We present the results of direct-method metallicity measurements in the diskand outflow of the low-metallicity starburst galaxy NGC 1569. We use KeckCosmic Web Imager observations to map the galaxy across 54$\arcsec$ (800 pc)along the major axis and 48$\arcsec$ (700 pc) along the minor axis with aspatial resolution of 1$\arcsec$ ($\sim$15 pc). We detect common strongemission lines ([\ion{O}{III}] $\lambda$5007, H$\beta$, [\ion{O}{II}]$\lambda$3727) and the fainter [\ion{O}{III}] $\lambda$4363 auroral line, whichallows us to measure electron temperature ($T_e$) and metallicity. Theorysuggests that outflows drive metals out of the disk driving observed trendsbetween stellar mass and gas-phase metallicity. Our main result is that themetallicity in the outflow is similar to that of the disk, $Z_{\rm out} /Z_{\rm ISM} \approx 1$. This is consistent with previous absorption linestudies in higher mass galaxies. Assumption of a mass-loading factor of$\dot{M}_{\rm out}/{\rm SFR}\sim3$ makes the metal-loading of NGC 1569consistent with expectations derived from the mass-metallicity relationship.Our high spatial resolution metallicity maps reveal a region around asupermassive star cluster (SSC-B) with distinctly higher metallicity and higherelectron density, compared to the disk. Given the known properties of SSC-B thehigher metallicity and density of this region are likely the result of starformation-driven feedback acting on the local scale. Overall, our results areconsistent with the picture in which metal-enriched winds pollute thecircumgalactic medium surrounding galaxies, and thus connect the small-scalefeedback processes to large-scale properties of galaxy halos.

The main sequence (MS) of star-forming galaxies (SFGs) is the tight relationbetween the galaxy stellar mass and its star formation rate (SFR) and wasobserved up to z ~ 6. The MS relation can be used as a reference forunderstanding the differences among galaxies, characterised by different ratesof stellar production (starbursts, SFGs, and passive galaxies), and thoseinside a galaxy made up of different components (bulge, disk, and halo). Toinvestigate peculiar features found in our sample galaxies, we focus here ontheir star formation history (SFH). We performed a spectral energy distributionfitting procedure that accounted for the energetic balance between UV andfar-IR radiation on a sample of eight nearby face-on spiral galaxies from theDustPedia sample. This approach allowed us to study the spatially resolved MSof the sample and to recover the past SFH. By exploiting the BAGPIPES code, weconstrained the SFHs for each galaxy with a delayed exponentially decliningmodel to derive their mass-weighted age (tMW). A central old region (tMW upto~7Gyr, consistent with the presence of a bulge for various systems) isfollowed by younger regions in which the disks are still forming stars(tMW~4Gyr). At larger distances, tMW increases mildly in general. Strikingly,in two galaxies (NGC4321 and NGC5194), we found a steep increase in tMW thatreached levels similar to those of the bulge. These old stellar populations inthe very galaxy outskirts are unexpected. We discuss their potential origin byconsidering the different gas phases of the source with the most prominentquenched ring, NGC4321, and argue for two main possibilities: 1) someenvironmental effect (e.g. starvation) or 2) the circumgalactic medium ofsources outside of high-density clusters might have stopped to supply pristinegas to the galaxy (e.g. if its specific angular moment is too high for beingaccreted).

The MHONGOOSE (MeerKAT HI Observations of Nearby Galactic Objects: ObservingSouthern Emitters) survey maps the distribution and kinematics of the neutralatomic hydrogen (HI) gas in and around 30 nearby star-forming spiral and dwarfgalaxies to extremely low HI column densities. The HI column densitysensitivity (3 sigma over 16 km/s) ranges from ~ 5 x 10^{17} cm^{-2} at 90''resolution to ~4 x 10^{19} cm^{-2} at the highest resolution of 7''. The HImass sensitivity (3 sigma over 50 km/s) is ~5.5 X 10^5 M_sun at a distance of10 Mpc (the median distance of the sample galaxies). The velocity resolution ofthe data is 1.4 km/s. One of the main science goals of the survey is thedetection of cold, accreting gas in the outskirts of the sample galaxies. Thesample was selected to cover a range in HI masses, from 10^7 M_sun to almost10^{11} M_sun, to optimally sample possible accretion scenarios andenvironments. The distance to the sample galaxies ranges from 3 to 23 Mpc. Inthis paper, we present the sample selection, survey design, and observation andreduction procedures. We compare the integrated HI fluxes based on the MeerKATdata with those derived from single-dish measurement and find good agreement,indicating that our MeerKAT observations are recovering all flux. We present HImoment maps of the entire sample based on the first ten percent of the surveydata, and find that a comparison of the zeroth- and second-moment values showsa clear separation between the physical properties of the HI in areas with starformation and areas without, related to the formation of a cold neutral medium.Finally, we give an overview of the HI-detected companion and satellitegalaxies in the 30 fields, five of which have not previously been catalogued.We find a clear relation between the number of companion galaxies and the massof the main target galaxy.

We examine the morphological and kinematical properties of SPT-2147, astrongly lensed, massive, dusty, star-forming galaxy at $z = 3.762$. Combiningdata from JWST, HST, and ALMA, we study the galaxy's stellar emission, dustcontinuum and gas properties. The imaging reveals a central bar structure inthe stars and gas embedded within an extended disc with a spiral arm-likefeature. The kinematics confirm the presence of the bar and of the regularlyrotating disc. Dynamical modeling yields a dynamical mass, ${M}_{\rm dyn} =(9.7 \pm 2.0) \times 10^{10}$ ${\rm M}_{\odot}$, and a maximum rotationalvelocity to velocity dispersion ratio, $V / \sigma = 9.8 \pm 1.2$. Frommulti-band imaging we infer, via SED fitting, a stellar mass, ${M}_{\star} =(6.3 \pm 0.9) \times 10^{10}$ $\rm{M}_{\odot}$, and a star formation rate,${\rm SFR} = 781 \pm 99$ ${\rm M_{\odot} yr^{-1}}$, after correcting formagnification. Combining these measurements with the molecular gas mass, wederive a baryonic-to-total mass ratio of ${M}_{\rm bar} / {M}_{\rm dyn} = 0.9\pm 0.2$ within 4.0 kpc. This finding suggests that the formation of bars ingalaxies begins earlier in the history of the Universe than previously thoughtand can also occur in galaxies with elevated gas fractions.