Astronomy & Astrophysics最新文献

{"title":"A `universal' supernova efficiency to drive the HI turbulence in nearby star-forming galaxies","authors":"Lauri Sassali,Cecilia Bacchini,Aku Venhola,Giuliano Iorio,Antonino Marasco","doi":"10.1051/0004-6361/202661120","DOIUrl":"https://doi.org/10.1051/0004-6361/202661120","url":null,"abstract":"The origin of cold gas turbulence in galaxies has been extensively debated. Supernovae (SNe), the dominant form of stellar feedback, were thought insufficient to sustain it against dissipation, especially in galactic environments with low star formation rates (SFRs). In this work, we investigate the origin of the neutral atomic gas (HI) turbulence in dwarf irregular galaxies, a challenging regime of low masses and SFRs. We built on a recent study of spirals showing that disc flaring prolongs the dissipation timescale, reducing the energy needed to sustain turbulence and making SN feedback viable. We measured the SN efficiency, which is the fraction of SN energy required to sustain HI turbulence in 14 dwarfs, and tested whether a universal efficiency holds across a sample representative of the star-forming main sequence. From the observed HI distributions and kinematics, we derived the radial profiles of the HI kinetic energy per unit area and modelled them as the sum of thermal energy and turbulent energy from SNe, constrained by the observed SFR surface density. We considered pure cold and warm neutral medium (WNM) phases as limiting cases, as well as a mixed two-phase scenario, obtaining the SN efficiency and WNM fraction via hierarchical Bayesian inference. We found that the observed HI kinetic energy in dwarfs requires only łesssim 3% of the SN energy, and that a universal efficiency of ≈ 2% explains the HI turbulence across our main sequence sample. Our findings suggest that the SN efficiency remains similar across galaxies with different properties, offering valuable constraint for feedback recipes in galaxy evolution models.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"68 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149209115","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Solar spicule population properties inferred from IRIS Mg II k off-limb spectra using likelihood-free Bayesian inference","authors":"Jiří Štěpán,Stanislav Gunár,Akiko Tei,Petr Heinzel","doi":"10.1051/0004-6361/202660744","DOIUrl":"https://doi.org/10.1051/0004-6361/202660744","url":null,"abstract":"Solar spicules are ubiquitous and strongly overlap in off-limb observations, which complicates the interpretation of individual events. We aim to infer population-level properties of spicules from IRIS Mg II k off-limb spectra using a forward model that explicitly accounts for line-of-sight superposition and instrumental effects. We constructed a stochastic 3D spicule-population model and synthesized Mg II k spectra with radiative transfer, including instrumental degradation and photon noise. We then constrained the hyperparameters that describe the underlying spicule population with likelihood-free Bayesian inference. This approach combines approximate Bayesian computation and an adaptive population Monte Carlo sampler, comparing observed and simulated datasets through principal-component summary statistics at five heights above the limb. The inferred posterior constrains effective population-level properties of the spicules that dominate the observed Mg II k variability and height dependence. These constraints provide a route to connect off-limb spectroscopy with forthcoming spectropolarimetric diagnostics of the chromosphere--corona interface.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"33 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149209116","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Vertical gradients of Galactic rotation from Gaia: The limiting-cone and comparison models","authors":"Łukasz Bratek,Joanna Jałocha,Szymon Sikora,Natalia Woźniak","doi":"10.1051/0004-6361/202660820","DOIUrl":"https://doi.org/10.1051/0004-6361/202660820","url":null,"abstract":"Vertical variation of Galactic rotation constrains mass geometry beyond the mid-plane rotation curve, but Gaia measures stellar streaming, not the circular speed associated with the radial force. We distinguish the streaming, Jeans, and conditional mass-model declines ̊m S ), (G_ ̊m J ), and (G_ ̊m M ). For Gaia DR3 over (4łeq Rłeq8,̨pc) and (0łeq|Z|łeq2.4,̨pc), unrestricted-sample streaming estimates span (33)--(41, =40.910 =15.321 ) at (R_0=8.122,̨pc). There is therefore no universal vertical gradient: streaming is population-dependent, whereas a properly defined off-plane force decline can reduce the mass-distribution--rotation-curve degeneracy but is subject to explicit tracer, dynamical, weighting, and model assumptions. with (G_ ̊m S under the adopted common weight. A stationary axisymmetric Jeans reconstruction using one tracer weight for three means and six intrinsic covariances gives (G_ ̊m J the difference, (25.588 _ arises from second moments, radial pressure support, and velocity-ellipsoid tilt. Tracer density is the dominant quantified model systematic, giving approximately (10)--(21, =22.535) and (14.315, =1.107^ Conditional disk-only and disk-plus-sphere fields give (G_ ̊m M whereas finite near-azimuthal selections give (15.035)--(15.548, ) to (G_ ) within a fixed-shape family preserving the mid-plane curve gives (M_ /M_ despite different two-dimensional fields. Matching (G_ ̊m M ̊m J ̊m sphere ̊m disk +0.124 -0.112","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"4 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149209118","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Investigating X-ray emission from radio-detected broad- and narrow-line Seyfert 1 galaxies","authors":"Minhua Zhou,Minfeng Gu,Lei Xu,Mai Liao,ZhengXue Chang","doi":"10.1051/0004-6361/202661782","DOIUrl":"https://doi.org/10.1051/0004-6361/202661782","url":null,"abstract":"This paper presents a study of the X-ray emission for a sample of radio-detected (RD-) broad- and narrow-line Seyfert 1 galaxies (BLS1s and NLS1s). Our aim is to investigate the X-ray emission properties of early-stage accretion activity or early jets in RD-NLS1s. By fitting XMM-Newton X-ray spectra and combining them with multi-band data from SDSS and FIRST, we conducted a statistical comparative study on the X-ray emission and multi-band correlations of RD-NLS1s and RD-BLS1s. RD-NLS1s and RD-BLS1s show no significant difference in their soft X-ray blackbody temperatures, but RD-NLS1s exhibit steeper hard X-ray photon indices and optical-to-X-ray slopes (( ̊m ox )). Moreover, correlation analyses of various parameters reveal intrinsic differences in the X-ray emission between the two samples. For instance, at comparable optical luminosities, RD-NLS1s exhibit a higher ( α_ ̊m ox ) (i.e. weaker X-ray emission), marginally distinct dependencies between the radio luminosity and black hole mass in the fundamental plane, and different correlations between ( α_ ̊m ox ) and radio loudness. Based on the relationship between the UV luminosity and ( α_ ̊m ox ) in radio-quiet (RQ-) active galactic nuclei (AGNs), the estimated X-ray excess (( Δ α_ ̊m ox )) in both samples is positively correlated with the radio loudness. RQ-BLS1s generally display an X-ray excess (( Δ α_ ̊m ox < 0 )), whereas RQ-NLS1s tend to show an X-ray deficiency (( Δ α_ ̊m ox > 0 )). The Eddington ratio of RQ-NLS1s derived from X-ray luminosity is lower than that inferred from optical luminosity, further supporting their intrinsically weaker X-ray emission. These differences in X-ray emission between RD-NLS1s and RD-BLS1s may ultimately stem from the earlier evolutionary stage of NLS1s. Multi-variate linear fits among the radio luminosity, X-ray luminosity, and radio loudness for RD-NLS1s and RD-BLS1s support a multi-wavelength emission connection associated with jets.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"32 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149209045","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The Fast and Fourier: Using neural operators to speed up radiative modeling of protoplanetary disks","authors":"L. Welzel,M. K. McClure","doi":"10.1051/0004-6361/202662720","DOIUrl":"https://doi.org/10.1051/0004-6361/202662720","url":null,"abstract":"Edge-on protoplanetary disks provide a spatially resolved view of the vertical distribution of icy planetary building blocks, but inferring their relative abundances requires radiative-transfer (RT) modeling with multiple anisotropic scattering. Each such model costs 10^1-10^3 CPU hours, which precludes principled Bayesian inference and homogeneous, population-scale analyses. We develop and validate a fast and reusable surrogate for Bayesian inference with ice-bearing edge-on disk models. We trained a Fourier neural operator on a grid of spectra. The network maps disk parameters and analytic physical input fields to the spectrum, using mixed-resolution spectra. We used the surrogate in an explicit-likelihood nested sampler. Then we validated it on held-out simulations and synthetic recovery tests with Test of Accuracy with Random Points (TARP) coverage tests. Finally, we used it to retrieve the disk structure and ice abundances of ESO-Hα 569 from its spectral energy distribution (SED). RADMC-3D The surrogate successfully reproduces the spectra with a median error of fwdPerSpecQFifty%. We recover synthetic parameters without detectable bias and with nominal coverage. For ESO-Hα 569, the posterior favors a massive (M_ RADMC-3D ̊m gas = nearly edge-on (i= . Its ice abundances and cavity size remain weakly constrained by broadband data alone. The marginal spectrum-evaluation speed-up is approximately 10^9--10^10. disk consistent with the image-plus-SED model of wolff2017hubblespacetelescope Neural-operator emulation makes full posterior inference feasible within the adopted model and training prior. Scientifically important posterior points should still be checked with high-fidelity RT models. By dramatically decreasing the evaluation time, for the first time this approach enables homogeneous population studies of ices in disks, which can be capitalized on for new JWST surveys to map the range of compositions within planetary nurseries.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"13 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149209109","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"BlackHoleWeather – Spin-coupled chaotic cold accretion across the meso scale: Kinematics and variability","authors":"Olmo Piana,Massimo Gaspari,Vieri Cammelli,Filippo Barbani,Davide M. Brustio,Giovanni Stel,Valeria Olivares,Ashkbiz Danehkar,Pasquale Temi,Roberto Serafinelli,Francesco Salvestrini,Filippo M. Maccagni,Francesco Tombesi","doi":"10.1051/0004-6361/202661140","DOIUrl":"https://doi.org/10.1051/0004-6361/202661140","url":null,"abstract":"Supermassive black hole (SMBH) spin records the vector history of accretion. In chaotic cold accretion (CCA), this history is set by clouds and filaments whose torques can add coherently, cancel, or reverse before reaching the horizon-scale closure. We test whether halo stirring regulates SMBH spin by changing the radial continuity and torque coherence of the meso-scale accretion bridge. We focus on spin evolution, jet-axis reorientation, accretion variability, and CCA kinematics. ̊m kpc ) box, reaching sub-parsec resolution, including SMBH spin-coupled jet feedback. All runs use the Hybrid SMBH spin model validated in a companion paper. Two simulations maintain continuously driven solenoidal turbulence, while two matched controls let the same initial turbulent field decay. -1 ) during coherent retrograde episodes. The same split appears in the power spectra and k-plots: connected rain is associated with a greater absolute low-frequency accretion power and produces narrower, phase-ordered kinematics, while persistent stirring steepens the high-frequency damping and broadens the gas velocity loci across phases. All runs remain CCA-like, with turbulent Taylor numbers of ( łesssim1). Ta_t Persistent halo stirring therefore regulates SMBH spin and jet-axis evolution primarily by controlling the radial continuity and torque coherence of the meso-scale CCA feeding bridge.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"53 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149210364","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"CosmoForge. I. A unified framework for quadratic maximum likelihood power spectrum estimation and pixel-based likelihood analysis","authors":"G. Galloni,L. Pagano","doi":"10.1051/0004-6361/202661478","DOIUrl":"https://doi.org/10.1051/0004-6361/202661478","url":null,"abstract":"Optimal power spectrum estimation on the largest angular scales of the cosmic microwave background relies on the quadratic maximum likelihood (QML) estimator. Existing public implementations, however, each address only a subset of the problem, and none combines power spectrum estimation with a self-consistent pixel-space likelihood within a single framework. We present ̧f, a public Python framework that unifies QML power spectrum estimation and pixel-based Gaussian likelihood evaluation for spin-0 and spin-2 fields on the sphere, with general (non-diagonal) noise covariances. The framework is split into three installable packages: ç (infrastructure), (łmax^4) for arbitrary noise covariances, with (Fisher and QML estimation), and (pixel-space likelihood). A common interface exposes two interchangeable computation bases -- a harmonic basis built on the Sherman--Morrison--Woodbury identity and a direct pixel-space basis -- selecting whichever is cheaper for the configuration at hand. Exact algorithmic optimisations reduce the Fisher cost to mathcal O Numba JIT compilation of the hot kernels and MPI parallelisation of the likelihood scan. ̧f reproduces the Planck low-ell Fortran reference implementation across both the QML and pixel-space likelihood pipelines, consistently with double-precision arithmetic. Native multipole binning and three output normalisations (deconvolved, de-correlated, and window-convolved) are exposed through a single code path, and the same covariance infrastructure powers both QML estimation and likelihood evaluation. ̧f offers a general-purpose, modular, and validated tool for the optimal analysis of large-scale data on the sphere. It is publicly available, pip-installable, and extensible to observables other than the cosmic microwave background.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"10 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149209021","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"TESS flares and chromospheric variability in the Pleiades, the Hyades, and Praesepe","authors":"A. Görgei,K. Vida,B. Seli,K. Oláh,P. Sági,B. Schmercz,R. M. Roettenbacher,Zs. Kővári","doi":"10.1051/0004-6361/202661417","DOIUrl":"https://doi.org/10.1051/0004-6361/202661417","url":null,"abstract":"Magnetic activity is a result of the interaction between rotation and dynamo processes in cool stars with outer convection zones. Since open cluster members share a common age, distance, and chemical composition, they provide an opportunity for studying the magnetic activity of cool stars in a controlled astrophysical context. We used photometric observations with a cadence of 120 s from the Transiting Exoplanet Survey Satellite (TESS) to study the flare activity of stars in three open clusters with different ages: the Pleiades (100,Myr), the Hyades (700,Myr), and Praesepe (700,Myr). We used the Ohio State Multi-Object Spectrograph (OSMOS) at MDM Observatory with the goal of identifying coronal mass ejections (CMEs) on stars in the Pleiades and Praesepe. We investigated the flaring characteristics of the cluster members using the TESS light curves: we identified the flares and then divided the dataset into different categories based on the effective temperature of the flaring stars and the amplitude of their light curves after flare removal. We calculated the flare energies and investigated the flare frequency distributions of each previously defined group. We studied the dynamic spectra of the Hα line and its environment for the stars of the Pleiades and Praesepe to search for an indication of CMEs. In order to quantify temporal variations in the line strength, we measured the Hα chromospheric activity indices for each spectrum. The power-law indices of the flare frequency distributions obtained in our analysis span the 1.8-2.8 range. We found the highest flare rates in the Pleiades for all investigated spectral types. Our results show that the flare rate of M dwarfs is similar in the Pleiades and the Hyades, while the flare rate for K-type stars in the Pleiades is higher by an order of magnitude. Our analysis reveals that the flare rate in M stars changes with their effective temperature: the rate is highest for T_ ̊m eff ∼3200-3300,K (which coincides with the transition between partially and fully convective stars), with a smooth decrease in flare rate toward cooler and hotter M dwarfs. We detected no CME signals in the OSMOS spectra, and we used this information to place an upper limit on the CME rate.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"11 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149209022","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Broadband non-thermal emission predictions based on 3D simulations of supernova explosions within active galactic nuclei jets","authors":"B. Longo,V. Bosch-Ramon,M. Perucho,J. M. Martí","doi":"10.1051/0004-6361/202661880","DOIUrl":"https://doi.org/10.1051/0004-6361/202661880","url":null,"abstract":"Thermonuclear and core-collapse supernovae are statistically expected to happen within extragalactic jets, as these jets cross the inner regions of their host galaxies, and supernova ejecta--jet interactions can potentially lead to strong non-thermal activity. We model the non-thermal emission from a supernova interacting with a jet on kiloparsec scales, using detailed numerical simulations of the interaction. Using a post-processing method, we applied a non-thermal model of the acceleration and transport of electron and their synchrotron and inverse Compton emissions, simplified and tuned for flexibility and computational speed, to the results of a three-dimensional relativistic hydrodynamics simulation of the ejecta of a supernova interacting with an extragalactic jet. For typical magnetic field strengths, a jet power 10^ 44 , , , and an electron energy distribution characteristic of diffusive shock acceleration, we predict: synchrotron emission that peaks in X-rays but reaches up to 100 MeV, with an overall luminosity of a few times 10^ 41 and emission from inverse Compton scattering mostly off galactic infrared photons, peaking at ∼ 1 TeV and with a luminosity up to ∼ 10^ 40 We also computed the evolution of the emission, and the distribution of the flux in the sky at its maximum, for five different energy bands: radio, optical, X-rays, high-energy and very high-energy γ-rays. The emission is roughly steady on a few 1000 yr timescales, with an extension on arcsec scales for a source in the local universe. For intermediate jet powers, radio, optical and X-ray fluxes from supernova ejecta-jet interactions may be detectable for distances łesssim 100 Mpc. The non-thermal luminosity budget and local conditions associated with these interactions could be enough to explain knots seen in kiloparsec scale jets at different energies. These conditions might also be suitable for the production of heavy ultra high-energy cosmic rays, but photon and neutrino generation from hadronic processes would be minor on kiloparsec scales. The leptonic γ-ray fluxes are modest but might non-negligibly contribute in TeV for the nearest or more powerful jet sources.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"25 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149209044","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The Quasar Feedback Survey: Ionised outflows in type 2 QSOs with MUSE data","authors":"M. Bianchin,C. M. Harrison,T. Costa,V. Mainieri,R. A. Riffel,G. Venturi,D. Kakkad,C. Ramos Almeida,P. H. Cezar,S. Ward,A. Girdhar,S. Molyneux,L. Ulivi,E. P. Farina,J. Mullaney,F. Arrigoni Battaia","doi":"10.1051/0004-6361/202661661","DOIUrl":"https://doi.org/10.1051/0004-6361/202661661","url":null,"abstract":"The impact of feedback from active supermassive black holes on their host galaxies is a key phenomenon in understanding galaxy evolution. We study ionised gas properties in a sample of 18 luminous (log L_ ̊m bol obscured Quasi-stellar objects (QSOs) in the nearby Universe (0.085<z<0.2$) observed with VLT/MUSE as part of the multi-wavelength Quasar Feedback Survey (QFeedS) and with VLA at low- and high-resolution data , 1 and 0.3 respectively . Our main goal is to characterise the disturbed gas kinematics in this galaxy sample. We compare the outflow-related quantities with values reported in the literature and investigate possible correlations between the outflows and other properties of the ionised gas, such as the electron density. We adopt a non-parametric approach to characterise the ionised gas kinematics, traced by the 4711,4740 doublet, only observable in the integrated r=1.5 <27700, leading to 0.03$< _ emission line, and use W_80 measured from the unresolved nuclear spectra as a threshold to identify outflow-dominated spaxels. A qualitative comparison between the radio and the W_80 maps shows that, in general, the peak of the radio coincides with the peak of the W_80. is used as a proxy for the ionised gas mass, and the outflow-related properties are obtained in two different ways: the global, using flux-weighted velocities and radii and the peak, which relies on radial profiles. We correct the flux for extinction using the Balmer decrement. We take advantage of the MUSE sensitivity and use the iv spectra, to measure the electron density in each galaxy. We obtain 500<n_ ̊m e cm^ -3 M ̊m out / ̊m M_⊙ yr^ -1 <4.17 and 39< _ E ̊m kin / ̊m -1 <42$. Our results emphasize the importance of accurate electron density determination, leading to a difference of 1 dex in the outflow rates and kinetic powers. We observe a positive correlation between n_e and $V_ ̊m out , interpreted as compression of the gas at higher velocities. This correlation should be further investigated at other luminosity and redshift ranges, but it can inform future outflow simulation studies.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"22 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149209046","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}