Tracing Abundance Gradients in Galaxies with the Spitzer Space Telescope Infrared Spectrograph

Details Tracing Abundance Gradients in Galaxies with the Spitzer Space Telescope Infrared Spectrograph Tracing Abundance Gradients in Galaxies with the Spitzer Space Telescope Infrared Spectrograph

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.1907g&link_type=abstract

American Astronomical Society Meeting 210, #19.07; Bulletin of the American Astronomical Society, Vol. 39, p.120

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Deriving abundance gradients across a galaxy is important for determining the galaxy's star formation history and chemical evolution. The spectral range of the Spitzer Space Telescope Infrared Spectrograph (IRS) includes, among others, lines from several ionic species of neon and sulfur, and we use these lines to derive the total elemental abundances. Abundances determined from infrared lines have the advantage over those determined from optical and UV lines in that they depend only weakly on electron temperature and are less affected by extinction. We are currently working on two projects. In the first we use IRS maps of HII regions across external galaxies (NGC 6946 and M51a) to characterize the abundance gradients of neon on sulfur. In the second we study planetary nebulae in the galactic bulge in order to characterize the abundance gradient near the galactic center and see if that gradient follows the trend of the gradient in the solar neighborhood. In this poster we will present the latest progress from these projects.
This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through Contract Number 1257184 issued by JPL/Caltec.

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