J/A+A/696/A206ivo://CDS.VizieR/J/A+A/696/A206doi:10.26093/cds/vizier.36960206CDSVasquez-Bustos P.Argudo-Fernandez M.Boquien M.Castillo-Baeza N.,Castillo-Rencoret A.Ariza-Quintana D.2025-06-02T20:01:10Z2025-04-25T15:28:18ZCDS support team

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

cds-question@unistra.frgalaxiescatalogsgalaxy-classification-systemsThere are still many open questions in the complex process of galaxy evolution during interactions, as each stage is characterized by different periods of star formation. We aim to better understand the processes triggered in galaxies by interactions. We consider low-density environments in which in-situ interaction between the members is the main process that drives evolution. In this work we carry out an analysis of star-formation and nuclear activity in the different stages during a galaxy merger identified in isolated systems (isolated galaxies, isolated pairs, and isolated triplets) using integral field spectroscopy from the SDSS-IV/MaNGA project. We classify galaxies into close pairs, pre-mergers, mergers, and post-mergers (including galaxies with post-starburst spectroscopic features), for a total sample of 137 galaxies. We constrained their star formation history from spectro-photometric SED fitting with CIGALE, and used spatially resolved WHAN diagrams, with other MaNGA data products to explore if there is any connection of their physical with their merging stage. In general, galaxies show characteristic properties intrinsically related to each stage of the merger process. Galaxies in the merger and post-merger stages present higher star formation activity (measured by their integrated sSFR). In the merger stage, the fraction of strong AGN spaxels is comparable to the fraction of spaxels with pure star- formation emission, with no difference between AGN activity in close pairs and strongly interacting galaxies with the same stellar mass. Our results support the scenario where galaxy interactions triggers star-formation and nuclear activity on galaxies. Nonetheless, AGN has a minor role in quenching galaxies following a merger, as AGN feedback might not have had sufficient time to inhibit star formation. In addition, we found that the quenching process in post-mergers galaxies with post-starburst emission is happening outside-in, being an observational proof of the effect of interactions on the quenching process. The transforming processes after a recent major galaxy interaction may happen slowly on isolated environments, where the system evolves in a common dark matter halo without any perturbation of external galaxies.2025A&A...696A.206Vhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/696/A206CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/578/A110 : Isolated galaxies, pairs and tripletsJ/MNRAS/476/3661 : Morphology of SDSS galaxies (Dominguez-Sanchez+, 2018)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/696/A206https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/696/A206http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/696/A206https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/696/A206https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/696/A206http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/696/A206GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/696/A206/tabled1Physical properties, and morphology of galaxy mergersSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPlate-IFUPlate-IFU of MaNGA galaxiesmeta.id;meta.maincharcatalogueCatalogues from Argudo-Fernandez et al., 2015A&A...578A.110A, Cat. J/A+A/578/A110 (1)meta.codecharMember[cs-] Type of member in the system (2)meta.notecharMType[ETG LTG] Morphologycal T-type (3)phot.colorcharMergeStageMerger stage (4)meta.code;src.morphcharSFRStar-formation ratelog(solMass.yr**-1)phys.SFRdoublee_SFRStar-formation rate errorlog(solMass.yr**-1)stat.error;phys.SFRdoubleMStellar Masslog(solMass)phys.massdoublee_MStellar Mass errorlog(solMass)stat.errordouble