First Spectra of O Stars in R136A

Details First Spectra of O Stars in R136A First Spectra of O Stars in R136A

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994hst..prop.5297h&link_type=abstract

HST Proposal ID #5297

Astronomy and Astrophysics

Astrophysics

Hst Proposal Id #5297 Stellar Astrophysics

Scientific paper

Hubble images of the cluster, R136a, in the LMC indicate that the cluster contains 3 Wolf-Rayet stars, R136a1,-a2, and a3 (Campbell et al. 1992) and numerous O and B-type stars. Although models for WR stars are not well enough developed to infer the basic parameters of the 3 WR stars in R136a, models for O stars are well well established, and they suggest that the O stars in R136a are relatively normal, having initial masses no higher than 60 Msun (Heap et al. 1992, Malumuth & Heap 1992, di Marchi et al. 1993); there are no unusual "super-massive" stars in R136a. With HST/GHRS/CoSTAR, it will be possible to obtain spectra of an O star in R136a without contam- ination by WR stars. These spectra will be able to confirm or invalidate the photometric results. Thus, these spectra will have implications both for the population of R136a and for the validity of stellar population studies of giant extragalactic HII regions and starbursts that are based entirely on photometry.

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