The physical properties and evolution of the interacting system AM 1204−292

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dc.contributor.authorRosa, Deise Aparecida
dc.contributor.authorOliveira Filho, Irapuan Rodrigues de
dc.contributor.authorKrabbe, Angela Cristina
dc.contributor.authorMilone, Andre de Castro
dc.contributor.authorCarvalho, Sarita Pereira de
dc.date.accessioned2025-04-08T18:29:20Z
dc.date.available2025-04-08T18:29:20Z
dc.date.issued22021
dc.description.abstractWe investigate interaction effects in the stellar and gas kinematics, stellar population, and ionized gas properties of the interacting galaxy pair AM 1204−292,composed of NGC 4105 and NGC 4106. The data consist of long-slit spectra in the range 3000–7050 Å. The massive E3 galaxy NGC 4105 presents a flat stellar velocity profile, while the ionized gas is in strong rotation, suggesting an external origin. Its companion, NGC 4106, shows asymmetries in the radial velocity field, likely due to the interaction. The dynamics of the interacting pair were modelled using the P-Gadget3 treepm/sph code, from which we show that the system has just passed the first perigalacticum, which triggered an outbreak of star formation, currently at full maximum. We characterized the stellar population properties using the stellar population synthesis code starlight and, on average, both galaxies are predominantly composed of old stellar populations. NGC 4105 has a slightly negative age gradient, comparable with that of the most massive elliptical galaxies, but a steeper metallicity gradient. The SB0 galaxy NGC 4106 presents smaller radial variations in both age and metallicity in comparison with intermediate-mass early-type galaxies. These gradients have not been disturbed by interaction, since the star formation happened very recently and was not extensive in mass. Electron density estimates for the pair are systematically higher than those obtained in isolated galaxies. The central O/H abundances were obtained from photoionization models in combination with emission-line ratios, which resulted in 12 + log(O/H) = 9.03 ± 0.02 and 12 + log(O/H) = 8.69 ± 0.05 for NGC 4105 and NGC 4106, respectively.
dc.description.physical17 p.
dc.description.sponsorshipCoordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)
dc.description.sponsorshipFundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)
dc.description.sponsorshipConselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)
dc.description.sponsorshipFinanciadora de Estudos e Projetos (Finep)
dc.description.uriCNPq ( 313489/2018-1 and 311331/2017-3) FAPESP ( 2016/21532-9; 2011/13250-0, 2013/17247-9 and 2014/10489-0) FINEP (01.10.0661-00)
dc.format.mimetypePDF
dc.identifier.affiliationUniversidade do Vale do Paraíba
dc.identifier.affiliationInstituto Nacional de Pesquisas Espaciais
dc.identifier.bibliographicCitationROSA, Deise Aparecida et al. The physical properties and evolution of the interacting system AM 1204−292. Monthly Notices of the Royal Astronomical Society, v. 501, n. 3, p. 3750-3766, 2021. Disponível em:
dc.identifier.doi10.1093/mnras/staa3850
dc.identifier.urihttps://repositorio.univap.br/handle/123456789/827
dc.language.isoen_US
dc.publisherRoyal Astronomical Society
dc.rights.holderMonthly Notices of the Royal Astronomical Society
dc.subject.keywordGalaxies: abundances
dc.subject.keywordGalaxies: formation
dc.subject.keywordGalaxies: groups
dc.subject.keywordGalaxies: stellar content
dc.titleThe physical properties and evolution of the interacting system AM 1204−292
dc.typeArtigos de Periódicos

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