Spectral Observations of Diffuse Far‐Ultraviolet Emission from the Hot Phase of the Interstellar Medium with the Diffuse Ultraviolet Experiment

Abstract

One of the keys to interpreting the character and evolution of interstellar matter in the Galaxy is understanding the distribution of the low-density hot (105-106 K) phase of the interstellar medium (ISM). This phase is much more difficult to observe than the cooler high-density components of the ISM because of its low density and lack of easily observable tracers. Because gas of this temperature emits mainly in the far-ultraviolet (FUV) (912-1800 A) and extreme-ultraviolet (EUV) (80-912 A), and (for gas hotter than 106 K) X-rays, observations in these bands can provide important constraints to the distribution of this gas. Because of interstellar opacity at EUV wavelengths, only FUV and X-ray observations can provide clues to the properties of hot gas from distant regions. We present results from a search for FUV emission from the diffuse ISM conducted with an orbital FUV spectrometer, DUVE, which was launched in 1992 July. The DUVE spectrometer, which covers the band from 950 to 1080 A with 3.2 A resolution, observed a region of low neutral hydrogen column density near the south Galactic pole for a total effective integration time of 1583 s. The only emission line detected was a geocoronal hydrogen line at 1025 A. We are able to place upper limits to several expected emission features that provide constraints on interstellar plasma parameters. We are also able to place limits on the continuum emission throughout the bandpass. We compare these limits and other diffuse observations with several models of the structure of the ISM and discuss the ramifications.