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Por favor, use este identificador para citar o enlazar a este item: http://hdl.handle.net/10261/140205
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dc.contributor.authorCava, Antonio-
dc.contributor.authorPérez-González, Pablo G.-
dc.contributor.authorAlonso-Herrero, A.-
dc.contributor.authorCenarro, A. J.-
dc.contributor.authorDomínguez Sánchez, Helena-
dc.contributor.authorEsquej, Pilar-
dc.contributor.authorGallego, Jesús-
dc.contributor.authorHernán-Caballero, Antonio-
dc.contributor.authorHuertas-Company, M.-
dc.contributor.authorRodríguez-Espinosa, J. M.-
dc.contributor.authorVillar, Víctor-
dc.date.accessioned2016-11-15T09:54:00Z-
dc.date.available2016-11-15T09:54:00Z-
dc.date.issued2015-
dc.identifierdoi: 10.1088/0004-637X/812/2/155-
dc.identifiere-issn: 1538-4357-
dc.identifierissn: 0004-637X-
dc.identifier.citationAstrophysical Journal 812(2): 155 (2015)-
dc.identifier.urihttp://hdl.handle.net/10261/140205-
dc.descriptionet al.-
dc.description.abstractIn this paper, we present a comprehensive analysis of star-forming galaxies (SFGs) at intermediate redshifts (z ∼ 1). We combine the ultra-deep optical spectro-photometric data from the Survey for High-z Absorption Red and Dead Sources (SHARDS) with deep UV-to-FIR observations in the GOODS-N field. Exploiting two of the 25 SHARDS medium-band filters, F687W17 and F823W17, we select [O ii] emission line galaxies at z ∼ 0.84 and z ∼ 1.23 and characterize their physical properties. Their rest-frame equivalent widths (EW([O ii])), line fluxes, luminosities, star formation rates (SFRs), and dust attenuation properties are investigated. The evolution of EW([O ii]) closely follows the SFR density evolution of the universe, with a trend of EW([O ii]) (1 + z) up to redshift z ≃ 1, followed by a possible flattening. The SF properties of the galaxies selected on the basis of their [O ii] emission are compared with complementary samples of SFGs selected by their MIR and FIR emission, and also with a general mass-selected sample of galaxies at the same redshifts. We demonstrate observationally that the UVJ diagram (or, similarly, a cut in the specific SFR) is only partially able to distinguish the quiescent galaxies from the SFGs. The SFR-M relation is investigated for the different samples, yielding a logarithmic slope ∼1, in good agreement with previous results. The dust attenuations derived from different SFR indicators (UV(1600), UV(2800), [O ii], IR) are compared and show clear trends with respect to both the stellar mass and total SFR, with more massive and highly star-forming galaxies being affected by stronger dust attenuation.-
dc.description.sponsorshipThe work of A.C. is supported by the STARFORM Sinergia Project funded by the Swiss National Science Foundation, and also benefited from a MERAC Funding and Travel Award. P.G.P.-G. acknowledges support from the Spanish Programa Nacional de Astronomía y Astrofísica under grants AYA2012-31277. A.V.G. acknowledges support from the ERC via an Advanced Grant under grant agreement no. 321323-NEOGAL. N.C. acknowledges support from the Spanish Ministry of Economy and Competitiveness under grant AYA2013-46724-P. A.A.H. and A.H.C. acknowledge financial support from the Spanish Ministry of Economy and Competitiveness through grant AYA2012-31447, which is partly funded by the FEDER program. A.J.C. is a Ramón y Cajal Fellow of the Spanish Ministry of Science and Innovation and acknowledges financial support from the Spanish Ministry of Economy and Competitiveness through grant AYA2012-30789, partly funded by the FEDER program.-
dc.relationinfo:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2013-46724-P-
dc.relationinfo:eu-repo/grantAgreement/EC/FP7/321323-
dc.relation.isversionofPublisher's version-
dc.rightsclosedAccess-
dc.subjectGalaxies: photometry-
dc.subjectQuasars: emission lines-
dc.subjectGalaxies: star formation-
dc.subjectGalaxies: high-redshift-
dc.subjectGalaxies: general-
dc.subjectGalaxies: evolution-
dc.titleSHARDS: A global view of the star formation activity at z∼ 0.84 and z∼ 1.23-
dc.typeartículo-
dc.identifier.doi10.1088/0004-637X/812/2/155-
dc.relation.publisherversionhttp://dx.doi.org/10.1088/0004-637X/812/2/155-
dc.date.updated2016-11-15T09:54:00Z-
dc.description.versionPeer Reviewed-
dc.language.rfc3066eng-
dc.contributor.funderEuropean Research Council-
dc.contributor.funderSwiss National Science Foundation-
dc.contributor.funderConsejo Superior de Investigaciones Científicas (España)-
dc.contributor.funderMinisterio de Ciencia e Innovación (España)-
dc.contributor.funderMinisterio de Economía y Competitividad (España)-
dc.contributor.funderEuropean Commission-
dc.relation.csicSí-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000781es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003339es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100004837es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003329es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000780es_ES
dc.type.coarhttp://purl.org/coar/resource_type/c_6501es_ES
item.openairetypeartículo-
item.grantfulltextnone-
item.cerifentitytypePublications-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.fulltextNo Fulltext-
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