J/A+A/701/A29ivo://CDS.VizieR/J/A+A/701/A29doi:10.26093/cds/vizier/bc-nx/lcjCDSPeluso G.Vulcani B.Radovich M.Moretti A.Poggianti B.M.Watson P.,Acharyya A.Lassen A.E.Gullieuszik M.Fritz J.Ignesti A.Tomicic N.,Delvecchio I.Khoram A.H.2026-08-03T06:57:28Z2025-09-01T17:11:39ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frastronomical-modelsactive-galactic-nucleichemical-abundancesIt has been reported that the gas-phase oxygen abundance of the circumnuclear regions around supermassive black holes (SMBHs) could be affected by the presence of an active galactic nucleus (AGN). However, there is currently no agreement on the processes behind this effect. Some studies have measured higher metallicities in the nuclear regions of AGN hosts compared to those of star-forming (SF) galaxies, while others have observed the opposite result. In this work, we explore whether the interplay between AGN activity and the Ram-Pressure Stripping (RPS) acting in the cluster environment can alter the metallicity distributions of nearby (z<0.07) galaxies. We measure the spatially resolved gas-phase oxygen abundances of 10 AGN hosts experiencing RPS from the GASP survey and 52 AGN hosts located in the field and hence undisturbed by the RP drawn from the MaNGA DR15. To measure the oxygen abundances in SF and AGN-ionized regions, we present a set of strong emission line (SEL) calibrators obtained through an indirect method in which the [OIII]/[SII] and [NII]/[SII] line ratios, observed and predicted from Cloudy photoionization models, were matched through the code NebulaBayes. We find that the metallicity gradients of RPS and field AGN do not present significant differences within the errors, but that 2 out of the 10 RP-stripped AGNs show lower oxygen abundances at any given radius than the rest of the AGN sample. Overall, this result highlights that the interplay between AGN and RPS seems not to play a major role in shaping the metallicity distributions of stripped galaxies within 1.5 times the galaxy's effective radius (r<1.5Re), but larger samples are needed to draw more robust conclusions. By adding a control sample of SF galaxies, both experiencing RPS and in the field, we find that the AGN hosts are more metal-enriched than SF galaxies at any given radius, but that the steepness of the gradients in the nuclear regions (r<0.5Re) is higher in AGN hosts than in SF galaxies. Particularly, AGN hosts show a metal enrichment in the nuclear regions ~=1.8-2.3 times higher than the enhancement in the disk at r~1.25Re, regardless of the host galaxy's stellar mass. These results favor the hypothesis that the AGN activity is causing metal pollution in the galaxy's nuclear regions.2025A&A...701A..29Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/701/A29CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/701/A29https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/701/A29http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/701/A29https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/701/A29https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/701/A29http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/701/A29GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/701/A29/agngridsPhotoionization models generated using the CLOUDY v17.02 code, ionization comes from the radiation of an active galactic nucleus (AGN)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintnH[100] Gas densitycm**-3phys.columnDensityfloatalpha[-2.0] AGN continuum slope (1)stat.fit.paramfloatdg[-0.52] Dust-to-gas ratio (G2)phys.mass;arith.ratiofloatlogU[-4.0/-0.5] Ionization parameter (G3)phys.ionizParamfloatlogZ[-1.0/0.7] Gas-phase metallicity (G4)phys.abund.ZfloatOIIaPredicted emission line flux relative to H{beta} for [OII]{lambda}3726phot.flux;arith.ratio;spect.linedoubleOIIbPredicted emission line flux relative to H{beta} for [OII]{lambda}3729phot.flux;spect.line;arith.ratiodoubleOIIPredicted emission line flux relative to H{beta} for [OII]{lambda}{lambda}3726,29phot.flux;arith.ratio;spect.linedoubleHaPredicted emission line flux relative to H{beta} for H{alpha}{lambda}6563phot.flux;spect.line;arith.ratiodoubleOIIIbPredicted emission line flux relative to H{beta} for [OIII]{lambda}5007phot.flux;spect.line;arith.ratiodoubleOIPredicted emission line flux relative to H{beta} for [OI] {lambda}6300phot.flux;arith.ratio;spect.linedoubleNIIbPredicted emission line flux relative to H{beta} for [NII] {lambda}6584phot.flux;arith.ratio;spect.linedoubleSIIaPredicted emission line flux relative to H{beta} for [SII] {lambda}6716phot.flux;arith.ratio;spect.linedoubleSIIbPredicted emission line flux relative to H{beta} for [SII] {lambda}6731phot.flux;arith.ratio;spect.linedoubleSIIPredicted emission line flux relative to H{beta} for [SII] {lambda}{lambda}6716,31phot.flux;spect.line;arith.ratiodoubleJ/A+A/701/A29/sfgridsPhotoionization models generated using the CLOUDY v17.02 code, ionization comes from the star forming galaxies (SF)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAge[4000000] Stellar ageyrtime.agedoublenH[100] Gas densitycm**-3phys.columnDensityfloatdg[-0.52] Dust-to-gas ratio (G2)phys.mass;arith.ratiofloatlogU[-4.0/-1.0] Ionization parameter (G3)phys.ionizParamfloatlogZ[-2.0/0.5] Gas-phase metallicity (G4)phys.abund.ZfloatOIIaPredicted emission line flux relative to H{beta} for [OII]{lambda}3726phot.flux;arith.ratio;spect.linedoubleOIIbPredicted emission line flux relative to H{beta} for [OII]{lambda}3729phot.flux;arith.ratio;spect.linedoubleOIIPredicted emission line flux relative to H{beta} for [OII]{lambda}{lambda}3726,29phot.flux;arith.ratio;spect.linedoubleHaPredicted emission line flux relative to H{beta} for H{alpha}{lambda}6563phot.flux;arith.ratio;spect.linedoubleOIIIbPredicted emission line flux relative to H{beta} for [OIII]{lambda}5007phot.flux;arith.ratio;spect.linedoubleOIPredicted emission line flux relative to H{beta} for [OI] {lambda}6300phot.flux;arith.ratio;spect.linedoubleNIIbPredicted emission line flux relative to H{beta} for [NII] {lambda}6584phot.flux;spect.line;arith.ratiodoubleSIIaPredicted emission line flux relative to H{beta} for [SII] {lambda}6716phot.flux;arith.ratio;spect.linedoubleSIIbPredicted emission line flux relative to H{beta} for [SII] {lambda}6731phot.flux;spect.line;arith.ratiodoubleSIIPredicted emission line flux relative to H{beta} for [SII] {lambda}{lambda}6716,31phot.flux;spect.line;arith.ratiodoubleJ/A+A/701/A29/compgridPhotoionization models generated using the CLOUDY v17.02 code, composite models (AGN + SF)recnoRecord number assigned by the VizieR team. 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