Program: GS-2023A-FT-104

The study of massive stars is important to understand a large range of astrophysical topics from star formation regions to supernovae progenitors. A way to test massive-star evolutionary models is to gather information of the nebulae often accompanying these stars because of their powerful winds. By determining the ejected abundances of matter that compose the nebulae, we can decipher the chemical abundances that were in the envelope of the previous phases of the star and compare them to the ones predicted by the evolutionary models. Spectroscopy is then an important technique needed for this study. The determination of chemical abundances requires to first establish the electron density and temperature of the gas linked to the star. The object of interest of this proposal is the Wolf-Rayet (WR) wind blown bubble NGC 2359. The objective is to determine the electron density in filaments of the bubble surrounding the star from the line ratio of the [ClIII] doublet (5518, 5538A) that we would acquire with GMOS-S with the B600 grating and a longslit. This data will serve for an article in the context of a M. Sc. student project about the mass loss history of the WR bubble nebula NGC 2359.