Modeling Ionized Gas in the Small Magellanic Cloud: The Wolf-Rayet Nebula N76
Elizabeth Tarantino, Alberto D. Bolatto, R’emy Indebetouw, M’onica Rubio, Karin M. Sandstrom, J. -D T. Smith, Daniel Stapleton, Mark Wolfire
arXiv:2404.08041v1 Announce Type: new
Abstract: We present Cloudy modeling of infrared emission lines in the Wolf-Rayet (WR) nebula N76 caused by one of the most luminous and hottest WR stars in the low metallicity Small Magellanic Cloud. We use spatially resolved mid-infrared Spitzer/IRS and far-infrared Herschel/PACS spectroscopy to establish the physical conditions of the ionized gas. The spatially resolved distribution of the emission allows us to constrain properties much more accurately than using spatially integrated quantities. We construct models with a range of constant hydrogen densities between n$_H$ = 4 – 10 cm$^{-3}$ and a stellar wind-blown cavity of 10 pc which reproduces the intensity and shape of most ionized gas emission lines, including the high ionization lines [OIV] and [NeV], as well as [SIII], [SIV], [OIII], and [NeIII]. Our models suggest that the majority of [SiII] emission (91%) is produced at the edge of the HII region around the transition between ionized and atomic gas while very little of the [CII] emission (arXiv:2404.08041v1 Announce Type: new
Abstract: We present Cloudy modeling of infrared emission lines in the Wolf-Rayet (WR) nebula N76 caused by one of the most luminous and hottest WR stars in the low metallicity Small Magellanic Cloud. We use spatially resolved mid-infrared Spitzer/IRS and far-infrared Herschel/PACS spectroscopy to establish the physical conditions of the ionized gas. The spatially resolved distribution of the emission allows us to constrain properties much more accurately than using spatially integrated quantities. We construct models with a range of constant hydrogen densities between n$_H$ = 4 – 10 cm$^{-3}$ and a stellar wind-blown cavity of 10 pc which reproduces the intensity and shape of most ionized gas emission lines, including the high ionization lines [OIV] and [NeV], as well as [SIII], [SIV], [OIII], and [NeIII]. Our models suggest that the majority of [SiII] emission (91%) is produced at the edge of the HII region around the transition between ionized and atomic gas while very little of the [CII] emission (