We present high-resolution Very Large Array continuum observations at the S band (3 GHz, 560 pc scale) and X band (10 GHz, 200 pc scale) of the ram-pressure-stripped Virgo galaxy NGC 4522 to investigate the characteristics of its radio continuum, spectral index, and magnetic field under the influence of the intracluster medium (ICM). The total radio continuum shows an asymmetry that extends northwest, mirroring the H i gas distribution but showing distinct features in the extraplanar regions. The spectral index steepens systematically from α ∼ −0.6 in the main disk to α ∼ −1.1 in the outer disk. We find that the spectral index behavior of the outer disk is mainly due to an ICM shock that can reaccelerate electrons and a significant reduction of thermal emission. Intriguingly, extraplanar clouds exhibit exceptionally flat spectral indices ( α ∼ −0.2 to 0), resulting from a combination of significantly enhanced thermal emission and pronounced spectral aging of the nonthermal component. Although some of these regions correlate with H α , others do not. We propose that the mixing between the ICM and interstellar medium (ISM) is an alternative mechanism that enhances thermal emission independently of star formation. Polarized continuum emissions are highly asymmetric, preferentially distributed along the ICM wind side, and the polarization fraction increases radially outward from the galactic midplane, indicating that the polarized emission is strongly influenced by the ICM wind. Our results show how and where the ICM substantially affects the ISM and also demonstrate that high-frequency observations are crucial for analyzing the radio continuum of ram pressure stripping galaxies.

The Next Generation Virgo Cluster Survey (NGVS) is a deep, high resolution imaging campaign that used the 1 deg^2 MegaCam instrument on the Canada-France-Hawaii Telescope to carry out a comprehensive optical survey of the Virgo cluster, from its core to its virial radius. The NGVS covers a contiguous area of 104 deg^2 (8.63 Mpc^2 at the 16.5 Mpc distance of Virgo) in the u^*-,g-,i-, and z-band, with additional limited coverage in r. In this paper, we present the final catalog of Virgo galaxies across the entire NGVS area. The catalog includes 3680 galaxies considered to be bona fide members of the cluster, spanning a factor of 2.5 million in luminosity, from g = 8.42 mag to g = 24.41 mag (M_g = -22.67 mag to M_g = -6.68 mag). With 2100 previously uncataloged galaxies, the NGVS catalog augments the number of known Virgo members by a factor 2.3. The catalog is complete down to g = 18.6 mag (M_g=-12.5 mag, corresponding to a stellar mass M_* ∼ 1.6×10^7 M_⊙ for an old stellar population) and 50

Globular clusters (GCs) are dense star clusters found in all massive galaxies. Recent work has established that they follow a tight relation between their internal stellar velocity dispersion σ and luminosity, enabling accurate distance measurements. In this work, we aim to apply this GC velocity dispersion (GCVD) distance method to measure the distance to M 104 (NGC 4594, the Sombrero galaxy). We have measured internal stellar velocity dispersions for 85 globular clusters (GCs) and one ultra-compact dwarf galaxy around M 104 using high-resolution multi-object integrated-light spectroscopy with FLAMES/GIRAFFE on the Very Large Telescope. The measured velocity dispersions range from σ = 4 − 30 km s, with a mean uncertainty of Δ σ = 2.5 km s. For a subset of 77 GCs with V -band magnitudes and reliable velocity dispersion measurements above σ > 4 km s, we constructed the M V - σ relation to measure the distance to M 104, finding D = 9.00 ± 0.29 (stat.) ± 0.26 (sys.) Mpc. The GCs follow the Milky Way and M 31 M V − σ relation closely, with the exception of the luminous ultra-compact dwarf SUCD1, which is nearly one magnitude brighter than the mean relation. 29 GCs in the sample have sizes determined from Hubble Space Telescope imaging which allowed us to determine their masses and V -band dynamical mass-to-light ratios (M/L). We find a mean < M / L V > = 2.6 M ⊙ / L ⊙ for the luminous ( M V < − 8 mag) M 104 GCs, which is higher than the Milky Way GCs, but is reminiscent of the brightest GCs in Centaurus A. With the exception of SUCD1, the GCs of M 104 follow the GCVD relation irrespective of their mass-to-light ratio.

We present 50-100pc-resolution JWST/MIRI and NIRCam measurements of mid-infrared (mid-IR) color variations in the diffuse interstellar medium (ISM) of 71 nearby star-forming galaxies from the PHANGS-JWST survey. Mid-IR emission traces the dust column density, intensity (U) and hardness of the interstellar radiation field, and the physical state (charge, size) and abundance of polycyclic aromatic hydrocarbons (PAHs). Mid-IR colors that trace PAH band-ratios remain fairly constant in the diffuse ISM of star-forming disks. However, they show stark variations in extreme environments: highly star-forming central molecular zones (CMZs) and star-formation deserts/quiescent bulges. In CMZs, PAH-to-continuum (3.3/21, 7.7/21, and 11.3/21 μm) and the 10/21 μm continuum colors are 0.2-0.4 dex lower than in normal disks. We attribute this to higher U based on the far-IR dust colors and the high 21 μ m/Σ_ Mol, which we suggest to be a good tracer of U outside star-forming regions. Meanwhile, star-formation deserts show low 7.7 μm PAH emission, resulting in low 7.7/21 μm and 7.7/11.3 μm, while all other mid-IR colors remain typical. This suggests the presence of more neutral PAHs in star-formation deserts, where low 7.7 μm likely reflects ISM conditions similar to early-type and elliptical galaxies. All environments form part of a continuous trend in 7.7/11.3 μm vs. specific star-formation rate.

We present the largest study to date of star cluster mass and age distributions in nearby galaxies. The analysis is based on a uniformly selected catalog of over 15,000 (36,000) human- (machine-) classified compact clusters across 38 spiral galaxies in the PHANGS-Hubble Space Telescope survey, with improved photometric SED age dating that mitigates key degeneracies with reddening and metallicity. The galaxies span a factor of ∼100 in star formation rate (SFR) and in their surface density of star formation and molecular gas (Σ _SFR , ${{\rm{\Sigma }}}_{{{\rm{H}}}_{2}}$ ), and cover a broad range of morphologies. We find that cluster mass functions are well described by a power law, dN / dM ∝ M ^β , with β = −1.9 ± 0.2, and that this shape is remarkably similar across all galaxies in our sample and eight composite groups of galaxies with similar SFRs, with no significant dependence on SFR, Σ _SFR , or ${{\rm{\Sigma }}}_{{{\rm{H}}}_{2}}$ . Cluster age distributions decline steeply and can be described by dN / dτ ∝ τ ^γ with γ = −0.83 ± 0.24, again with little dependence on host-galaxy properties or cluster mass. The independence of the mass and age distributions implies a separable joint distribution, g ( M , τ ) ∝ M ^β τ ^γ , and suggests that cluster populations in spiral disks are dominated by strong, mass-independent dissolution over their first approximately gigayear. These results establish a benchmark for interpreting cluster demographics across diverse galactic environments and provide context for studies of young cluster populations at high redshift.

We present early science results from the Multiphase Astrophysics to Unveil the Virgo Environment (MAUVE) program, which targets 40 Virgo Cluster galaxies to investigate the effect of environment on the interstellar medium (ISM) at similar to 100 pc scales. From 12 galaxies in the MAUVE-Multi Unit Spectroscopic Explorer (MUSE) early sample, we find systematically elevated line ratios compared to Physics at High Angular resolution in Nearby GalaxieS (PHANGS)-MUSE field disks, with higher medians of [N ii]/H alpha (0.75 versus 0.50), [S ii]/H alpha (0.57 versus 0.49), and [O iii]/H beta (1.04 versus 0.68). Spatially resolved Baldwin-Phillips-Terlevich diagrams show 74% of MAUVE spaxels ionized by sources other than H ii regions versus 61% in the field, and we find these ionization differences to be closely coupled to broadened kinematics. In all, 44% of MAUVE spaxels exceed H alpha sigma(LOS) = 40 km s(-1) (versus 26% in the field), driven mainly by non-star-forming gas with sigma(LOS) between 40 and 80 km s(-1), consistent with enhanced contribution of diffuse ionized gas (DIG). A subdominant tail of 5% of spaxels at sigma(LOS) > 100 km s(-1), largely absent in PHANGS-MUSE (1%), points to shocks or turbulent mixing layers from intracluster interactions. Our results show that environmental quenching primarily suppresses star formation, unveiling DIG as the dominant ionized component in cluster disks. The elevated line ratios and broadened kinematics observed in the MAUVE sample reflect the physical state of the ISM in the absence of vigorous star formation, rather than widespread direct environmental excitation. The observed shock-like emission provides an additional, secondary contribution likely driven by active interactions with the intracluster medium.

We use the full-disk Very Large Telescope/MUSE mosaic of NGC 253 to identify 2492 H ii regions and study their resolved structure. With an average physical resolution of 17 pc, this is one of the largest samples of highly resolved spectrally mapped extragalactic H ii regions. Regions of all luminosities exhibit a characteristic emission profile described by a double Gaussian with a marginally resolved or unresolved core with radius < 10 pc surrounded by a more extended halo of emission with radius = 20–30 pc. Approximately 80% of the emission of a region originates from the halo component. As a result of this compact structure, the luminosity–radius relations for core and effective radii of H ii regions depend sensitively on the adopted methodology. Only the isophotal radius yields a robust relationship in NGC 253, but this measurement has an ambiguous physical meaning. We invert the measured emission profiles to infer density profiles and find central densities of n _e ≈ 10–100 cm ^−3 . In the brightest regions, these agree well with densities inferred from the [S ii ] λλ 6716, 6730 doublet. The central density of H ii regions correlates well with the surface brightness within the effective radius. We show that this same scaling relation applies to the recent MUSE + Hubble Space Telescope catalog for 19 nearby galaxies. We also discuss potential limitations, including completeness, impacts of background subtraction and spatial resolution, and the generality of our results when applied to other galaxies.

We present PHANGS-H alpha, a narrowband imaging survey that maps H alpha emission over a sample of 65 nearby massive star-forming galaxies. The data were obtained using the MPG-ESO 2.2-meter telescope at La Silla and the du Pont 2.5-meter telescope at Las Campanas Observatory, within the framework of the multi-wavelength cloud-scale (50-100 pc) resolution mapping of molecular gas and star formation conducted by the Physics at High Angular resolution in Nearby GalaxieS (PHANGS) collaboration. PHANGS-H alpha complements the published PHANGS-ALMA, PHANGS-MUSE, PHANGS-HST, and PHANGS-JWST surveys, providing an anchor point for the photometric and astrometric calibration of these datasets, as well as samples of H II regions and star formation rate maps for the bulk of the PHANGS sample. We describe the observations, data processing, and calibration of the PHANGS-H alpha dataset, as well as the procedures used to derive emission-line fluxes from narrowband imaging. A subset of galaxies with available spectroscopic Ha mapping from the PHANGS-MUSE survey serves as the basis of a detailed comparison with the narrowband photometry presented here. This comparison informs a set of best practices for the processing of narrowband H alpha imaging, which we subsequently apply to the full dataset.

Galactic bars play a critical role in the secular evolution of their hosts by reorganising the ISM. We use a sample of 57 star-forming disc galaxies observed with JWST at 3 and 7.7 μm to probe how the spatial distribution of PAH emission, as a structural marker of the cold ISM, depends on stellar mass and bar presence. We find evidence for a "watershed" at a stellar mass of 10^10 Msun, marking a fundamental transition in the bar-driven distribution of PAH emission. This confirms trends previously predicted by numerical simulations and observed via ionised gas or UV light. While lower-mass galaxies exhibit a disordered and clumpy distribution of PAH emission regardless of bar presence, higher-mass barred hosts display well-structured dynamical features traced by PAH emission with significant gas reservoirs (e.g., discs and rings) within the central 15

We analyse the assembly history of the edge-on lenticular galaxy NGC 3957 using deep integral-field spectroscopic MUSE data from the GECKOS survey. By applying a dust-corrected Multi-Gaussian Expansion and a population-orbit superposition model, we disentangle the galaxy's stellar kinematics, age, and metallicity. We dynamically decompose the galaxy and identify three distinct components: a dynamically-cold main disc, a compact Nuclear Stellar Disc (NSD), and a hot component. The NSD emerges as the youngest and most metal-rich component (t = 6.9 ± 0.4 Gyr; [Z/H] = 0.49 ± 0.06 dex), implying that the stellar bar is a long-lived structure that formed at least ∼ 7 Gyr ago. The main stellar disc is dynamically cold (σ_z ∼ 20-30 km/s), precluding any significant mergers over the last ∼ 8 Gyr, and exhibits a strong positive age gradient (younger inside, older outside) beyond the bar radius. Synthesising these dynamical fossil records, NGC 3957 likely evolved as a `faded spiral' in a small-to-medium group environment. Its outer disc might passively fade due to mild gas starvation, while the bar fuelled prolonged central star formation. Comparison with S0s in the Fornax cluster reveals that this combination of internal secular evolution and mild starvation produces `outside-in' fading signatures that could mimic the environmental stripping typically seen in dense clusters.

We present stellar kinematics of the MUSE Most Massive Galaxies (M3G) Survey, comprising 25 galaxies brighter than -25.7 mag in the Ks band and stellar masses above approximate to 6 & times; 10(11 )M circle dot. The galaxies are divided into brightest cluster galaxies (BCGs) and lower-ranked (in brightness) galaxies (non-BCGs) in three rich galaxy clusters within the core of the Shapley Supercluster. We find several velocity maps with rich kinematic structures, including multiple spin reversals within the region encompassing two central effective radii, typically associated with BCGs. Additionally, the majority of the BCGs show rotation around the major axis of the galaxy at least in one of the visible velocity components. These kinematic structures are possible only if galaxies have non-axisymmetric shapes and contain several orbital families with both prograde and retrograde rotations. We argue that such velocity maps provide further evidence that the evolution of very massive galaxies is influenced by, possibly repeated, gas-poor major merging. There are six fast rotators in the M3G sample, and they are all among non-BCGs and typically ranked below the third brightest galaxy in their clusters. Based on the properties of the h(3) Gauss-Hermite moment, fast rotation can be linked to the dominance of prograde rotating short-axis tubes in the orbital distribution. Slow rotators are BCGs or the second or sometimes third brightest galaxies, indicating that the galaxy mass (brightness) is not the only driver of low spin and that the location within the local environment also plays a role. Slow rotators, as evidenced from their multi-spin velocity maps, require more complex orbital structures. Furthermore, some BCGs show kinematic evidence for a secondary component at larger radii, which is likely not in equilibrium with the main galaxy and possibly made of stars accreted from other cluster galaxies. Multi-spin velocity maps, low angular momentum, and additional kinematic components highlight the differences in the evolutionary histories of BCGs (including second-ranked galaxies) and non-BCGs.

We present PHANGS-H α , a narrowband imaging survey that maps H α emission over a sample of 65 nearby massive star-forming galaxies. The data were obtained using the MPG-ESO 2.2-meter telescope at La Silla and the du Pont 2.5-meter telescope at Las Campanas Observatory, within the framework of the multi-wavelength cloud-scale (50–100 pc) resolution mapping of molecular gas and star formation conducted by the Physics at High Angular resolution in Nearby GalaxieS (PHANGS) collaboration. PHANGS-H α complements the published PHANGS-ALMA, PHANGS-MUSE, PHANGS-HST, and PHANGS-JWST surveys, providing an anchor point for the photometric and astrometric calibration of these datasets, as well as samples of H II regions and star formation rate maps for the bulk of the PHANGS sample. We describe the observations, data processing, and calibration of the PHANGS-H α dataset, as well as the procedures used to derive emission-line fluxes from narrowband imaging. A subset of galaxies with available spectroscopic Ha mapping from the PHANGS-MUSE survey serves as the basis of a detailed comparison with the narrowband photometry presented here. This comparison informs a set of best practices for the processing of narrowband H α imaging, which we subsequently apply to the full dataset.

Context. Nearby galaxies exhibit a variety of structures, including so-called central or (circum-)nuclear rings that are similar to the Milky Way (MW) Central Molecular Zone (CMZ). These rings are common in barred galaxies and can be gas-rich and highly star-forming. Aims. We aim to study the molecular gas content and star formation rate of central rings within nearby galaxies and link them to global galaxy properties, especially the bar morphology. Methods. We utilized 1 ''(less than or similar to 100 pc) resolution CO(2-1) observations from the PHANGS-ALMA survey, visually identifying 20 central rings and determine their properties. For 14 of these rings, MUSE observations tracing star formation rate (SFR) surface density were available. We derived the rings' geometry, integrated molecular gas masses, SFRs, depletion times, and compared them to host galaxy and bar properties from the literature. Results. Molecular gas is an effective tracer for central rings. Previous studies have used ionized gas and dust tracers to identify central rings in galaxies of similar morphological types as the PHANGS galaxies (numerical Hubble type T similar to -3 to T similar to 9). In comparison, molecular gas yields similar fractions of galaxies hosting central rings and similar radii distributions. The gaseous central rings have typical radii of similar to 400(-150)(+250)pc, molecular gas masses of log(M/M-circle dot) similar to 8.1(-0.23)(+0.17), and SFRs of similar to 0.21(-0.16)(+0.15) M-circle dot/yr. As a result, they contribute 5.6(-2.1)(+4.5)% and 13(-5)(+10)% to their host galaxies' molecular gas mass and SFR, respectively. While the MW CMZ sits at the lower end of the radius, molecular gas mass, and SFR distribution, it matches well in terms of ring molecular gas mass and SFR fraction, and depletion time. Longer bars contain more massive molecular central rings, but there is no correlation between the classical bar strength parameters (Q(b), epsilon(bar), A(2)(max)) and the ring's molecular gas content. Conclusions. Although absolute central ring properties (ring radius, molecular gas mass, SFR) likely depend on host galaxy properties, the similarities between the MW CMZ and PHANGS central rings in relative parameters (molecular gas and SFR fraction, depletion time) suggest that the processes of gas inflow and star formation are similar for central rings across nearby galaxies.

Galactic bars are thought to play a critical role in the secular evolution of their hosts by, for example, reorganising the interstellar medium (ISM). We used a sample of 57 star-forming disc galaxies observed with JWST at 3 and 7.7 μm to probe how the spatial distribution of polycyclic aromatic hydrocarbon (PAH) emission as a structural marker of the cold ISM might depend on galaxy stellar mass and the presence of a bar. We find evidence for a 'watershed' at a stellar mass of 10^10 ,R_b range in barred systems with stellar masses above 10^10 marking a fundamental transition in the bar-driven distribution of PAH emission. This confirms trends previously predicted by numerical simulations and observed via ionised gas or UV light. While lower-mass galaxies exhibit a disordered and clumpy distribution of PAH emission regardless of bar presence, higher-mass barred hosts display well-structured dynamical features traced by PAH emission with significant gas reservoirs (e.g., discs and rings) within the central 15% of the bar radius (R_b). Furthermore, we observed a systematic depletion of PAH emission within the 0.2–0.8 Such central discs, rings, and associated radial dips ('bar deserts') appear to be a mass-dependent phenomenon as they are ubiquitous in massive galaxies but mostly absent in their lower-mass counterparts. In contrast to the structured features in massive hosts, the disorganised ISM in lower-mass galaxies masks the commonly observed bar-driven signatures. This suggests that tracer selection and dust obscuration may significantly bias observed bar fractions. Our study underlines the existence of two regimes of secular evolution, with different impacts and observability of bar-driven processes, and it reaffirms the role of bars as the primary drivers of rapid secular evolution in galaxies above 10^10, while the impact of bars is significantly reduced or delayed below this threshold. Our results further underscore the need to critically account for these processes when modelling galaxy evolution in cosmological simulations.

We present PHANGS-Hα, a narrowband imaging survey that maps Hα emission over a sample of 65 nearby massive star-forming galaxies. The data were obtained using the MPG-ESO 2.2-meter telescope at La Silla and the du Pont 2.5-meter telescope at Las Campanas Observatory, within the framework of the multi-wavelength cloud-scale (50–100 pc) resolution mapping of molecular gas and star formation conducted by the Physics at High Angular resolution in Nearby GalaxieS (PHANGS) collaboration. PHANGS-Hα complements the published PHANGS-ALMA, PHANGS-MUSE, PHANGS-HST, and PHANGS-JWST surveys, providing an anchor point for the photometric and astrometric calibration of these datasets, as well as samples of H II regions and star formation rate maps for the bulk of the PHANGS sample. We describe the observations, data processing, and calibration of the PHANGS-Hα dataset, as well as the procedures used to derive emission-line fluxes from narrowband imaging. A subset of galaxies with available spectroscopic Ha mapping from the PHANGS-MUSE survey serves as the basis of a detailed comparison with the narrowband photometry presented here. This comparison informs a set of best practices for the processing of narrowband Hα imaging, which we subsequently apply to the full dataset.

The vertical evolution of galactic discs is governed by the sub-structures within them. Several of these features, including bulges and kinematically distinct discs, are best studied in edge-on galaxies, as the viewing angle allows the easier separation of component light. For this work, we examined the diversity of kinematic sub-structure present in the first 12 galaxies observed from the GECKOS survey, a VLT/MUSE large programme providing a systematic study of 36 edge-on Milky Way-mass disc galaxies. Employing the NGIST analysis pipeline, we derived the mean luminosity-weighted line-of-sight stellar velocity (V-star), velocity dispersion (sigma(star)), skew (h(3)), and kurtosis (h(4)) for the sample, and examined 2D maps and 1D line profiles. Common clear kinematic signatures were observed: all galaxies display h(3) - V-star sign mismatches in the outer disc regions consistent with a (quasi-)axisymmetric, rotating disc of stars. After scrutinising visual morphologies, we found that the majority of this sample (8/12) possess boxy-peanut bulges and host the corresponding kinematic structure predicted for stellar bars viewed in projection. Inferences were made on the bar viewing angle with respect to the line of sight from the strength of these kinematic indicators; we found one galaxy whose bar is close to side-on with respect to the observer, and two that are close to end-on. Four galaxies exhibit strong evidence for the presence of nuclear discs, including central h(3)-V-star profile anti-correlations, croissant-shaped central depressions in sigma(star) maps, strong gradients in h(3), and positive h(4) plateaus over the expected nuclear disc extent. The strength of the h(3) feature corresponds to the size of the nuclear disc, measured from the h(3) turnover radius, taking into account geometric effects. We can explain the features within the kinematic maps of the four unbarred galaxies via disc structure(s) alone. We do not find any need to invoke the existence of dispersion-dominated bulges in any of the sample galaxies. Obtaining the specialised data products for this paper and the broader GECKOS survey required significant development of existing integral field spectroscopic (IFS) analysis tools. Therefore, we also present the NGIST pipeline: a modern, sophisticated, and easy-to-use pipeline for the analysis of galaxy IFS data, and the key tool employed by the GECKOS survey for producing value-added data products. We conclude that the variety of kinematic sub-structures seen in GECKOS galaxies requires a contemporary view of galaxy morphology, expanding on the traditional view of galaxy structure, and uniting the kinematic complexity observed in the Milky Way with the extragalactic.

The Multiphase Astrophysics to Unveil the Virgo Environment (MAUVE) project is a multi-facility programme exploring how dense environments transform galaxies. Combining a VLT/MUSE P110 Large Programme and ALMA observations of 40 late-type Virgo Cluster galaxies, MAUVE resolves star formation, kinematics, and chemical enrichment within their molecular gas discs. A key goal is to track the evolution of cold gas that survives in the inner regions of satellites after entering the cluster, and how it evolves across different infall stages. With its high spatial resolution – probing down to the physical scales of giant molecular cloud complexes – and multiphase synergy, MAUVE aims to offer a time-resolved view of environmental quenching and set a new benchmark for cluster galaxy studies.

Spiral arms play a central role in disc galaxies, but their dynamical nature remains a long-standing open question. Azimuthal offsets between molecular gas and star formation are expected if gas crosses spiral arms, as predicted by quasi-stationary density wave theory. In this work, we measure offsets between CO and H alpha peaks in radial bins for 24 galaxies from the PHANGS survey that display a well-delineated spiral structure. The offsets exhibit substantial scatter, implying that star formation is not exclusively initiated at a coherent spiral shock. We define offsets such that positive values mean H alpha peaks lie ahead of CO peaks in the direction of galactic rotation. With this convention, 14 galaxies show mean positive CO-H alpha offsets, typically of a few hundred parsecs. In four of these 14 galaxies (17% of the total), offsets become smaller with increasing radius, as expected for a single quasi-stationary spiral density wave. Ten galaxies (42%) show positive mean offsets but no clear correlation with radius, which is compatible with multiple overlapping modes. In the remaining ten galaxies (42%), we find no significantly positive offsets, which could point to transient dynamical spirals or material arms, where gas and stars co-rotate with the spiral perturbation. Across the full sample, we find mostly positive offsets between CO peaks and the gravitational potential minimum, confirming that gas often crosses the spiral perturbation. For the four galaxies with clear positive offsets and a radial trend, we derived pattern speeds in good agreement with the literature. Overall, our results suggest that even well-delineated spirals in the local Universe can arise from a variety of underlying dynamical mechanisms.