Non-circular (NC) motions represent the imprints of non-axisymmetricstructures in galaxies, providing opportunities to study the physicalproperties of gas departing from circular rotation. In this work, we haveconducted a systematic study of the non-circular motions in a sample of 1624gas-rich disk galaxies from the MaNGA MPL-11. By using the H$\alpha$ velocityas a tracer of the disk rotation, we find indications that the amplitude of thenon-circular motions is related to the stellar mass, with the low mass andlate-type galaxies the most affected. In our sample, we find ratios ofnon-circular to circular rotation ranging from 5% to 20%. By implementingharmonic models to include NC motions associated with spiral arms and stellarbars, we find that the rotational curves traced with H$\alpha$ are barelyaffected by the NC induced by these structures. Consequently, in our sample, wedo not find evidence that NC motions contribute to the scatter of the stellarTully-Fisher relation. Our results suggest that non-circular motions might havea more localized effect in galaxies rather than a global one.

Metallicity measurements in galaxies can give valuable clues about galaxyevolution. One of the mechanisms postulated for metallicity redistribution ingalaxies is gas flows induced by AGN, but the details of this process remainelusive. We report the discovery of a positive radial gradient in the gas-phasemetallicity of the narrow line region of the Seyfert 2 galaxy NGC 7130, whichis not found when considering the star-forming components in the galaxy disk.To determine gas-phase metallicities for each kinematic component, we use bothactive galactic nuclei (AGN) and star-forming (SF) strong-line abundancerelations, as well as BPT diagnostic diagrams. These relations involvesensitive strong emission lines, namely [OIII]5007, [NII]6584, H$\alpha$,H$\beta$, [SII]6716, and [SII]6731, observed with the adaptive-optics-assistedmode of the Multi Unit Spectroscopic Explorer (MUSE) at the Very LargeTelescope (VLT). The presence of a positive radial metallicity gradient only inthe AGN ionized component suggests that metals may be transported from centralareas to its purlieus by AGN activity.

Despite the ubiquity of clumpy star-forming galaxies at high-redshift, theorigin of clumps are still largely unconstrained due to the limitedobservations that can validate the mechanisms for clump formation. We postulatethat if clumps form due to the accretion of metal-poor gas that leads toviolent disk instability, clumpy galaxies should have lower gas-phasemetallicities compared to non-clumpy galaxies. In this work, we obtain thenear-infrared spectrum for 42 clumpy and non-clumpy star-forming galaxies ofsimilar masses, SFRs, and colors at $z\approx0.7$ using the GeminiNear-Infrared Spectrograph (GNIRS) and infer their gas-phase metallicity fromthe {\nii} and {\halpha} line ratio. We find that clumpy galaxies have lowermetallicities compared to non-clumpy galaxies, with an offset in the weightedaverage metallicity of $0.07\pm0.02$ dex. We also find an offset of$0.06\pm0.02$ dex between clumpy and non-clumpy galaxies in a comparable sampleof 23 star-forming galaxies at $z\approx1.5$ using existing data from theFMOS-COSMOS survey. Similarly, lower {\nii}/{\halpha} ratio are typically foundin galaxies that have more of their $\mathrm{UV_{rest}}$ luminosity originatingfrom clumps, suggesting that \enquote{clumpier} galaxies are more metal poor.We also derive the intrinsic velocity dispersion and line-of-sight rotationalvelocity for galaxies from the GNIRS sample. The majority of galaxies have$\sigma_0/v_c \approx 0.2$, with no significant difference between clumpy andnon-clumpy galaxies. Our result indicates that clump formation may be relatedto the inflow of metal-poor gas; however, the process that forms them does notnecessarily require significant, long-term kinematic instability in the disk.

We present ALMA observations on the high-redshift galaxy GHZ2 and report asuccessful detection of the rest-frame 88um atomic transition fromdoubly-ionized Oxygen at z=12.3327+/-0.0005. Based on these observations,combined with additional constraints on the [OIII] 52um line luminosity andprevious JWST data, we argue that GHZ2 is likely powered by compact and youngstar formation, and show that it follows well-established relationships foundfor giant HII regions and metal-poor star-forming dwarf galaxies that are knownto host bright super star clusters. Additionally, these observations providenew constraints on the Oxygen electron density (100 < n_e[cm^-3] < 4,000) anddynamical mass (M_dyn=3-8x10^8M_sun). The existence of these massive starburstsystems 13.3Gyr ago might explain the origin of today's globular clusters, along-standing question in astronomy. To test this, we present observationalprobes to investigate whether sources like GHZ2 are linked to the formation oftoday's globular clusters or other more massive compact stellar systems.