We present a new instrument for wide-field, narrow-band imaging of the O VI doublet at 1032, 1038 Å. This doublet constitutes the brightest astrophysical line emission from diffuse gas at 300,000 degrees K. Gases at this temperature are primarily formed by supernova blast waves, and are key in understanding the energy budget of the galaxy. We use a conventional Gregorian telescope design to provide excellent zero-order imaging, in conjunction with aberration-corrected holography to yield high-resolution images of O VI in first order. This instrument design uses only two reflective elements and no transmissions, minimizing the light lost due to the poor reflectivity and transmissivity of materials in the far ultraviolet. The holographic recording solution provides 4-9 arcsecond imaging over a 0.5 degree field of view. This instrument demonstrates the versatility of the holographic telescope concept by expanding is applicability to larger fields of view. We are developing a sounding rocket payload to demonstrate the power of this wide field holographic telescope design, particularly as a means of mapping shocked gas in the interstellar medium, at temperatures intermediate to those sampled in optical and X-ray emission. We present the optical design, instrument performance, image reconstruction techniques, and relevant scientific simulations.