We investigate the 3D spin alignment of galaxies with respect to thelarge-scale filaments using the MaNGA survey. The cosmic web is reconstructedfrom the Sloan Digital Sky Survey using Disperse and the 3D spins of MaNGAgalaxies are estimated using the thin disk approximation with integral fieldspectroscopy kinematics. Late-type spiral galaxies are found to have theirspins parallel to the closest filament's axis. The alignment signal is found tobe dominated by low-mass spirals. Spins of S0-type galaxies tend to be orientedpreferentially in perpendicular direction with respect to the filament's axis.This orthogonal orientation is found to be dominated by S0s that show a notablemisalignment between their kinematic components of stellar and ionised gasvelocity fields and/or by low mass S0s with lower rotation support compared totheir high mass counterparts. Qualitatively similar results are obtained whensplitting galaxies based on the degree of ordered stellar rotation, such thatgalaxies with high spin magnitude have their spin aligned, and those with lowspin magnitude in perpendicular direction to the filaments. In the context ofconditional tidal torque theory, these findings suggest that galaxies' spinsretain memory of their larger-scale environment. In agreement with measurementsfrom hydrodynamical cosmological simulations, the measured signal at lowredshift is weak, yet statistically significant. The dependence of thespin-filament orientation of galaxies on their stellar mass, morphology andkinematics highlights the importance of sample selection to detect the signal.

Outflows of ionized gas driven by active galactic nuclei (AGN) maysignificantly impact the evolution of their host galaxies. However, determiningthe energetics of these outflows is difficult with spatially unresolvedobservations that are subject to strong global selection effects. We presentpart of an ongoing study using Hubble Space Telescope (HST) and Apache PointObservatory (APO) spectroscopy and imaging to derive spatially-resolved massoutflow rates and energetics for narrow line region (NLR) outflows in nearbyAGN that are based on multi-component photoionization models to account forspatial variations in the gas ionization, density, abundances, and dustcontent. This expanded analysis adds Mrk 3, Mrk 78, and NGC 1068, doubling thesample in Revalski (2019). We find that the outflows contain total ionized gasmasses of $M \approx 10^{5.5} - 10^{7.5}$ $M_{\odot}$ and reach peak velocitiesof $v \approx 800 - 2000$ km s$^{-1}$. The outflows reach maximum mass outflowrates of $\dot M_{out} \approx 3 - 12$ $M_{\odot}$ yr$^{-1}$ and encompasstotal kinetic energies of $E \approx 10^{54} - 10^{56}$ erg. The outflowsextend to radial distances of $r \approx 0.1 - 3$ kpc from the nucleus, withthe gas masses, outflow energetics, and radial extents positively correlatedwith AGN luminosity. The outflow rates are consistent with in-situ ionizationand acceleration where gas is radiatively driven at multiple radii. Theseradial variations indicate that spatially-resolved observations are essentialfor localizing AGN feedback and determining the most accurate outflowparameters.

Lenticular galaxies (S0s) were considered mainly as passive evolved spiralsdue to environmental effects for a long time; however, most S0s in the fieldcannot fit into this common scenario. In this work, we study one special case,SDSS J120237.07+642235.3 (PGC 38025), a star-forming field S0 galaxy with anoff-nuclear blue core. We present optical integral field spectroscopic (IFS)observation with the 3.5 meter telescope at Calar Alto (CAHA) Observatory, andhigh-resolution millimeter observation with the NOrthern Extended MillimeterArray (NOEMA). We estimated the star formation rate (SFR = 0.446 $M_\odotyr^{-1}$) and gaseous metallicity (12 + log(O/H) = 8.42) for PGC 38025, whichfollows the star formation main sequence and stellar mass - metallicityrelation. We found that the ionized gas and cold molecular gas in PGC 38025show the same spatial distribution and kinematics, whilst rotating misalignedwith stellar component. The off-nuclear blue core is locating at the sameredshift as PGC 38025 and its optical spectrum suggest it is \rm H\,{\sc ii}region. We suggest that the star formation in PGC 38025 is triggered by agas-rich minor merger, and the off-nuclear blue core might be a localstar-formation happened during the accretion/merger process.