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dc.contributor.authorHernán Caballero, Antonio
dc.contributor.authorAlonso Herrero, Almudena
dc.contributor.authorPérez-González, Pablo G.
dc.contributor.authorCardiel, Nicolás
dc.contributor.authorCava, Antonio
dc.contributor.authorFerreras, Ignacio
dc.contributor.authorBarro, Guillermo
dc.contributor.authorTresse, Laurence
dc.contributor.authorDaddi, Emanuele
dc.contributor.authorCenarro, Javier
dc.contributor.authorConselice, Christopher J.
dc.contributor.authorGuzmán, Rafael
dc.contributor.authorGallego, Jesús
dc.contributor.otherUniversidad de Cantabriaes_ES
dc.date.accessioned2014-06-10T13:13:11Z
dc.date.available2014-06-10T13:13:11Z
dc.date.issued2013-09
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.urihttp://hdl.handle.net/10902/4806
dc.description.abstractWe report on results from the analysis of a stellar mass-selected (log (M*/M⊙) ≥ 9.0) sample of 1644 galaxies at 0.65 < z < 1.1 with ultradeep (mAB < 26.5) optical medium-band (R ∼ 50) photometry from the Survey for High-z Absorption Red and Dead Sources (SHARDS). The spectral resolution of SHARDS allows us to consistently measure the strength of the 4000 Å spectral break [Dn(4000), an excellent age indicator for the stellar populations of quiescent galaxies] for all galaxies at z ∼ 0.9 down to log (M*/M⊙) ∼ 9. The Dn(4000) index cannot be resolved from broad-band photometry, and measurements from optical spectroscopic surveys are typically limited to galaxies at least 10 times more massive. When combined with the rest-frame U − V colour, (U − V)r, Dn(4000) provides a powerful diagnostic of the extinction affecting the stellar population that is relatively insensitive to degeneracies with age, metallicity or star formation history. We use this novel approach to estimate de-reddened colours and light-weighted stellar ages for individual sources. We explore the relationships linking stellar mass, (U − V)r, and Dn(4000) for the sources in the sample, and compare them to those found in local galaxies. The main results are: (a) both Dn(4000) and (U − V)r correlate with M*. The dispersion in Dn(4000) values at a given M* increases with M*, while the dispersion for (U − V)r decreases due to the higher average extinction prevalent in massive star-forming galaxies. (b) For massive galaxies, we find a smooth transition between the blue cloud and red sequence in the intrinsic U − V colour, in contrast with other recent results. (c) At a fixed stellar age, we find a positive correlation between extinction and stellar mass. (d) The fraction of sources with declining or halted star formation increases steeply with the stellar mass, from ∼5 per cent at log (M*/M⊙) = 9.0–9.5 to ∼80 per cent at log (M*/M⊙) > 11, in agreement with downsizing scenarios.es_ES
dc.format.extent17 p.es_ES
dc.language.isoenges_ES
dc.publisherOxford University Presses_ES
dc.publisherRoyal Astronomical Societyes_ES
dc.rights© 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society*
dc.sourceMonthly Notices of the Royal Astronomical Society, vol. 434, iss.3, Pp.2136-2152 (2013)es_ES
dc.subject.otherGalaxies: evolutiones_ES
dc.subject.otherGalaxies: fundamental parameterses_ES
dc.subject.otherGalaxies: high-redshiftes_ES
dc.subject.otherGalaxies: statisticses_ES
dc.subject.otherGalaxies: stellar contentes_ES
dc.subject.otherInfrared: galaxieses_ES
dc.titleSHARDS: stellar populations and star formation histories of a mass-selected sample of 0.65 < z < 1.1 galaxieses_ES
dc.typeinfo:eu-repo/semantics/articlees_ES
dc.relation.publisherVersionhttp://dx.doi.org/10.1093/mnras/stt1165es_ES
dc.rights.accessRightsopenAccesses_ES
dc.identifier.DOI10.1093/mnras/stt1165
dc.type.versionpublishedVersiones_ES


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