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Date and Time of the Query: 2019-06-18 T13:48:56 PDT
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For refcode 2011ApJ...731...10M:
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2011ApJ...731...10M Radial Distribution of Stars, Gas, and Dust in SINGS Galaxies. III. Modeling the Evolution of the Stellar Component in Galaxy Disks Munoz-Mateos, J. C.; Boissier, S.; Gil de Paz, A.; Zamorano, J.; Kennicutt, R. C., Jr.; Moustakas, J.; Prantzos, N.; Gallego, J. Abstract. 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 {lambda}. 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 {lambda} is close to the lognormal function obtained in cosmological N-body simulations, peaking at {lambda} ~ 0.03 regardless of the total halo mass. We do not find any evident trend between {lambda} 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. Key words: galaxies: abundances, galaxies: evolution, galaxies: photometry, galaxies: spiral
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