AGN outflows can remove large quantities of gas from their host galaxyspheroids, potentially shutting off star formation. On the other hand, they cancompress this gas, potentially enhancing or triggering star formation, at leastfor short periods. We present a set of idealised simulations of AGN outflowsaffecting turbulent gas spheres, and investigate the effect of the outflow andthe AGN radiation field upon gas fragmentation. We show that AGN outflows ofsufficient luminosity shut off fragmentation while the nucleus is active, butgas compression results in a burst of fragmentation after the AGN switches off.Self-shielding of gas against the AGN radiation field allows some fragmentationto occur during outbursts, but too much shielding results in a lower overallfragmentation rate. For our idealised simulation setup, there is a critical AGNluminosity which results in the highest fragmentation rate, with outflows beingtoo efficient at removing gas when $L > L_{\rm crit}$ and not efficient enoughto compress the gas to high densities otherwise. These results, althoughpreliminary, suggest that the interaction between AGN and star formation intheir host galaxies is particularly complex and requires careful study in orderto interpret observations correctly.

We have discovered large amounts of molecular gas, as traced by CO emission,in the ram pressure stripped gas tail of the Coma cluster galaxy D100 (GMP2910), out to large distances of about 50 kpc. D100 has a 60 kpc long,strikingly narrow tail which is bright in X-rays and H{\alpha}. Ourobservations with the IRAM 30m telescope reveal in total ~ 10^9 M_sun of H_2(assuming the standard CO-to-H_2 conversion) in several regions along the tail,thus indicating that molecular gas may dominate its mass. Along the tail wemeasure a smooth gradient in the radial velocity of the CO emission that isoffset to lower values from the more diffuse H{\alpha} gas velocities. Such adynamic separation of phases may be due to their differential acceleration byram pressure. D100 is likely being stripped at a high orbital velocity >2200km/s by (nearly) peak ram pressure. Combined effects of ICM viscosity andmagnetic fields may be important for the evolution of the stripped ISM. Wepropose D100 has reached a continuous mode of stripping of dense gas remainingin its nuclear region. D100 is the second known case of an abundant molecularstripped-gas tail, suggesting that conditions in the ICM at the centers ofgalaxy clusters may be favorable for molecularization. From comparison withother galaxies, we find there is a good correlation between the CO flux and theH{\alpha} surface brightness in ram pressure stripped gas tails, over about 2dex.

We derive two-dimensional dust attenuation maps at $\sim1~\mathrm{kpc}$resolution from the UV continuum for 10 galaxies on the $z\sim2$ Star-FormingMain Sequence (SFMS). Comparison with IR data shows that 9 out of 10 galaxieshave no further obscuration in addition to the UV-based correction. Theindividual rest-frame $V$-band dust attenuation (A$_{\rm V}$) radial profilesscatter around an average profile that gently decreases from $\sim1.8$ mag inthe center down to $\sim0.6$ mag at $\sim3-4$ half-mass radii. We use theseA$_{\rm V}$ maps to correct UV- and H$\alpha$-based star-formation rates(SFRs), which agree with each other. At masses $\leq10^{11}~M_{\odot}$, thespecific SFR (sSFR) profiles are on average radially constant at amass-doubling timescale of $\sim300~\mathrm{Myr}$, pointing at a synchronousgrowth of bulge and disk components in such galaxies. At masses$\geq10^{11}~M_{\odot}$, the dust-corrected sSFR profiles are typicallycentrally-suppressed by a factor of $\sim10$ relative to the galaxy outskirts.With total central obscuration disfavored, this indicates that at least afraction of massive $z\sim2$ SFMS galaxies have started inside-out theirstar-formation quenching that will move them to the quenched sequence; thisalso highlights the key role of progenitor bias effects in the observedevolution of the quenched population. Galaxies above and below the ridge of theSFMS relation have respectively centrally-enhanced and centrally-suppressedsSFRs relative to their outskirts, supporting a picture where bulges are builtdue to gas `compaction' that leads to a high central SFR as galaxies movetowards the upper envelope of SFMS.

We examine the kinematic morphology of early-type galaxies (ETGs) in eightgalaxy clusters in the Sydney-AAO Multi-object Integral field spectrograph(SAMI) Galaxy Survey. The clusters cover a mass range of14.2<log(M_200/M_odot)<15.2 and we measure spatially-resolved stellarkinematics for 315 member galaxies with stellar masses10.0<log(M_*/M_odot)<11.7 within 1R_200 of the cluster centers. We calculatethe spin parameter, lambda_R and use that to classify the kinematic morphologyof the galaxies as fast or slow rotators. The total fraction of slow rotatorsin the early-type galaxy population, F_SR=0.14+/-0.02 and does not depend onhost cluster mass. Across the eight clusters, the fraction of slow rotatorsincreases with increasing local overdensity. We also find that the slow-rotatorfraction increases at small clustercentric radii (R_cl<0.3R_200), and note thatthere is also an increase in slow-rotator fraction at R_cl~0.6R_200. The slowrotators at these larger radii reside in cluster substructure. We find thestrongest increase in slow-rotator fraction occurs with increasing stellarmass. After accounting for the strong correlation with stellar mass, we find nosignificant relationship between spin parameter and local overdensity in thecluster environment. We conclude that the primary driver for the kinematicmorphology--density relationship in galaxy clusters is the changingdistribution of galaxy stellar mass with local environment. The presence ofslow rotators in substructure suggests that the cluster kinematicmorphology--density relationship is a result of mass segregation ofslow-rotating galaxies forming in groups that later merge with clusters andsink to the cluster center via dynamical friction.