AAS 205th Meeting, 9-13 January 2005
Session 60 Secular Evolution Potpourri: Star Formation to Galactic Structures
Poster, Tuesday, January 11, 2005, 9:20am-6:30pm, Exhibit Hall

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[60.06] Spitzer Observations of Two Early-Type Spiral Galaxies with Dust Rings

G. J. Bendo (Steward Observatory), L. Armus (Spitzer Science Center), D. Calzetti (Space Telescope Science Institute), D. A. Dale (University of Wyoming), B. T. Draine (Princeton University), C. W. Engelbracht, K. D. Gordon (Steward Observatory), A. Grauer (University of Arkansas, Little Rock), G. Helou (California Institute of Technology), D. J. Hollenbach (NASA Ames Research Center), T. H. Jarrett (California Institute of Technology), R. D. Joseph (Institute for Astronomy), R. C. Kennicutt (Steward Observatory), L. J. Kewley (Institute for Astronomy), C. Leitherer (Space Telescope Science Institute), A. Li (University of Missouri - Columbia), S. Malhotra, M. Meyer (Space Telescope Science Institute), E. J. Murphy (Yale University), M. W. Regan (Space Telescope Science Institute), G. H. Rieke, M. J. Rieke (Steward Observatory), H. Roussel, K. Sheth (California Institute of Technology), J. D. T. Smith (Steward Observatory), M. D. Thornley (Bucknell University), F. Walter (Max Planck Institute for Astronomy)

We present Spitzer images of the SB0/a galaxy NGC 1291 and the SAa galaxy NGC 4594. Both galaxies contain dust rings that can be used for studying the relation between dust emission and star formation activity. At 24 microns, the nuclei of both galaxies are the brightest sources in the galaxies, and dust emission from the rings is relatively weak. At 160 microns, however, the dust rings are more prominent sources; in NGC 4594, the dust ring is the source of virtually all of the 160 micron emission. We discuss whether the 160 micron emission from the rings is related to star formation activity or to heating by older stellar populations, and we examine the relation between dust and PAH emission. For NGC 4594, we also present submillimeter data that show that the nucleus dominates the 850 micron emission. These results demonstate that the 850 micron emission cannot come from the same dust that dominates the 160 micron emission. We examine the possible mechanisms that could be generating the 850 micron emission as well as the implications for dust models and galaxy spectral energy distribution templates.

The author(s) of this abstract have provided an email address for comments about the abstract: gbendo@as.arizona.edu

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© 2004. The American Astronomical Society.