There are several problems in astrophysics that cannot be addressed until very high resolution spectroscopy ((lambda) /(Delta) (lambda) > 100,000) in the far ultraviolet ((lambda) < 2000 angstroms) can be achieved simultaneously with high efficiency. Issues such as atomic isotopic abundances in the interstellar medium, velocity structure in interstellar clouds, and fine and hyperfine line structure in atomic transitions require 100,000 - 200,000 class resolution and high sensitivity; a capability that currently does not exist. Historically, resolutions this high have been obtained with echelle spectrographs, which require two gratings, and must suffer the losses due to reflective efficiency and diffraction efficiency on both gratings. These losses are much more significant in the far ultraviolet than in the visible. We present a means of obtaining very high resolution spectroscopy in the far ultraviolet with a single, holographic grating, which should be significantly more efficient than classic echelle designs.© (1993) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.