Abundance ratios and IMF slopes in the dwarf elliptical galaxy NGC 1396 with MUSE

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dc.contributor.authorMentz, J. J.
dc.contributor.authorLa Barbera, F.
dc.contributor.authorPeletier, R. F.
dc.contributor.authorFalcon-Barroso, J.
dc.contributor.authorLisker, T.
dc.contributor.authorvan de Ven, G.
dc.contributor.authorLoubser, S. I.
dc.contributor.authorHilker, M.
dc.contributor.authorSanchez-Janssen, R.
dc.contributor.authorNapolitano, N.
dc.contributor.authorCantiello, M.
dc.contributor.authorCapaccioli, M.
dc.contributor.authorNorris, M.
dc.contributor.authorPaolillo, M.
dc.contributor.authorSmith, R.
dc.contributor.authorBeasley, M. A.
dc.contributor.authorLyubenova, M.
dc.contributor.authorMunoz, R.
dc.contributor.authorPuzia, T.
dc.date.accessioned2025-01-23T21:27:21Z
dc.date.available2025-01-23T21:27:21Z
dc.date.issued2016
dc.description.abstractDeep observations of the dwarf elliptical (dE) galaxy NGC 1396 (M-V = -16.60, Mass similar to 4 x 10(8) M-circle dot), located in the Fornax cluster, have been performed with the Very Large Telescope/Multi Unit Spectroscopic Explorer spectrograph in the wavelength region from 4750 to 9350 angstrom. In this paper, we present a stellar population analysis studying chemical abundances, the star formation history (SFH) and the stellar initial mass function (IMF) as a function of galactocentric distance. Different, independent ways to analyse the stellar populations result in a luminosity-weighted age of similar to 6 Gyr and a metallicity [Fe/H]similar to -0.4, similar to other dEs of similar mass. We find unusually overabundant values of [Ca/Fe]similar to+0.1, and underabundant Sodium, with [Na/Fe] values around -0.1, while [Mg/Fe] is overabundant at all radii, increasing from similar to+0.1 in the centre to similar to+0.2 dex. We notice a significant metallicity and age gradient within this dwarf galaxy. To constrain the stellar IMF of NGC 1396, we find that the IMF of NGC 1396 is consistent with either a Kroupa-like or a top-heavy distribution, while a bottom-heavy IMF is firmly ruled out. An analysis of the abundance ratios, and a comparison with galaxies in the Local Group, shows that the chemical enrichment history of NGC 1396 is similar to the Galactic disc, with an extended SFH. This would be the case if the galaxy originated from a Large Magellanic Cloud-sized dwarf galaxy progenitor, which would lose its gas while falling into the Fornax cluster.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stw2129
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stw2129
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/101379
dc.identifier.wosidWOS:000393566000042
dc.issue.numero3
dc.language.isoen
dc.pagina.final2838
dc.pagina.inicio2819
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectgalaxies: abundances
dc.subjectgalaxies: dwarf
dc.subjectgalaxies: evolution
dc.subjectgalaxies: individual: (NGC 1396)
dc.subjectgalaxies: stellar content
dc.titleAbundance ratios and IMF slopes in the dwarf elliptical galaxy NGC 1396 with MUSE
dc.typeartículo
dc.volumen463
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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