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Título:
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Radial distribution of stars, gas, and dust in sings galaxies. III. Modeling the evolution of the stellar component in galaxy disks
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Autores:
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Muñoz Mateos, J. C. ;
Boissier, S. ;
Gil de Paz, Armando ;
Zamorano Calvo, Jaime ;
Kennicutt, R. C., Jr. ;
Moustakas, J. ;
Prantzos, N. ;
Gallego Maestro, Jesús
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Tipo de documento:
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texto impreso
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Editorial:
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American Astronomical Society, 2011-04-10
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Dimensiones:
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application/pdf
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Nota general:
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info:eu-repo/semantics/openAccess
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Idiomas:
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Palabras clave:
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Estado = Publicado
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Materia = Ciencias: Física: Astrofísica
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Materia = Ciencias: Física: Astronomía
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Tipo = Artículo
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Resumen:
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We analyze the evolution of 42 spiral galaxies in the Spitzer Infrared Nearby Galaxies Survey. We make use of ultraviolet (UV), optical, and near-infrared radial profiles, corrected for internal extinction using the total-infrared to UV ratio, to probe the emission of stellar populations of different ages as a function of galactocentric distance. We fit these radial profiles with models that describe the chemical and spectro-photometric evolution of spiral disks within a self-consistent framework. These backward evolutionary models successfully reproduce the multi-wavelength profiles of our galaxies, except for the UV profiles of some early-type disks for which the models seem to retain too much gas. From the model fitting we infer the maximum circular velocity of the rotation curve V_C and the dimensionless spin parameter ?. The values of V_C are in good agreement with the velocities measured in H I rotation curves. Even though our sample is not volume limited, the resulting distribution of ? is close to the lognormal function obtained in cosmological N-body simulations, peaking at ? ?0.03 regardless of the total halo mass. We do not find any evident trend between ? and Hubble type, besides an increase in the scatter for the latest types. According to the model, galaxies evolve along a roughly constant mass-size relation, increasing their scale lengths as they become more massive. The radial scale length of most disks in our sample seems to have increased at a rate of 0.05-0.06 kpc Gyr^-1, although the same cannot be said of a volume-limited sample. In relative terms, the scale length has grown by 20%-25% since z = 1 and, unlike the former figure, we argue that this relative growth rate can be indeed representative of a complete galaxy sample.
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En línea:
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https://eprints.ucm.es/33814/1/jesusgallego24libre.pdf
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