2004/03/20 by William C. Keel, Jay B. Holberg, Patrick M. Treuthardt · 16 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Galaxies: Formation, Evolution, Phenomena #Galaxy #Local Group #Metallicity #Milky Way #Population #Spectral line #Spectroscopy #Stars #Stellar population #astro-ph
paper · pdf · doi:10.1086/421367
published in The Astronomical Journal 128(1), 211-223 (Institute of Physics) · Astronomical Journal, in press (July 2004). 8 figures; before publication, full-resolution figures are available as a single PDF file from http://www.astr.ua.edu/keel/fusefigs.pdf
arxiv created 2004/03/20 · openalex publication_date 2004/07/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present Far Ultraviolet Spectroscopic Explorer spectroscopy and supporting data for star-forming regions in nearby galaxies, to examine their massive-star content and explore the use of abundance and population indicators in this spectral range for high-redshift galaxies. New far-ultraviolet spectra are shown for four bright H II regions in M33 (NGC 588, 592, 595, and 604), the H II region NGC 5461 in M101, and the starburst nucleus of NGC 7714, supplemented by the very low metallicity galaxy I Zw 18. In each case we see strong Milky Way absorption systems from H 2 , but intrinsic absorption within each galaxy is weak or undetectable, perhaps because of the "UV bias" in which reddened stars that lie behind molecular-rich areas are also heavily reddened. We see striking changes in the stellar wind lines from these populations with metallicity, suggesting that C II, C III, C IV, N II, N III, and P V lines are potential tracers of stellar metallicity in star-forming galaxies. Three of these relations—involving N IV, C III, and P V—are nearly linear over the range from O/H = 0.05–0.8 solar. The major difference in continuum shapes among these systems is that the giant H II complex NGC 604 has a stronger continuum shortward of 950 Å than any other object in this sample. Small number statistics would likely go in the other direction; we favor this as the result of a discrete star-forming event ≈3 Myr ago, as suggested by previous studies of its stellar population.