Journal article
An ultraviolet-to-radio broadband spectral atlas of nearby galaxies
The Astrophysical journal, Vol.655(2), pp.863-884
02/01/2007
DOI: 10.1086/510362
Abstract
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.
Details
- Title: Subtitle
- An ultraviolet-to-radio broadband spectral atlas of nearby galaxies
- Creators
- D. A Dale - University of WyomingA GIL DE PAZ - Universidad Complutense de MadridB. A Buckalew - California Institute of TechnologyV Buat - Laboratoire d’Astrophysique de MarseilleD Burgarella - Laboratoire d’Astrophysique de MarseilleD Calzetti - Space Telescope Science InstituteJ. M Cannon - Wesleyan UniversityC. W Engelbracht - University of ArizonaG Helou - California Institute of TechnologyD. J Hollenbach - Ames Research CenterT. H Jarrett - California Institute of TechnologyR. C Kennicutt - University of ArizonaK. D Gordon - University of ArizonaC Leitherer - Space Telescope Science InstituteA LI - University of MissouriB. F Madore - Carnegie ObservatoriesD. C Martin - California Institute of TechnologyM. J Meyer - Space Telescope Science InstituteE. J Murphy - Yale UniversityM. W Regan - Space Telescope Science InstituteH Roussel - Max Planck Institute for AstronomyJ. D. T Smith - University of ArizonaM. L Sosey - Space Telescope Science InstituteH. M Hanson - University of WyomingD. A Thilker - Johns Hopkins UniversityF Walter - Max Planck Institute for AstronomyL Armus - California Institute of TechnologyG. J Bendo - Imperial College LondonL Bianchi - Johns Hopkins UniversityM Block - University of ArizonaS Boissier - Laboratoire d’Astrophysique de MarseilleA Boselli - Laboratoire d’Astrophysique de Marseille
- Resource Type
- Journal article
- Publication Details
- The Astrophysical journal, Vol.655(2), pp.863-884
- Publisher
- University of Chicago Press
- DOI
- 10.1086/510362
- ISSN
- 0004-637X
- eISSN
- 1538-4357
- Language
- English
- Date published
- 02/01/2007
- Academic Unit
- Physics and Astronomy
- Record Identifier
- 9984627200302771
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