An Ultraviolet-to-Radio Broadband Spectral Atlas of Nearby Galaxies

By D. Dale, A. Paz, Karl D. Gordon, H. Hanson, Lee Armus, G. Bendo, L. Bianchi, M. Block, S. Boissier, A. Boselli and 22 more. 2006

313 citations recorded by the source corpus.

The ultraviolet-to-radio continuum spectral energy distributions are presented for all 75 galaxies in the Spitzer Infrared Nearby Galaxies Survey (SINGS). A principal component analysis of the sample shows that most of the sample's spectral variations stem from two underlying components, one representative of a galaxy with a low infrared-to-ultraviolet ratio and one representative of a galaxy with a high infrared-to-ultraviolet ratio. The influence of several parameters on the infrared-to-ultraviolet ratio is studied (e.g., optical morphology, disk inclination, far-infrared color, ultraviolet spectral slope, and star formation history). Consistent with our understanding of normal star-forming galaxies, the SINGS sample of galaxies in comparison to more actively star-forming galaxies exhibits a larger dispersion in the infrared-to-ultraviolet versus ultraviolet spectral slope correlation. Early-type galaxies, exhibiting low star formation rates and high optical surface brightnesses, have the most discrepant infrared-to-ultraviolet correlation. These results suggest that the star formation history may be the dominant regulator of the broadband spectral variations between galaxies. Finally, a new discovery shows that the 24 μm morphology can be a useful tool for parameterizing the global dust temperature and ultraviolet extinction in nearby galaxies. The dust emission in dwarf/irregular galaxies is clumpy and warm accompanied by low ultraviolet extinction, while in spiral galaxies there is typically a much larger diffuse component of cooler dust and average ultraviolet extinction. For galaxies with nuclear 24 μm emission, the dust temperature and ultraviolet extinction are relatively high compared to disk galaxies.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

A simple model to interpret the ultraviolet, optical and infrared emission from galaxies (2008, methodology): “Dale et al. (2007) find that the Dale & Helou (2002) models that best fit the MIPS colours of NGC 3521, NGC 337 and Mrk 33 have αSED = 3.32, 2.23 and 1.44, respectively (these models are shown as blue lines in Fig.”
HERSCHEL FAR-INFRARED AND SUBMILLIMETER PHOTOMETRY FOR THE KINGFISH SAMPLE OF NEARBY GALAXIES (2011, methodology): “The same aperture is used to extract the flux at each wavelength studied here, and they are very similar, if not identical, to those used for SINGS photometry (Dale et al. 2007), for the 57 galaxies that overlap the two samples.”
THE SPITZER LOCAL VOLUME LEGACY: SURVEY DESCRIPTION AND INFRARED PHOTOMETRY (2009, methodology): “A correction of the form f 70µmtrue = 0.502(f 70µm measured) 1.182, (1) derived from data presented by Gordon et al. (2009) and slightly different than the form first presented in Dale et al. (2007) for SINGS galaxies, is applied to pixel values above a threshold of ∼44 MJy sr−1.”
Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample (2007, background): “The global fluxes Fobs;b and 1 uncertainties for each band b are taken from Dale et al. (2007).”
RADIAL DISTRIBUTION OF STARS, GAS, AND DUST IN SINGS GALAXIES. II. DERIVED DUST PROPERTIES (2009, methodology): “In their analysis of the integrated properties of the SINGS galaxies, Dale et al. (2007) found that most of the scatter towards redder UV colors in the IRX-β diagram was due to ellipticals and early-type spirals.”
The UV-Optical Color Magnitude Diagram. II. Physical Properties and Morphological Evolution On and Off of a Star-forming Sequence (2007, background): “Several recent investigations have explored how this dust geometry might be linked to galaxy morphology(e.g., Pierini et al. 2004; Dale et al. 2007; Zheng et al. 2007).”
Probing the dust properties of galaxies up to submillimetre wavelengths. II. Dust-to-gas mass ratio trends with metallicity and the submm excess in dwarf galaxies (2011, methodology): “The submm fluxes presented in Dale et al. (2007) should therefore be used with caution in a global analysis of the galaxies.”
ESTIMATING THE STAR FORMATION RATE AT 1 kpc SCALES IN NEARBY GALAXIES (2012, methodology): “Proposals to identify and subtract cirrus emission tend to be morphological, defining the cirrus as a smooth background and removing it via image processing techniques such as iterative median filtering (e.g., see Greenawalt et al. 1998; Thilker et al. 2000; Dale et al. 2007; Rahman et al. 2010).”
A Search for Extended Ultraviolet Disk (XUV-Disk) Galaxies in the Local Universe (2007, background): “Assuming a mass-to-light ratio of 0.8 (Dale et al. 2007), it would appear that galaxies are unable to (or already have undergone?) support a [Type 2] galaxy-wide transformational burst of star formation when their stellar mass becomes on the order of 109M⊙ or greater.”
The Behavior of the Aromatic Features in M101 H II Regions: Evidence for Dust Processing (2008, result): “The dust-to-gas ratio we measure is consistent with that expected for a galaxy with a global metallicity of 8.4 (Kennicutt et al. 2003a; Moustakas & Kennicutt 2006) from the work of Draine et al. (2007) on SINGS global SEDs.”
DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. I. COMBINATIONS OF Hα AND INFRARED TRACERS (2009, methodology): “…whether the integrated (mainly nonthermal) radio continuum fluxes of galaxies can be combined in the same way with optical emission-line fluxes to provide attenuation-corrected SFRs. Radio continuum fluxes at 1.4 GHz for the SINGS sample were taken from the compilation of Dale et al. (2007).”