We investigate the compact, early-type galaxy NGC 1281 with integral fieldunit observations to map the stellar LOSVD out to 5 effective radii andconstruct orbit-based dynamical models to constrain its dark and luminousmatter content. Under the assumption of mass-follows-light, the H-band stellarmass-to-light ratio (M/L) is {\Upsilon} = 2.7(+-0.1) {\Upsilon}_{sun}, higherthan expected from our stellar population synthesis fits with either acanonical Kroupa ({\Upsilon} = 1.3 {\Upsilon}_{sun}) or Salpeter ({\Upsilon} =1.7 {\Upsilon}_{sun}) stellar initial mass function. Such models also cannotreproduce the details of the LOSVD. Models with a dark halo recover thekinematics well and indicate that NGC 1281 is dark matter dominated, making up~ 90 per cent of the total enclosed mass within the kinematic bounds.Parameterised as a spherical NFW profile, the dark halo mass is 11.5 <log(M_{DM}/M_{sun}) < 11.8 and the stellar M/L is 0.6 < {\Upsilon} < 1.1.However, this stellar M/L is lower than predicted by its old stellarpopulation. Moreover, the halo mass within the kinematic extent is ten timeslarger than expected based on {\Lambda}CDM predictions, and an extrapolationyields cluster sized dark halo masses. Adopting {\Upsilon} = 1.7{\Upsilon}_{sun} yields more moderate dark halo virial masses, but these modelsfit the kinematics worse. A non-NFW model might solve the discrepancy betweenthe unphysical consequences of the best-fitting dynamical models and modelsbased on more reasonable assumptions for the dark halo and stellarmass-to-light ratio, which are disfavoured according to our parameterestimation.

This proceeding overviews our current understanding of the orbital historyand mass of the Large and Small Magellanic Clouds. Specifically I will arguethat the Clouds are on their first infall about our Milky Way and that theirtotal masses are necessarily ~10 times larger than traditionally estimated.This conclusion is based on the recently revised HST proper motions of theClouds and arguments concerning the binary status of the LMC-SMC pair and theirbaryon fractions

Using Blue Horizontal Branch stars identified in the Dark Energy Survey Year1 data, we report the detection of an extended and lumpy stellar debrisdistribution around the Magellanic Clouds. At the heliocentric distance of theClouds, overdensities of BHBs are seen to reach at least to ~30 degrees, andperhaps as far as ~50 degrees from the LMC. In 3D, the stellar halo istraceable to between 25 and 50 kpc from the LMC. We catalogue the mostsignificant of the stellar sub-structures revealed, and announce the discoveryof a number of narrow streams and diffuse debris clouds. Two narrow streamsappear approximately aligned with the Magellanic Clouds' proper motion.Moreover, one of these overlaps with the gaseous Magellanic Stream on the sky.Curiously, two diffuse BHB agglomerations seem coincident with several of therecently discovered DES satellites. Given the enormous size and the conspicuouslumpiness of the LMC's stellar halo, we speculate that the dwarf could easilyhave been more massive than previously had been assumed.

We measure the evolution of the quiescent fraction and quenching efficiencyof satellites around star-forming and quiescent central galaxies with stellarmass $\log(M_{\mathrm{cen}}/M_{\odot})>10.5$ at $0.3<z<2.5$. We combine imagingfrom three deep near-infrared-selected surveys (ZFOURGE/CANDELS, UDS, andUltraVISTA), which allows us to select a stellar-mass complete sample ofsatellites with $\log(M_{\mathrm{sat}}/M_{\odot})>9.3$. Satellites for bothstar-forming and quiescent central galaxies have higher quiescent fractionscompared to field galaxies matched in stellar mass at all redshifts. We alsoobserve "galactic conformity": satellites around quiescent centrals are morelikely to be quenched compared to the satellites around star-forming centrals.In our sample, this conformity signal is significant at $\gtrsim3\sigma$ for$0.6<z<1.6$, whereas it is only weakly significant at $0.3<z<0.6$ and$1.6<z<2.5$. Therefore, conformity (and therefore satellite quenching) has beenpresent for a significant fraction of the age of the universe. The satellitequenching efficiency increases with increasing stellar mass of the central, butdoes not appear to depend on the stellar mass of the satellite to the masslimit of our sample. When we compare the satellite quenching efficiency ofstar-forming centrals with stellar masses 0.2 dex higher than quiescentcentrals (which should account for any difference in halo mass), the conformitysignal decreases, but remains statistically significant at $0.6<z<0.9$. This isevidence that satellite quenching is connected to the star-formation propertiesof the central as well as to the mass of the halo. We discuss physical effectsthat may contribute to galactic conformity, and emphasize that they must allowfor continued star-formation in the central galaxy even as the satellites arequenched.

In recent years, a growing zoo of compact stellar systems (CSSs) have beenfound whose physical properties (mass, size, velocity dispersion) place thembetween classical globular clusters (GCs) and true galaxies, leading to debatesabout their nature. Here we present results using a so far underutiliseddiscriminant, their stellar population properties. Based on new spectroscopyfrom 8-10m telescopes, we derive ages, metallicities, and [\alpha/Fe] of 29CSSs. These range from GCs with sizes of merely a few parsec to compactellipticals larger than M32. Together with a literature compilation, thisprovides a panoramic view of the stellar population characteristics ofearly-type systems. We find that the CSSs are predominantly more metal richthan typical galaxies at the same stellar mass. At high mass, the compactellipticals (cEs) depart from the mass-metallicity relation of massiveearly-type galaxies, which forms a continuous sequence with dwarf galaxies. Atlower mass, the metallicity distribution of ultra-compact dwarfs (UCDs) changesat a few times $10^7$ M$_{\odot}$, which roughly coincides with the mass whereluminosity function arguments previously suggested the GC population ends. Thehighest metallicities in CSSs are paralleled only by those of dwarf galaxynuclei and the central parts of massive early types. These findings can beinterpreted as CSSs previously being more massive and undergoing tidalinteractions to obtain their current mass and compact size. Such aninterpretation is supported by CSSs with direct evidence for tidal stripping,and by an examination of the CSS internal escape velocities.

We report a bimodality in the azimuthal angle ($\Phi$) distribution of gasaround galaxies traced by OVI absorption. We present the mean $\Phi$probability distribution function of 29 HST-imaged OVI absorbing (EW>0.1A) and24~non-absorbing (EW<0.1A) isolated galaxies (0.08<z<0.67) within 200kpc ofbackground quasars. We show that EW is anti-correlated with impact parameterand OVI covering fraction decreases from 80% within 50kpc to 33% at 200kpc. Thepresence of OVI absorption is azimuthally dependent and occurs between$\pm10-20^{\circ}$ of the galaxy projected major axis and within$\pm30^{\circ}$ of the projected minor axis. We find higher EWs along theprojected minor axis with weaker EWs along the project major axis. Highlyinclined galaxies have the lowest covering fractions due to minimizedoutflow/inflow cross-section geometry. Absorbing galaxies also have bluercolors while non-absorbers have redder colors, suggesting that star-formationis a key driver in the OVI detection rate. OVI surrounding blue galaxies existsprimarily along the projected minor axis with wide opening angles while OVIsurrounding red galaxies exists primarily along the projected major axis withsmaller opening angles, which may explain why absorption around red galaxies isless frequently detected. Our results are consistent with CGM originating frommajor axis-fed inflows/recycled gas and from minor axis-driven outflows.Non-detected OVI occurs between $\Phi=20-60^{\circ}$, suggesting that OVI isnot mixed throughout the CGM and remains confined within the outflows and thedisk-plane. We find low OVI covering fractions within $\pm10^{\circ}$ of theprojected major axis, suggesting that cool dense gas resides in a narrow planergeometry surrounded by diffuse OVI gas.

We study the stellar properties of 44 face-on spiral galaxies from the CalarAlto Legacy Integral Field Area survey via full spectrum fitting techniques. Wecompare the age profiles with the surface brightness distribution in order tohighlight differences between profile types (type I, exponential profile; andII, down-bending profile). We observe an upturn ("U-shape") in the age profilesfor 17 out of these 44 galaxies with reliable stellar information up to theirouter parts. This "U-shape" is not a unique feature for type II galaxies butcan be observed in type I as well. These findings suggest that the mechanismsshaping the surface brightness and stellar population distributions are notdirectly coupled. This upturn in age is only observable in the light-weightedprofiles while it flattens out in the mass-weighted profiles. Given recentresults on the outer parts of nearby systems and the results presented in thisLetter, one of the most plausible explanations for the age upturn is an earlyformation of the entire disc ($\sim$~10~Gyr ago) followed by an inside-outquenching of the star formation.