We present a comprehensive study of the interstellar NaI $\lambda$5890, 5895(NaD) resonant lines in a complete spectroscopic sample of $\sim 600,000$passive, star-forming and starburst galaxies drawn from SDSS DR7 in order tolook for cold-gas outflows in the local Universe. Individual galaxy spectra arestacked in bins of stellar mass and SFR and the dependence of galactic winds,with respect to the galaxies position in the SFR-$M_{\star}$ plane isinvestigated. While in most cases the interstellar medium (ISM) lines are fixedat the galaxy systemic velocity, at the higher SFR tail (SFR$>12.5 M_{\odot}yr^{-1}$), we find evidence of blue-shifted NaD absorption profiles, which weinterpret as evidence of neutral outflowing gas. We explore the properties ofthe ISM in these galaxies with high SFR, in particular relating the absorptionNaD line shape with the galaxy geometry in galaxies with different ionizationmechanisms: AGN and star-formation. We find that: a) the ISM NaD absorptionlines show a clear transition from a strong disk-like component, perfectlycentered to the systemic velocity, in the edge-on system ($i > 50^\circ$ of thedisk rotation axis), to an outflow, blue-shifted, component in face-on galaxies($i < 50^\circ$); b) these trends are observed in galaxies classified as"purely" SF and AGN dominated objects. We compare the kinematics of the neutralgas with the kinematics of the ionized gas as traced by the [OIII]$\lambda$5007emission lines. We find that, in these high SFR galaxies, the perturbations ofthe [OIII] emission line are present only in AGN or composite systems. Inconclusion, we find that, in the local Universe, galactic winds show two faceswhich are related to two different ejection mechanisms, namely the neutraloutflowing gas phase related to the star formation rate along the galaxy diskand the ionized winds related to the AGN feedback.

We present spatially resolved stellar kinematic maps, for the first time, fora sample of 17 intermediate redshift galaxies (0.2 < z < 0.8). We used deepMUSE/VLT integral field spectroscopic observations in the Hubble Deep FieldSouth (HDFS) and Hubble Ultra Deep Field (HUDF), resulting from ~30hintegration time per field, each covering 1'x1' field of view, with ~0.65"spatial resolution. We selected all galaxies brighter than 25mag in the I bandand for which the stellar continuum is detected over an area that is at leasttwo times larger than the spatial resolution. The resulting sample containsmostly late-type disk, main-sequence star-forming galaxies with 10^8.5 -10^10.5 Msun. Using a full-spectrum fitting technique, we derivetwo-dimensional maps of the stellar and gas kinematics, including the radialvelocity V and velocity dispersion sigma. We find that most galaxies in thesample are consistent with having rotating stellar disks with roughly constantvelocity dispersions and that the Vrms=sqrt{V^2+sigma^2} of the gas and stars,a scaling proxy for the galaxy gravitational potential, compare well to eachother. These spatially resolved observations of intermediate redshift galaxiessuggest that the regular stellar kinematics of disk galaxies that is observedin the local Universe was already in place 4 - 7 Gyr ago and that their gaskinematics traces the gravitational potential of the galaxy, thus is notdominated by shocks and turbulent motions. Finally, we build dynamicalaxisymmetric Jeans models constrained by the derived stellar kinematics for twospecific galaxies and derive their dynamical masses. These are in goodagreement (within 25%) with those derived from simple exponential disk modelsbased on the gas kinematics. The obtained mass-to-light ratios hint towardsdark matter dominated systems within a few effective radii.

Studies of low surface brightness (LSB) galaxies in nearby clusters haverevealed a sub-population of extremely diffuse galaxies with central surfacebrightness $\mu_{0,g'}$ > 24 mag arcsec$^{-2}$ and effective radius between 1.5kpc < R$_{e}$ < 10 kpc. The origin of these Ultra Diffuse Galaxies (UDGs) isstill unclear, although several theories have been suggested. We exploit thedeep g', r' and i'-band images of the Fornax Deep Survey (FDS), in order toidentify LSB galaxies in the center of the Fornax cluster. We identifiedvisually all extended structures having r'-band central surface brightness of$\mu_{0,r'}$ > 23 mag arcsec$^{-2}$. We classified the objects based on theirappearance and performed 2D S\'ersic model fitting with GALFIT. We analyzedtheir distribution and orientations in the cluster, and studied their colorsand compared the LSB galaxies in Fornax with those in other environments. Oursample consists of 205 galaxies of which 196 are LSB dwarfs (with R$_e$ <1.5kpc) and nine are UDGs (R$_e$ > 1.5 kpc). We show that the UDGs have g'-r'colors similar to those of LSB dwarfs. The largest UDGs in our sample appeardifferent from the other LSB galaxies, in that they are significantly moreelongated and extended, whereas the smaller UDGs differ from the LSB dwarfsonly by their effective radii. We do not find clear differences between thestructural parameters of the UDGs in our sample and those of UDGs in othergalaxy environments. We find that the dwarf LSB galaxies in our sample are lessconcentrated in the cluster center than the galaxies with higher surfacebrightness, and that their number density drops in the core of the cluster. Ourfindings are consistent with the small UDGs forming the tail of a continuousdistribution of less extended LSB galaxies. However, the elongated anddistorted shapes of the large UDGs could imply that they are tidally disturbedgalaxies.

X-ray emitting gaseous coronae around massive galaxies are a basic predictionof galaxy formation models. Although the coronae around spiral galaxies offer afundamental test of these models, observational constraints on theircharacteristics are still scarce. While the presence of extended hot coronaehas been established around a handful of massive spiral galaxies, the shortX-ray observations only allowed to measure the basic characteristics of thecoronae. In this work, we utilize deep XMM-Newton observations of NGC 6753 toexplore its extended X-ray corona in unprecedented detail. Specifically, weestablish the isotropic morphology of the hot gas, suggesting that it residesin hydrostatic equilibrium. The temperature profile of the gas shows a decreasewith increasing radius: it drops from $kT\approx0.7$ keV in the innermost partsto $kT\approx0.4$ keV at 50 kpc radius. The temperature map reveals the complextemperature structure of the gas. We study the metallicity distribution of thegas, which is uniform at $Z\approx0.1$ Solar. This value is about an order ofmagnitude lower than that obtained for elliptical galaxies with similar darkmatter halo mass, hinting that the hot gas in spiral galaxies predominantlyoriginates from external gas inflows rather than from internal sources. Byextrapolating the density profile of the hot gas out to the virial radius, weestimate the total gas mass and derive the total baryon mass of NGC 6753. Weconclude that the baryon mass fraction is $f_{\rm b} \approx 0.06$, implyingthat about half of the baryons are missing.

We present the analysis of the XMM-Newton data of the Circum-Galactic Mediumof MASsive Spirals (CGM-MASS) sample of six extremely massive spiral galaxiesin the local Universe. All the CGM-MASS galaxies have diffuse X-ray emissionfrom hot gas detected above the background extending $\sim(30-100)\rm~kpc$ fromthe galactic center. This doubles the existing detection of such extended hotCGM around massive spiral galaxies. The radial soft X-ray intensity profile ofhot gas can be fitted with a $\beta$-function with the slope typically in therange of $\beta=0.35-0.55$. This range, as well as those $\beta$ valuesmeasured for other massive spiral galaxies, including the Milky Way (MW), arein general consistent with X-ray luminous elliptical galaxies of similar hotgas luminosity and temperature, and with those predicted from a hydrostaticisothermal gaseous halo. Hot gas in such massive spiral galaxy tends to havetemperature comparable to its virial value, indicating the importance ofgravitational heating. This is in contrast to lower mass galaxies where hot gastemperature tends to be systematically higher than the virial one. The ratio ofthe radiative cooling to free fall timescales of hot gas is much larger thanthe critical value of $\sim10$ throughout the entire halos of all the CGM-MASSgalaxies, indicating the inefficiency of gas cooling and precipitation in theCGM. The hot CGM in these massive spiral galaxies is thus most likely in ahydrostatic state, with the feedback material mixed with the CGM, instead ofescaping out of the halo or falling back to the disk. We also homogenize andcompare the halo X-ray luminosity measured for the CGM-MASS galaxies and othergalaxy samples and discuss the "missing" galactic feedback detected in thesemassive spiral galaxies.