FUSE observations of hot, massive stars

A central component of my research will be involved with the detailed analysis of FUSE spectroscopy of hot, massive stars, such as the one shown below, using state-of-the-art theoretical codes. A large sample of O-type stars will be studied in our own Milky Way galaxy, plus nearby satellite galaxies known as the Magellanic Clouds. Our group at UCL are the sole UK members of the Project Science Team, and have been spearheading this programme which has been allocated a large amount of FUSE observing time.


The above graph shows the intensity of far-ultraviolet light (vertical axis) as a function of wavelength (horizontal axis) for the central star of a planetary nebula known as NGC 1535. This "spectrum" tells us that the star is very hot, and yet is surrounded by cooler atomic and molecular hydrogen gas, which causes many of the features in the graph. The prominent "O VI" P Cygni profile arises from a huge stellar wind that emanates from the star. (This spectrum was obtained with the Hopkins Ultraviolet Telescope during the Astro-1 Space Shuttle mission in 1990.)