RT Journal Article
T1 Radial distribution of stars, gas, and dust in sings galaxies. III. Modeling the evolution of the stellar component in galaxy disks
A1 Muñoz Mateos, J. C.
A1 Boissier, S.
A1 Gil de Paz, Armando
A1 Zamorano Calvo, Jaime
A1 Kennicutt, R. C., Jr.
A1 Moustakas, J.
A1 Prantzos, N.
A1 Gallego Maestro, Jesús
AB 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 λ. 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 λ is close to the lognormal function obtained in cosmological N-body simulations, peaking at λ ∼0.03 regardless of the total halo mass. We do not find any evident trend between λ 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.
PB American Astronomical Society
SN 0004-637X
YR 2011
FD 2011-04-10
LK https://hdl.handle.net/20.500.14352/44778
UL https://hdl.handle.net/20.500.14352/44778
LA eng
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NO © 2011. The American Astronomical Society. J.C.M.M. acknowledges the receipt of a Formación del Profesorado Universitario fellowship from the Spanish Ministerio de Educación y Ciencia, as well as finantial support from NASA JPL/Spitzer grant RSA 1374189 provided for the S4G project. A.G.dP. is also financed by the Spanish Ramón y Cajal program. J.C.M.M., A.G.dP., J.Z., and J.G. are partially financed by the Spanish Programa Nacional de Astronomía y Astrofísica under grants AYA2006-02358 and AyA2009-10368. They are also partly supported by the Consolider-GTC program under grant CSD2006-00070 and the AstroMadrid project (CAM S2009/ESP-1496). Part of this work was performed during a three-month stay at the Laboratoire d'Astrophysique de Marseille (LAM). J.C.M.M. thanks the Spanish Ministerio de Educación y Ciencia for providing the necessary funds, as well as the LAM staff for their support and warm hospitality. He also acknowledges support from the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We also thank THINGS members A. Leroy and F. Walter for kindly providing the Hi radial profiles in advance of publication. We also thank the anonymous referee for providing valuable comments that have improved the paper. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. This work is part of SINGS, the Spitzer Infrared Nearby Galaxies Survey. The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, Caltech, under NASA contract 1403.Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/.The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Finally, we have made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology (Caltech) under contract with NASA. Facilities: GALEX, Sloan, CTIO:1.5m, KPNO:2.1m, FLWO:2MASS, CTIO:2MASS, Spitzer, VLA.
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