The Origin of Highly Ionized Gas in the Milky Way and Its Relationship To Large Galactic Structures

Details The Origin of Highly Ionized Gas in the Milky Way and Its Relationship To Large Galactic Structures The Origin of Highly Ionized Gas in the Milky Way and Its Relationship To Large Galactic Structures

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7270s&link_type=abstract

HST Proposal ID #7270

Physics

Hst Proposal Id #7270 Interstellar Matter

Scientific paper

We propose to obtain STIS high-resolution {E140H} spectra of the interstellar Si IV, C IV, and N V absorption line profiles along four extended sight lines to study the properties of highly ionized gas in the Milky Way. We have chosen these sight lines to sample a variety of different highly ionized environments, such as H I shells and supershells, spiral arm and interarm gas, and evolved supernova remnants. , By observing these key diagnostic tracers of the highly ionized interstellar medium at a resolution sufficient to fully resolve the observable line profiles, we will accomplish the following three objectives: 1} Determine the primary ionization mechanisms responsible for the highly ionized gas ie., photoionization in warm, T 10^4 K, gas and/or collisional ionization in hot, T 10^5 K, gas. 2} Relate the observed absorption profiles of the high ions and the derived physical conditions of the highly ionized regions to the properties of lower ionization gas to distinguish between the competing ionization models for the production of hot gas {shocks, supernova remnants, photoionized and collisionally ionized interfaces, mixing layers, etc}. 3} Determine the extent to which different Galactic environments contribute to the irregular distribution of highly ionized gas in the Milky Way. By doing so, we will better understand the multiple origins of highly ionized gases and how they affect the distribution, gas-phase abundances, dust content, and ionization of diffuse clouds in the Galaxy.

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