We present results from analysis of deep Herschel Space Observatoryobservations of six nearby dwarf galaxies known to host galactic-scale winds.The superior far-infrared sensitivity and angular resolution of Herschel haveallowed detection of cold circumgalactic dust features beyond the stellarcomponents of the host galaxies traced by Spitzer 4.5 $\mu$m images.Comparisons of these cold dust features with ancillary data reveal an imperfectspatial correlation with the ionized gas and warm dust wind components. We findthat typically $\sim$10-20\% of the total dust mass in these galaxies residesoutside of their stellar disks, but this fraction reaches $\sim$60\% in thecase of NGC 1569. This galaxy also has the largest metallicity (O/H) deficit inour sample for its stellar mass. Overall, the small number of objects in oursample precludes drawing strong conclusions on the origin of the circumgalacticdust. We detect no statistically significant trends with star formationproperties of the host galaxies, as might be expected if the dust were liftedabove the disk by energy inputs from on-going star formation activity. Althougha case for dust entrained in a galactic wind is seen in NGC 1569, in all cases,we cannot rule out the possibility that some of the circumgalactic dust mightbe associated instead with gas accreted or removed from the disk by recentgalaxy interaction events, or that it is part of the outer gas-rich portion ofthe disk that lies below the sensitivity limit of the Spitzer 4.5 $\mu$m data.

Galaxies with 'rows' in Vorontsov-Velyaminov's terminology stand out amongthe variety of spiral galactic patterns. A characteristic feature of suchobjects is the sequence of straight-line segments that forms the spiral arm. In2001 A. Chernin and co-authors published a catalog of such galaxies whichincludes 204 objects from the Palomar Atlas. In this paper, we supplement thecatalog with 276 objects based on an analysis of all the galaxies from the NewGeneral Catalogue and Index Catalogue. The total number of NGC and IC galaxieswith rows is 406, including the objects of Chernin et al. (2001). The use ofmore recent galaxy images allowed us to detect more 'rows' on average, comparedwith the catalog of Chernin et al. When comparing the principal galaxyproperties we found no significant differences between galaxies with rows andall S-type NGC/IC galaxies.We discuss twomechanisms for the formation ofpolygonal structures based on numerical gas-dynamic and collisionless N-bodycalculations, which demonstrate that a spiral pattern with rows is a transientstage in the evolution of galaxies and a system with a powerful spiralstructure can pass through this stage. The hypothesis of A. Chernin et al.(2001) that the occurrence frequency of interacting galaxies is twice higheramong galaxies with rows is not confirmed for the combined set of 480 galaxies.The presence of a central stellar bar appears to be a favorable factor for theformation of a system of 'rows'.

During pilot observations of the Virgo Environmental Survey Tracing GalaxyEvolution (VESTIGE), a blind narrow-band Halpha+[NII] imaging survey of theVirgo cluster carried out with MegaCam at the CFHT, we have observed the spiralgalaxy NGC 4254 (M99). Deep Halpha+[NII] narrow-band and GALEX UV imagesrevealed the presence of 60 compact (70-500 pc radius) star forming regions upto ~ 20 kpc outside the optical disc of the galaxy. These regions are locatedalong a tail of HI gas stripped from the disc of the galaxy after a rapidgravitational encounter with another Virgo cluster member that simulationsindicate occurred 280-750 Myr ago. We have combined the VESTIGE data withmultifrequency data from the UV to the far-infrared to characterise the stellarpopulations of these regions and study the star formation process in an extremeenvironment such as the tails of stripped gas embedded in the hot intraclustermedium. The colour, spectral energy distribution (SED), and linear sizeconsistently indicate that these regions are coeval and have been formed aftera single burst of star formation that occurred ~< 100 Myr ago. These regionsmight become free floating objects within the cluster potential well, and bethe local analogues of compact sources produced after the interaction ofgas-rich systems that occurred during the early formation of clusters.

We study the kinematics and the stellar populations of the bulge and disc ofthe spiral galaxy NGC 3521. At each position in the field of view, we separatethe contributions of the bulge and the disc from the total observed spectrumand study their kinematics, age, and metallicities independently. Theirproperties are clearly distinct: the bulge rotates more slowly, has a highervelocity dispersion, and is less luminous than the disc. We identify three mainpopulations of stars in NGC 3521: old ($\geq7$ Gyr), intermediate ($\approx$ 3Gyr), and young ($\leq$1 Gyr). The mass and light of NGC 3521 are dominated bythe intermediate stellar population. The youngest population contributes mostlyto the disc component and its contribution increases with radius. We also studythe luminosity-weighed properties of the stars in NGC 3521. Along thephotometric major axis, we find: i) no age gradient for the stars in the bulge,and a negative age gradient for the stars in the disc; ii) negative metallicitygradients and sub-solar $\alpha$-enhancement for both the bulge and the disc.We propose the following picture for the formation of NGC 3521: initialformation a long time ago ($\geq 7$ Gyr), followed by a second burst of starformation or a merger ($\approx$ 3 Gyrs ago), which contributed predominantlyto the mass-build up of the bulge. Recently ($\leq 1$ Gyr), the disc of NGC3521 experienced an additional episode of star formation that started in theinnermost regions.

We study Red Misfits, a population of red, star-forming galaxies in the localUniverse. We classify galaxies based on inclination-corrected optical coloursand specific star formation rates derived from the Sloan Digital Sky SurveyData Release 7. Although the majority of blue galaxies are star-forming andmost red galaxies exhibit little to no ongoing star formation, a small butsignificant population of galaxies ($\sim$11 per cent at all stellar masses)are classified as red in colour yet actively star-forming. We explore a numberof properties of these galaxies and demonstrate that Red Misfits are not simplydusty or highly-inclined blue cloud galaxies or quiescent red galaxies withpoorly-constrained star formation. The proportion of Red Misfits is nearlyindependent of environment and this population exhibits both intermediatemorphologies and an enhanced likelihood of hosting an AGN. We conclude that RedMisfits are a transition population, gradually quenching on their way to thered sequence and this quenching is dominated by internal processes rather thanenvironmentally-driven processes. We discuss the connection between Red Misfitsand other transition galaxy populations, namely S0's, red spirals and greenvalley galaxies.

ABRIDGED- The UV-optical color magnitude diagram (CMD) of rich galaxy groupsis characterised by a well developed Red Sequence (RS), a Blue Cloud (BC) andthe so-called Green Valley (GV). Loose, less evolved groups of galaxies likelynot virialized yet may lack a well defined RS. This is actually explained inthe framework of galaxy evolution. We are focussing on understanding galaxymigration towards the RS, checking for signatures of such a transition in theirphotometric and morphological properties. We report on the UV properties of asample of ETGs galaxies inhabiting the RS. The analysis of their structures, asderived by fitting a Sersic law to their UV luminosity profiles, suggests thepresence of an underlying disk. This is the hallmark of dissipation processesthat still must have a role in the evolution of this class of galaxies. SPHsimulations with chemo-photometric implementations able to match the globalproperties of our targets are used to derive their evolutionary paths throughUV-optical CDM, providing some fundamental information such as the crossingtime through the GV, which depends on their luminosity. The transition from theBC to the RS takes several Gyrs, being about 3-5 Gyr for the the brightestgalaxies and more long for fainter ones, if it occurs. The photometric study ofnearby galaxy structures in UV is seriously hampered by either the limited FoVof the cameras (e.g in HST) or by the low spatial resolution of the images (e.gin the GALEX). Current missions equipped with telescopes and cameras sensitiveto UV wavelengths, such as Swift-UVOT and Astrosat-UVIT, provide a relativelylarge FoV and better resolution than the GALEX. More powerful UV instruments(size, resolution and FoV) are obviously bound to yield fundamental advances inthe accuracy and depth of the surface photometry and in the characterisation ofthe galaxy environment.

Massive galaxies are thought to form in two phases: an initial, earlycollapse of gas and giant burst of central star formation, followed by thelater accretion of material that builds up their stellar and dark matterhaloes. The globular cluster systems of such galaxies are believed to form in asimilar manner. The initial central burst forms metal-rich (red) clusters,while more metal-poor (blue) clusters are brought in by the later accretion ofless massive satellites. This formation process is thought to lead the creationof the multimodal optical colour distributions seen in the globular clustersystems of massive galaxies. Here we report HST/ACS observations of the massiverelic galaxy NGC 1277 and its globular clusters, a nearby unevolved example ofa high redshift "red nugget". The g-z cluster colour distribution shows thatthe globular cluster system of the galaxy is unimodal and uniquely red. This isin strong contrast to normal galaxies of similar and larger stellar mass, whosecluster systems always exhibit (and are generally dominated by) blue clusters.We argue that the globular cluster system of NGC 1277 indicates that the galaxyhas undergone little (if any) mass accretion after its initial collapse and useanalytic merger trees to show that the total stellar mass accretion is likelyless than ~ 10 %. These results confirm that NGC 1277 is a genuine relic galaxyand show that the blue, metal-poor globular clusters constitute an accretedpopulation in present day massive galaxies.

The Milky Way's satellite galaxies and Globular Clusters (GCs) are known toexhibit an anisotropic spatial distribution. We examine in detail thisanisotropy by the means of the inertia tensor. We estimate the statisticalsignificance of the results by repeating this analysis for random catalogueswhich use the radial distribution of the real sample. Our method reproduces thewell-known planar structure in the distribution of the satellite galaxies. Weshow that for GCs several anisotropic structures are observed. The GCs at smalldistances, $2<R<10$ kpc, show a structure coplanar with the Galactic plane. Atsmaller and larger distances the whole sample of GCs shows quite weakanisotropy. Nevertheless, at largest distances the orientation of the structureis close to that of the satellite galaxies, i.e. perpendicular to the Galacticplane. We estimate the probability of random realization for this structure of1.7%. The Bulge-Disk GCs show a clear disk-like structure lying within thegalactic disk. The Old Halo GCs show two structures: a well pronounced polarelongated structure at $R<3$ kpc which is perpendicular to the galactic plane,and a less pronounced disk-like structure coplanar with the galactic disk at$6<R<20$ kpc. The Young Halo GCs do not show significant anisotropy.