IMF-Metallicity: A tigh local relation revealed by the CALIFA survey
Entity
UAM. Departamento de Física TeóricaPublisher
Institute of Physics PublishingDate
2015-06-18Citation
10.1088/2041-8205/806/2/L31
Astrophysical Journal Letters 806.2 (2015): L31
ISSN
2041-8205 (print); 2041-8213 (online)DOI
10.1088/2041-8205/806/2/L31Funded by
We acknowledge support from grants AYA2013-48226-C3-1 P and AYA2010-15081 from the Spanish MINECO. C.J.W. acknowledges support through the Marie Curie Career Integration Grant 303912. P.S.-B. acknowledges support from the Ramón y Cajal program, ATA2010-21322-C03-02 (MINECO). J.F.B. and Gvd.V. acknowledge the DAGAL network from the People Programme (Marie Curie Actions) of the European Unions Seventh Framework Programme FP7/2007–2013 under REA grant agreement number PITN-GA-2011-289313Project
Gobierno de España. AYA2010-15081; Gobierno de España. ATA2010-21322-C03-02; info:eu-repo/grantAgreement/EC/FP7/289313; Gobierno de España. AYA2013-48226-C3-1P; info:eu-repo/grantAgreement/EC/FP7/303912Editor's Version
http://dx.doi.org/10.1088/2041-8205/806/2/L31Subjects
cD; Galaxies: elliptical and lenticular; Galaxies: evolution; Galaxies: formation; Galaxies: fundamental parameters; Galaxies: stellar content; FísicaNote
Astrophysical Journal Letters 806.2 (2015): L31 reproduced by permission of the AASRights
© 2015. The American Astronomical SocietyAbstract
Variations in the stellar initial mass function (IMF) have been invoked to explain the spectroscopic and dynamical properties of early-type galaxies (ETGs). However, no observations have yet been able to disentangle the physical driver. We analyze here a sample of 24 ETGs drawn from the CALIFA survey, deriving in a homogeneous way their stellar population and kinematic properties. We find that the local IMF is tightly related to the local metallicity, becoming more bottom-heavy toward metal-rich populations. Our result, combined with the galaxy mass-metallicity relation, naturally explains previous claims of a galaxy mass-IMF relation, derived from non-IFU spectra. If we assume that - within the star formation environment of ETGs - metallicity is the main driver of IMF variations, a significant revision of the interpretation of galaxy evolution observables is necessary
Files in this item
Google Scholar:Martín-Navarro, I.
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Vazdekis, A.
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La Barbera, F.
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Falcón-Barroso, J.
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Lyubenova, M.
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Ferreras, I.
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Sánchez, S. F.
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Trager, S. C.
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García-Benito, R.
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Mast, D.
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Mendoza, M. A.
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Sánchez-Blázquez, Patricia
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González Delgado, R.
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Walcher, C. J.
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The CALIFA Team
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Van de Ven, Glenn
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