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provided by CERN Document Server −1 −1 ˙ [12pt,aasms4,epsf]article Hα M yr M km s Z M M◦ NVλ1240 Si IV λ1400 C IV λ1550 C I λ1657 He II λ1640 N IV λ1720 Si II λ1260 O I/Si II λ1303 C II λ1335 Fe II λ1610 Al II λ1670 O VI λ1034 33715 January 1989 1114 accepted for publication in the ApJL document HST Ultraviolet Spectroscopy of NGC 1741 — a Nearby Template for Distant Energetic StarburstsBased on observations with the NASA/ESA , obtained at the Space Telescope Science Institute, which is operated by AURA for NASA under contract NAS5-26555 Peter S. Conti JILA, University of Colorado, Boulder, CO 80309-0440 e-mail: [email protected] Claus Leitherer Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 e-mail: [email protected] William D. Vacca Institute of Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 e-mail: [email protected] abstract We have obtained a Hubble Space Telescope ultraviolet image and spectrum of the nearby Wolf- Rayet NGC 1741. The spatial morphology from the Faint Object Camera image is dominated by two main starburst centers, each being about 100 times as luminous as 30 Doradus. Both starburst centers are composed of several intense knots of recent formation. A Goddard High Resolution Spectrograph spectrum of a portion of the southern starburst center is consistent with a population of young following a Salpeter IMF for masses above ∼15 (lower mass stars may also be present), and extending up to ∼100 ; about 104 O-type stars are inferred from the UV luminosity. Numerous strong interstellar lines are detected. Although not resolved, their strength suggests that they are formed in individual bubbles and shells with velocities up to a few hundred . The red wing of the Lyman-α absorption profile indicates the presence of several neutral hydrogen components, one in our own Galaxy and the others at or close to the distance of NGC 1741. Overall, the stellar and interstellar line spectrum, as well as the continuum shape of NGC 1741, strongly resembles star-forming recently discovered at high .

ontract NAS5-26555

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