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C. H. Nelson, D. Weistrop, M. Hancock (UNLV)
We obtained UV images using STIS on board HST, of two interacting galaxy systems, NGC 3395, 3396 and NGC 3991, 3994, 3995. All of these galaxies are known to have strong UV emission from IUE observations (Kinney et al. 1993). To study the young stellar populations and the UV morphologies we used two bandpasses, the F25QTZ on the far-UV MAMA detector (\lambda\rm c ~1590Å) and the F25CN182 on the near-UV MAMA detector (\lambda\rm c ~1820Å). These images show many knots of UV emission indicating concentrated star-forming regions. To determine the intrinsic UV flux of these knots we use the fact that the unreddened UV spectra of stellar populations younger than 20 Myr follow F\lambda \propto \lambda-2.5 (Calzetti et al. 1994, Leitherer & Heckman 1995). We calculate the extinction from the UV flux ratio and compare with ground-based estimates based on the Balmer decrement. We combine the UV fluxes with ground based optical aperture photometry to compare with evolutionary synthesis models of star-forming populations.
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The author(s) of this abstract have provided an email address for comments about the abstract: cnelson@physics.unlv.edu