GASP XXXIII. The ability of spatially resolved data to distinguish among the diferent physical mechanisms afecting galaxies in low-density environments

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dc.contributor.authorVulcani, Benedetta
dc.contributor.authorPoggianti, Bianca M.
dc.contributor.authorMoretti, Alessia
dc.contributor.authorFranchetto, Andrea
dc.contributor.authorBacchini, Cecilia
dc.contributor.authorMcgee, Sean
dc.contributor.authorJaffé, Yara L.
dc.contributor.authorMingozzi, Matilde
dc.contributor.authorWerle, Ariel
dc.contributor.authorTomičić, Neven
dc.contributor.authorFritz, Jacopo
dc.contributor.authorBettoni, Daniela
dc.contributor.authorWolter, Anna
dc.contributor.authorGullieuszik, Marco
dc.date.accessioned2022-11-30T02:47:09Z
dc.date.available2022-11-30T02:47:09Z
dc.date.issued2021
dc.description.abstractGalaxies inhabit a wide range of environments and therefore are affected by different physical mechanisms. Spatially resolved maps combined with the knowledge of the hosting environment are very powerful for classifying galaxies by physical process. In the context of the GAs Stripping Phenomena in galaxies (GASP), we present a study of 27 non-cluster galaxies: 24 of them were selected for showing asymmetries and disturbances in the optical morphology, suggestive of gas stripping; 3 of them are passive galaxies and were included to characterize the final stages of galaxy evolution. We therefore provide a panorama of the different processes taking place in low-density environments. The analysis of VLT/MUSE data allows us to separate galaxies into the following categories: galaxy–galaxy interactions (2 galaxies), mergers (6), ram pressure stripping (4), cosmic web stripping (2), cosmic web enhancement (5), gas accretion (3), and starvation (3). In one galaxy we identify the combination of merger and ram pressure stripping. Only 6/27 of these galaxies have just a tentative classification. We then investigate where these galaxies are located on scaling relations determined for a sample of undisturbed galaxies. Our analysis shows the successes and limitations of a visual optical selection in identifying the processes that deplete galaxies of their gas content and probes the power of IFU data in pinning down the acting mechanism.en_ES
dc.facultadFacultad de Cienciasen_ES
dc.file.nameVulcani_Gas2021.pdf
dc.identifier.doihttps://doi.org/10.3847/1538-4357/abf655
dc.identifier.urihttp://repositoriobibliotecas.uv.cl/handle/uvscl/7587
dc.languageen
dc.publisherAmerican Astronomical Society (Aas)
dc.rights© 2021. The American Astronomical Society. All rights reserved.
dc.sourceThe Astrophysical Journal
dc.subjectGALAXIESen_ES
dc.subjectFIELD GALAXIESen_ES
dc.subjectGALAXY EVOLUTIONen_ES
dc.subjectGALAXY FORMATIONen_ES
dc.subjectGALAXY GROUPSen_ES
dc.subjectSTAR FORMATIONen_ES
dc.subjectSTELLAR KINEMATICSen_ES
dc.titleGASP XXXIII. The ability of spatially resolved data to distinguish among the diferent physical mechanisms afecting galaxies in low-density environments
dc.typeArticulo
uv.departamentoInstituto de Fisica y Astronomia

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