In this paper we investigate the statistical properties of the BaryonicTully-Fisher relation (BTFr) for a sample of 32 galaxies with accuratedistances based on Cepheids and/or TRGB stars. We make use of homogeneouslyanalysed photometry in 18 bands ranging from the FUV to 160 \mu m, allowing usto investigate the effect of the inferred stellar mass-to-light ratio\Upsilon$_{*}$ on the statistical properties of the BTFr. Stellar masses of oursample galaxies are derived with four different methods based on fullSED-fitting, studies of stellar dynamics, near-infrared colours, and theassumption of the same \Upsilon$_{*}^{[3.6]}$ for all galaxies. In addition, weuse high-quality, resolved HI kinematics to study the BTFr based on threekinematic measures: $W_{50}^{i}$ from the global HI profile, and $V_{max}$ and$V_{flat}$ from the rotation curve. We find the intrinsic perpendicularscatter, or tightness, of our BTFr to be $\sigma_{\perp} = 0.026 \pm 0.013$dex, consistent with the intrinsic tightness of the 3.6 \mu m luminosity-basedTFr. However, we find the slope of the BTFr to be $2.99 \pm 0.2$ instead of$3.7 \pm 0.1$ for the luminosity-based TFr at 3.6 \mu m. We use our BTFr toplace important observational constraints on theoretical models of galaxyformation and evolution by making comparisons with theoretical predictionsbased on either the \Lambda CDM framework or modified Newtonian dynamics.

Selecting disk galaxies from the cosmological, hydrodynamical simulationMagneticum Pathfinder we show that almost half of our poster child diskgalaxies at $z=2$ show significantly declining rotation curves and low darkmatter fractions, very similar to recently reported observations. Thesegalaxies do not show any anomalous behavior, reside in standard dark matterhalos and typically grow significantly in mass until $z=0$, where they span allmorphological classes, including disk galaxies matching present day rotationcurves and observed dark matter fractions. Our findings demonstrate thatdeclining rotation curves and low dark matter fractions in rotation dominatedgalaxies at $z=2$ appear naturally within the $\Lambda$CDM paradigm and reflectthe complex baryonic physics, which plays a role at the peak epoch ofstar-formation. In addition, we find that dispersion dominated galaxies at$z=2$, which host a significant gas disk, exhibit similar shaped rotationcurves as the disk galaxy population, rendering it difficult to differentiatebetween these two populations with currently available observation techniques.

We present the results of a Chandra X-ray observation of the massive relicgalaxy Mrk 1216, a present day red nugget. Compact massive galaxies with$r_{\rm e} \lesssim 2$ kpc and $M_{\star}\gtrsim10^{11} M_{\odot}$ observed at$z>2$, also called red nuggets, formed in quick dissipative events and latergrew by a series of dry mergers into the local giant ellipticals. Due to thestochastic nature of mergers, a few of the primordial massive galaxies avoidedthe mergers and remained untouched over cosmic time. Here we report the firstdetection of an X-ray emitting atmosphere surrounding such a relic galaxy. Thehot atmosphere extends far beyond the stellar population and has an 0.5-7 keVX-ray luminosity of $L_{\rm X}=(6.9\pm0.9)\times10^{41}$ erg s$^{-1}$, which issimilar to typical giant ellipticals. The hot gas has a short cooling time of$\sim45$ Myr and the galaxy has a $\sim13$ Gyr old stellar population. Thepresence of an X-ray atmosphere with a short nominal cooling time and the lackof young stars indicate the presence of a sustained heating source, whichprevented star formation since the dissipative origin of the galaxy 13 Gyrsago. The central temperature peak and the presence of radio emission in thecore of the galaxy indicate that the heating source is radio-mechanical AGNfeedback. The presence of hot atmospheres around massive galaxies in the earlyuniverse has important consequences for studies of galaxy quenching andmaintenance mode feedback.

(X/peanut)-shaped features observed in a significant fraction of diskgalaxies are thought to have formed from vertically buckled bars. Despite beingthree dimensional structures, they are preferentially detected in near edge-onprojection. Only a few galaxies are found to have displayed such structureswhen their disks are relatively face-on - suggesting that either they aregenerally weak in face-on projection or many may be hidden by the light oftheir galaxy's face-on disk. Here we report on three (collisionless) simulated galaxies displayingpeanut-shaped structures when their disks are seen both face-on and edge-on -resembling a three-dimensional peanut or dumbbell. Furthermore, thesestructures are accompanied by ansae and an outer ring at the end of the bar ---as seen in real galaxies such as IC~5240. The same set of quantitative parameters used to measure peanut structures inreal galaxies have been determined for the simulated galaxies, and a broadagreement is found. In addition, the peanut length grows in tandem with thebar, and is a maximum at half the length of the bar. Beyond the cutoff of thesepeanut structures, towards the end of the bar, we discover a newpositive/negative feature in the $B_6$ radial profile associated with theisophotes of the ansae/ring. Our simulated, self-gravitating, three-dimensional peanut structures displaycylindrical rotation even in the near-face-on disk projection. In addition, wereport on a kinematic pinch in the velocity map along the bar minor-axis,matching that seen in the surface density map.