Dynamical versus stellar masses of ultracompact dwarf galaxies in the Fornax cluster☆

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dc.contributor.authorChilingarian, Igor V.
dc.contributor.authorMieske, Steffen
dc.contributor.authorHilker, Michael
dc.contributor.authorInfante, Leopoldo
dc.date.accessioned2025-01-21T00:02:20Z
dc.date.available2025-01-21T00:02:20Z
dc.date.issued2011
dc.description.abstractThe origin of ultracompact dwarf (UCD) galaxies, compact extragalactic stellar systems, is still a puzzle for present galaxy formation models. We present the comprehensive analysis of high-resolution multi-object spectroscopic data for a sample of 24 Fornax cluster UCDs obtained with VLT with Fibre Large Array Multi Element Spectrograph (FLAMES). It comprises previously published data for 19 objects which we re-analysed, including 13 with available Hubble Space Telescope (HST) photometric data. Using Virtual Observatory technologies we found archival HST images for two more UCDs and then determined their structural properties. For all objects we derived internal velocity dispersions, stellar population parameters and stellar mass-to-light ratios (M/L)(*) by fitting individual simple stellar population (SSP) synthetic spectra convolved with a Gaussian against the observed spectra using the NBursts full spectral fitting technique. For 14 objects we estimated dynamical masses suggesting no dark matter (DM) in 12 of them and no more than 40 per cent DM mass fraction in the remaining two, in contrast to findings for several UCDs in the Virgo cluster. Some Fornax UCDs even have too high values of (M/L)(*) estimated using the Kroupa stellar initial mass function (IMF) resulting in negative formally computed DM mass fractions. The objects with too high (M/L)(*) ratios compared to the dynamical ones have relatively short dynamical relaxation time-scales, close to the Hubble time or below. We therefore suggest that their lower dynamical ratios (M/L)(dyn) are caused by low-mass star depletion due to dynamical evolution. Overall, the observed UCD characteristics suggest at least two formation channels: tidal threshing of nucleated dwarf galaxies for massive UCDs (similar or equal to 108 M-circle dot), and a classical scenario of red globular cluster formation for lower-mass UCDs (less than or similar to 107 M-circle dot).
dc.fuente.origenWOS
dc.identifier.doi10.1111/j.1365-2966.2010.18000.x
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1111/j.1365-2966.2010.18000.x
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/95420
dc.identifier.wosidWOS:000289159100014
dc.issue.numero3
dc.language.isoen
dc.pagina.final1638
dc.pagina.inicio1627
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectgalaxies: dwarf
dc.subjectgalaxies: elliptical and lenticular, cD
dc.subjectgalaxies: evolution
dc.subjectgalaxies: kinematics and dynamics
dc.subjectgalaxies: stellar content
dc.subject.ods09 Industry, innovation and infrastructure
dc.subject.odspa09 Industria, innovación e infraestructura
dc.titleDynamical versus stellar masses of ultracompact dwarf galaxies in the Fornax cluster☆
dc.typeartículo
dc.volumen412
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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