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M. Hancock, D. Weistrop, D. Eggers (UNLV), C. H. Nelson (Drake University)
We have obtained ultraviolet and visible wavelength images for the interacting galaxies, NGC 3395 and NGC 3396, using STIS on HST. The images show many isolated sources of ultraviolet emission which are young star forming regions (knots). There are 59 knots in NGC 3395 and 49 knots in NGC 3396 that have fluxes greater than our 99% completeness limit. These knots emit 17% of the total detected FUV flux. Comparison with models from Leitherer et al. (1999) indicates that the ages of the knots are less than 8x107 Myrs.
These knots were found to have masses less than 106 Solar Masses. Estimates of the escape velocities of the knots suggest that many of the knots are likely bound. A determination of the dynamical lifetime confirms the likelihood of those knots being bound. We find that 6 knots in this system are good proto-globular cluster candidates. The observed FUV luminosity function can be fit with a power law with exponent alpha=-1.17 ±0.19 for NGC 3395 and alpha=-0.83 ±0.23 for NGC 3396. There does not appear to be a turnover in the luminosity function brighter than our completeness limit.
This work has been supported in part by NASA, under contract NAS5-31231, and through the Nevada Space Grant Consortium.
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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.