Far-UV Spectroscopy: An Unexplored Frontier

A three year, NASA mission, successfully launched at 15:44:00 GMT on 24 June 1999 covering the far-UV region (905-1195Å) at high spectral resolution. 10,000 times more sensitive than Copernicus (1970s), allowing amongst other things accurate measurements of deuterium in a variety of environments.

The only UK Science Team involvement is at UCL for the hot star programme. A large sample of OB and WR stars have been selected in Galaxy and Magellanic Clouds, covering all spectral types and luminosity classes (see below). Observations will allow a direct determination of mass-loss versus metallicity through stellar wind resonance lines in the far-UV, necessary for an improved understanding of high redshift primordial galaxies.

o FUSE Homepage (John Hopkins - Baltimore)

o Observers guide to FUSE

o Introduction to FUSE

o Scientific benefits of far-UV spectroscopy

o Details of principal FUSE science goals

o Introduction to massive stars

o FUSE observations of massive stars

o Importance for high redshift galaxies

o LMC OB targets (OPTICAL data)

o SMC OB targets (OPTICAL data)

o Wolf-Rayet stars


Poster on FUSE observations of Sand 2 a Wolf-Rayet star in the Large Magellanic Cloud presented at the Jan 2000 AAS meeting, plus FUSE Hot Star team colleagues, Derck Massa & Orsola De Marco.

Return to Hot-Star Group home page


10-Apr-00 pac@star.ucl.ac.uk