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dc.contributor.author Forte, Juan Carlos
dc.contributor.author Vega, Ema Irene
dc.contributor.author Faifer, Favio Raúl
dc.date.available 2018-06-13T15:07:04Z
dc.date.issued 2009-08
dc.identifier.citation Forte, Juan Carlos; Vega, Ema Irene; Faifer, Favio Raúl; The globular clusters-stellar haloes connection in early-type galaxies; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 397; 2; 8-2009; 1003-1020
dc.identifier.issn 0035-8711
dc.identifier.uri http://hdl.handle.net/11336/48507
dc.description.abstract This paper explores if, and to what an extent, the stellar populations of early-type galaxies can be traced through the colour distribution of their globular cluster (GC) systems. The analysis, based on a galaxy sample from the Virgo Advanced Camera for Surveys data, is an extension of a previous approach that has been successful in the cases of the giant ellipticals NGC 1399 and NGC 4486, and assumes that the two dominant GC populations form along diffuse stellar populations sharing the cluster chemical abundances and spatial distributions. The results show that (a) integrated galaxy colours can be matched to within the photometric uncertainties and are consistent with a narrow range of ages; (b) the inferred mass to luminosity ratios and stellar masses are within the range of values available in the literature; (c) most GC systems occupy a thick plane in the volume space defined by the cluster formation efficiency, total stellar mass and projected surface mass density. The formation efficiency parameter of the red clusters shows a dependency with projected stellar mass density that is absent for the blue globulars. In turn, the brightest galaxies appear clearly detached from that plane as a possible consequence of major past mergers; (d) the stellar mass–metallicity relation is relatively shallow but shows a slope change at M*≈ 1010 M⊙. Galaxies with smaller stellar masses show predominantly unimodal GC colour distributions. This result may indicate that less massive galaxies are not able to retain chemically enriched interstellar matter.
dc.format application/pdf
dc.language.iso eng
dc.publisher Wiley Blackwell Publishing, Inc
dc.rights info:eu-repo/semantics/openAccess
dc.rights.uri https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject Globular clusters: general
dc.subject Galaxies: haloes
dc.subject Galaxies: star clusters
dc.subject.classification Astronomía
dc.subject.classification Ciencias Físicas
dc.subject.classification CIENCIAS NATURALES Y EXACTAS
dc.title The globular clusters-stellar haloes connection in early-type galaxies
dc.type info:eu-repo/semantics/article
dc.type info:ar-repo/semantics/artículo
dc.type info:eu-repo/semantics/publishedVersion
dc.date.updated 2018-04-23T14:57:50Z
dc.journal.volume 397
dc.journal.number 2
dc.journal.pagination 1003-1020
dc.journal.pais Reino Unido
dc.journal.ciudad Londres
dc.description.fil Fil: Forte, Juan Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
dc.description.fil Fil: Vega, Ema Irene. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
dc.description.fil Fil: Faifer, Favio Raúl. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
dc.journal.title Monthly Notices of the Royal Astronomical Society
dc.relation.alternativeid info:eu-repo/semantics/altIdentifier/doi/https://dx.doi.org/10.1111/j.1365-2966.2009.15023.x
dc.relation.alternativeid info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/397/2/1003/972631
dc.conicet.fuente unificacion


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info:eu-repo/semantics/openAccess Excepto donde se diga explícitamente, este item se publica bajo la siguiente descripción: Creative Commons Attribution-NonCommercial-ShareAlike 2.5 Unported (CC BY-NC-SA 2.5)