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Radial distribution of stars, gas and dust in sings galaxies. I. Surface photometry and morphology



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Muñoz Mateos, J. C. and Gil de Paz, Armando and Zamorano Calvo, Jaime and Boissier, S. and Dale, D. A. and Pérez González, Pablo Guillermo and Gallego Maestro, Jesús and Madore, B. F. and Bendo, G. and Boselli, A. and Buat, V. and Calzetti, D. and Moustakas, J. and Kennicutt, R. C. Jr. (2009) Radial distribution of stars, gas and dust in sings galaxies. I. Surface photometry and morphology. Astrophysical journal, 703 (2). pp. 1569-1596. ISSN 0004-637X

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Official URL: http://dx.doi.org/10.1088/0004-637X/703/2/1569


We present ultraviolet through far-infrared (FIR) surface brightness profiles for the 75 galaxies in the Spitzer Infrared Nearby Galaxies Survey (SINGS). The imagery used to measure the profiles includes Galaxy Evolution Explorer UV data, optical images from Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and Sloan Digital Sky Survey, near-IR data from Two Micron All Sky Survey, and mid- and FIR images from Spitzer. Along with the radial profiles, we also provide multi-wavelength asymptotic magnitudes and several nonparametric indicators of galaxy morphology: the concentration index (C42), the asymmetry (A), the Gini coefficient (G), and the normalized second-order moment of the brightest 20% of the galaxy’s flux (M20). In this paper, the first of a series, we describe the technical aspects regarding the surface photometry, and present a basic analysis of the global and structural properties of the SINGS galaxies at different wavelengths. The homogeneity in the acquisition, reduction, and analysis of the results presented here makes these data ideal for multiple unanticipated studies on the radial distribution of the properties of stars, dust, and gas in galaxies. Our radial profiles show a wide range of morphologies and multiple components (bulges, exponential disks, inner and outer disk truncations, etc.) that vary not only from galaxy to galaxy but also with wavelength for a given object. In the optical and near-IR, the SINGS galaxies occupy the same regions in the C42–A-G-M20 parameter space as other normal galaxies in previous studies. However, they appear much less centrally concentrated, more asymmetric, and with larger values of G when viewed in the UV (due to star-forming clumps scattered across the disk) and in the mid-IR (due to the emission of polycyclic aromatic hydrocarbons at 8.0 μm and very hot dust at 24 μm). In an accompanying paper by Mu˜noz-Mateos et al., we focus on the radial distribution of dust properties in the SINGS galaxies, providing a detailed analysis of the radial variation of the attenuation, the dust column density, the dust-to-gas ratio, the abundance of PAHs, and the intensity of the heating starlight.

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© 2009. 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. J.C.M.M., A.G.dP, J.Z., P.G.P., and J.G. are partially financed by the Spanish Programa Nacional de Astronomía y Astrofísica under grant AYA2006-02358. A.Gd.P. is also financed by the MAGPOP EU Marie Curie Research Training Network. We also thank the anonymous referee for very useful comments that have significantly 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 Ko-rean 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-PlanckInstitute 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. This research has also made use of the VizieR catalogue access tool, CDS, Strasbourg, France.

Uncontrolled Keywords:Multiband imaging photometer; Spitzer-space-telescope; Digital sky survey; Disk-dominated galaxies; Compact dwarf galaxies; Infrared array camera; Absolute calibration; Spiral galaxies; Nearby galaxies; μ-m
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
ID Code:34140
Deposited On:05 Nov 2015 13:46
Last Modified:10 Dec 2018 15:05

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