Wandering massive black holes (MBHs) are thought to form throughgravitational recoil or galaxy mergers, but observational confirmation of theirdisplacement in dwarf galaxies, critical laboratories for early-universe SMBHseeding, remains scarce. Using multi-epoch very long baseline interferometry(VLBI), we identify a displaced MBH in the dwarf galaxy MaNGA 12772-12704,located 0.94 kilo-parsec from its optical center. The source exhibitsunambiguous signatures of an accreting MBH: a brightness temperature exceeding$10^9$K, a parsec-scale jet, and flux density variability over a 30-yearbaseline. This system provides the first robust evidence that dynamical blackhole interactions predicted in hierarchical galaxy evolution occur even inlow-mass hosts. The discovery challenges models requiring centralized gasreservoirs for MBH growth and directly informs high-redshift seeding scenarios.

We analyze the morphology of 125 submillimeter galaxies (SMGs) in thePRIMER-COSMOS field using double Sersic modeling on JWST NIRCam images acrosssix bands (F150W, F200W, F277W, F356W, F410M and F444W), with SMGs beingclassified by bulge Sersic index (n_bulge) and bulge-to-total luminosity ratio(B/T). The Kolmogorov-Smirnov test between the bright (SFR > 175 M_sun yr^{-1})and the faint group (SFR < 175 M_sun yr^{-1}) reveals no significantstatistical differences in morphology across bands. However, we notice thatSMGs skew towards higher B/T ratios and lower n_bulge from shorter to longerwavelengths. In F444W, bright SMGs exhibit higher B/T and lower n_bulge,indicating flatter, disturbed bulges, while faint SMGs show lower B/T andhigher n_bulge. Notably, SMGs with higher B/T tend to have low Sersic index,challenging the local universe dichotomy of classical bulges (B/T > 0.5, n > 4)versus pseudo-bulges (B/T < 0.35, n < 2). In the F277W band, non-parametricmeasurements indicate predominantly disk-dominated patterns, with only 24percent of SMGs demonstrating merger signatures. After the removal of SMGs withdisturbed morphology, the bulge classification scheme in F277W showspseudo-bulges (21 percent) and clump migration bulges (16 percent) from secularevolution, compared to 4 percent merger-built bulges. Surprisingly, 48 percentof SMGs defy the classification scheme, showing high B/T (approximately 0.7)but low Sersic index (n_bulge <= 1). Bars are confirmed in 7 percent of SMGs.This work suggests that secular evolution takes precedence over major mergers,supporting the idea that isolated evolution fueled by filamentary gas inflowplays a non-negligible role in the SMG bulge formation.

We present an investigation of the central structure of the S0 galaxy NGC1553, to understand its origin and the underlying dynamical processes thatshape it. The high-resolution integral field spectroscopic data from the MultiUnit Spectroscopic Explorer (MUSE) reveal a well-ordered rotation pattern,consisting of a rapidly rotating nuclear disc that is somewhat decoupled fromthe main disc, together with an inner lens; we collectively refer to thesestructures as the "disc-lens". The central peak in the velocity dispersionindicates the presence of a classical bulge. The nuclear disc is dynamicallycolder than the surrounding disc, while the lens is dynamically hotter. Thehigher-order Gauss-Hermite moments, $h_{3}$ and $h_{4}$, further characterisethe stellar kinematics. An anti-correlation between the line-of-sight velocityand skewness ($h_{3}$) is consistent with regular rotation. In contrast, thering-like enhancement in kurtosis ($h_{4}$) confirms the presence of thenuclear disc component. Unsharp masking of HST images (Erwin et al. 2015)reveals a nuclear bar and faint spiral structures within the central 10 arcsec,supporting the role of secular evolution. The mass-weighted stellar age mapshows an old stellar population in the central regions, with high metallicitythat suggests the in-situ formation of the disc-lens from disc material. Wediscuss possible formation scenarios for the disc-lens, including both minormergers and secular processes, and examine the influence of the Dorado groupenvironment on NGC 1553. Our findings suggest that the disc-lens in NGC 1553formed during the early stages of the galaxy's evolution. However, itssubsequent development has been shaped by internal and external processes.These results provide new insights into the origin and evolution ofkinematically distinct substructures in S0 galaxies.