We use a 0.7-m telescope in the framework of the Halos and Environments ofNearby Galaxies (HERON) survey to probe low surface brightness structures innearby galaxies. One of our targets, UGC 4599, is usually classified as anearly-type galaxy surrounded by a blue ring making it a potential Hoag's Objectanalog. Prior photometric studies of UGC 4599 were focused on its bright coreand the blue ring. However, the HERON survey allows us to study its faintextended regions. With an eight hour integration, we detect an extremely faintouter disk with an extrapolated central surface brightness of$\mu_\mathrm{0,d}(r)=25.5$ mag arcsec$^{-2}$ down to 31 mag arcsec$^{-2}$ and ascale length of 15 kpc. We identify two distinct spiral arms of pitch angle~6{\deg} surrounding the ring. The spiral arms are detected out to ~45 kpc inradius and the faint disk continues to ~70 kpc. These features are also seen inthe GALEX FUV and NUV bands, in a deep u-band image from the 4.3m LowellDiscovery Telescope (which reveals inner spiral structure emerging from thecore), and in HI. We compare this galaxy to ordinary spiral and ellipticalgalaxies, giant low surface brightness (GLSB) galaxies, and Hoag's Objectitself using several standard galaxy scaling relations. We conclude that thepseudobulge and disk properties of UGC 4599 significantly differ from those ofHoag's Object and of normal galaxies, pointing toward a GLSB galaxy nature andfilamentary accretion of gas to generate its outer disk.

During the visual observations of optical imaging data obtained from theDECaLS, a serendipitous discovery emerged, revealing the presence of a ringedgalaxy, DES J024008.08-551047.5 (DJ0240). We performed one dimensionalisophotal and two-dimensional GALFIT analysis to confirm the orthogonal natureof the ring galaxy and identify distinct components within the host galaxy. Wediscovered the galaxy DJ0240 as a potential PRG candidate with a ring componentpositioned almost perpendicular to the host galaxy. The position angles of thering and host components have been determined to be 80 and 10 degrees,respectively, indicating that they are nearly orthogonal to each other. Weobserved that the ring component extends three times more than the host galaxyand shows a distinct colour separation, being bluer than the host. Theestimated g - r colour values of host and ring components are 0.86+/-0.02 and0.59+/-0.10 mag, respectively. The colour value of the ring component issimilar to typical spiral galaxies. The host galaxy`s colour and the presenceof a bulge and disk components indicate the possibility of the host galaxybeing a lenticular type. Based on the comparison of photometric propertiesbetween the PRGs and other ring-type galaxies (RTGs), our findings reveal asubtle, yet noticeable, colour difference between the host and ring components.We observed that both host and ring components of DJ0240 align more closelywith PRGs than with RTGs. Furthermore, we compared the sersic index values ofthe ring component (nring) of galaxy DJ0240 with a selected sample of PRGs andHoag-type galaxies. The results showed DJ0240 had a remarkably low nring valueof 0.13, supporting the galaxy`s classification as a PRG. Hence, we suggestthat the ring galaxy DJ0240 is a highly promising candidate for inclusion inthe family of PRGs.

The $z$~0.1 type-2 QSO J1430+1339 (the 'Teacup') is a complex galaxy showinga loop of ionised gas ~10 kpc in diameter, co-spatial radio bubbles, a compact(~1 kpc) jet, and outflow activity. We used VLT/MUSE optical integral fieldspectroscopic observations to characterise the properties and effects of thegalactic ionised outflow from kpc up to tens of kpc scales and compare themwith those of the radio jet. We detect a velocity dispersion enhancement (>300km/s) elongated over several kpc perpendicular to the radio jet, the AGNionisation lobes, and the fast outflow, similar to what is found in othergalaxies hosting compact, low-power jets, indicating that the jet stronglyperturbs the host ISM. The mass outflow rate decreases with distance from thenucleus, from around 100 $M_\odot$/yr in the inner 1-2 kpc to <0.1 $M_\odot$/yrat 30 kpc. The ionised mass outflow rate is ~1-8 times higher than themolecular one, in contrast with what is often quoted in AGN. The driver of themulti-phase outflow is likely a combination of AGN radiation and the jet. Theoutflow mass-loading factor (~5-10) and the molecular gas depletion time(<10$^8$ yr) indicate that the outflow can significantly affect the starformation and the gas reservoir in the galaxy. However, the fraction of theionised outflow that is able to escape the dark matter halo potential is likelynegligible. We detect blue-coloured continuum emission co-spatial with theionised gas loop. Here, stellar populations are younger (<100-150 Myr) than inthe rest of the galaxy (~0.5-1 Gyr). This constitutes possible evidence forstar formation triggered at the edge of the bubble due to the compressingaction of the jet and outflow ('positive feedback'), as predicted by theory.All in all, the Teacup constitutes a rich system in which AGN feedback fromoutflows and jets, in both its negative and positive flavours, co-exist.

We employ a recently developed population-orbit superposition technique tosimultaneously fit the stellar kinematic and age maps of 82 CALIFA spiralgalaxies and obtain the ages of stars in different dynamical structures. Wefirst evaluated the capabilities of this method on CALIFA-like mock datacreated from the Auriga simulations. The recovered mean ages of dynamicallycold, warm, and hot components match the true values well, with anobservational error of up to $20\%$ in the mock age maps. For CALIFA spiralgalaxies, we find that the stellar ages of the cold, warm, and hot componentsall increase with the stellar mass of the galaxies, from $\overline{t_{\rmcold}}\sim2.2$ Gyr, $\overline{t_{\rm warm}}\sim2.3$ Gyr, and $\overline{t_{\rmhot}}\sim2.6$ Gyr for galaxies with stellar mass $M_*<10^{10}\,\rm M_{\odot}$,to $\overline{t_{\rm cold}}\sim4.0$ Gyr, $\overline{t_{\rm warm}}\sim5.1$ Gyr,and $\overline{t_{\rm hot}}\sim5.9$ Gyr for galaxies with $M_*>10^{11}\,\rmM_{\odot}$. About $80\%$ of the galaxies in our sample have $t_{\rm hot}>t_{\rmcold}$, and the mean values of $t_{\rm hot}-t_{\rm cold}$ also increase withstellar mass, from $0.7_{-0.2}^{+0.6}$ Gyr in low-mass galaxies ($10^{8.9}\,\rmM_{\odot}<M_*\le10^{10.5}\,\rm M_{\odot}$) to $1.7_{-0.2}^{+0.7}$ Gyr inhigh-mass galaxies ($10^{10.5}\,\rm M_{\odot}<M_*<10^{11.3}\,\rm M_{\odot}$).The stellar age is younger in disks than in bulges, on average. This suggeststhat either the disks formed later and/or that they experienced a moreprolonged and extensive period of star formation. Lower-mass spiral galaxieshave younger bulges and younger disks, while higher-mass spiral galaxiesgenerally have older bulges, and their disks span a wide range of ages. This isconsistent with the scenario in which the bulges in more massive spirals formedearlier than those in less massive spirals.