2012/05/28 by C. J. Evans, R. Hainich, L. M. Oskinova +8
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #Distance modulus #Effective temperature #Large Magellanic Cloud #Nebula #O-type star #Photometry (optics) #Physics #Population #Small Magellanic Cloud #Star (game theory) #Star formation #Stars #Stellar, planetary, and galactic studies #Telescope #astro-ph.SR
paper · pdf · doi:10.1088/0004-637x/753/2/173
Accepted by ApJ, 10 pages, 7 figures, v2 after proofs
arxiv created 2012/05/28 · openalex publication_date 2012/06/26 · arxiv updated 2015/06/05 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
Sk 183 is the visually brightest star in the N90 nebula, a young star-forming region in the Wing of the Small Magellanic Cloud (SMC). We present new optical spectroscopy from the Very Large Telescope which reveals Sk 183 to be one of the most massive O-type stars in the SMC. Classified as an O3-type dwarf on the basis of its nitrogen spectrum, the star also displays broadened He i absorption, which suggests a later type. We propose that Sk 183 has a composite spectrum and that it is similar to another star in the SMC, MPG 324. This brings the number of rare O2- and O3-type stars known in the whole of the SMC to a mere four. We estimate physical parameters for Sk 183 from analysis of its spectrum. For a single-star model, we estimate an effective temperature of 46 ± 2 kK, a low mass-loss rate of ∼10 −7 M ☉ yr −1 , and a spectroscopic mass of 46 +9 −8 M ☉ (for an adopted distance modulus of 18.7 mag to the young population in the SMC Wing). An illustrative binary model requires a slightly hotter temperature (∼47.5 kK) for the primary component. In either scenario, Sk 183 is the earliest-type star known in N90 and will therefore be the dominant source of hydrogen-ionizing photons. This suggests Sk 183 is the primary influence on the star formation along the inner edge of the nebula.