1995
DOI: 10.1086/176295
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The Massive Stars of I ZW 18 as Seen in Hubble Space Telescope Images

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Cited by 99 publications
(128 citation statements)
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“…However, it is equally clear that young, massive stars are the dominant contributors to the UV flux of the NW component. Observations of individual stars in I Zw 18 with WFC2 (Hunter & Thronson 1995) and STIS (Brown et al 2002;Heap et al 2013) on HST indicate that the NW massive star cluster has a range of ages. The brightest stars in the UV are also the youngest, and their inferred masses range up to 150 M .…”
Section: Contamination By Stellar Absorptionmentioning
confidence: 97%
“…However, it is equally clear that young, massive stars are the dominant contributors to the UV flux of the NW component. Observations of individual stars in I Zw 18 with WFC2 (Hunter & Thronson 1995) and STIS (Brown et al 2002;Heap et al 2013) on HST indicate that the NW massive star cluster has a range of ages. The brightest stars in the UV are also the youngest, and their inferred masses range up to 150 M .…”
Section: Contamination By Stellar Absorptionmentioning
confidence: 97%
“…Hereafter we identify this region as the Galactic Region. Historically, IZw18 has been considered as a very young galaxy, probably experiencing star formation for the first time (Searle & Sargent 1972;Hunter & Thronson 1995;Dufour et al 1996). The presence of WR stars in the brighter (NW) component (Izotov et al 1997a;Legrand et al 1997;de Mello et al 1998;Brown et al 2002) indicate an ongoing star formation, or a star formation which has stopped only a few Myr ago.…”
Section: The History Of the Star Formation History Determinations Of mentioning
confidence: 99%
“…Loose & Thuan 1986;Papaderos et al 1996a;Cairós et al 2001;Bergvall & Östlin 2002;Noeske et al 2003;Gil de Paz & Madore 2005). Initial CMD studies suggested an age for the main body between several 10 Myr (Hunter & Thronson 1995;Dufour et al 1996b) and ∼1 Gyr (Aloisi et al 1999). Östlin (2000) argues from an HST NICMOS near infrared (NIR) study that a fit to the J vs. J − H CMD of I Zw 18 is best achieved for a stellar population of age ∼5 Gyr.…”
Section: Introductionmentioning
confidence: 99%