to the primary stellar body of IC 0719). In the interior, wheredynamical time-scales are shorter, the HI has settled into the equatorial planeforming the retrograde secondary stellar disc. This is the first directevidence that a double-disc stellar counterrotator could be formed through theaccretion of retrograde gas. However, the dominant formation pathway for theformation of $2\sigma$ galaxies is still unclear. The Atlas3D sample shows somecases of the retrograde accretion scenario and also some cases in which ascenario based on an unusually well-aligned merger is more likely.