Far-Ultraviolet Spectroscopic Explorer Observations of Degree-Scale Variations in Galactic Halo OVI

Details Far-Ultraviolet Spectroscopic Explorer Observations of Degree-Scale Variations in Galactic Halo OVI Far-Ultraviolet Spectroscopic Explorer Observations of Degree-Scale Variations in Galactic Halo OVI

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...572..264h&link_type=abstract

The Astrophysical Journal, Volume 572, Issue 1, pp. 264-275.

Astronomy and Astrophysics

Astronomy

35

Ism: Atoms, Ism: Structure, Ultraviolet: Ism

Scientific paper

We report Far-Ultraviolet Spectroscopic Explorer (FUSE) observations of interstellar O VI absorption in the halo of the Milky Way toward 12 early-type stars in the Large Magellanic Cloud (LMC) and 11 in the Small Magellanic Cloud (SMC). The mean column densities of O VI associated with the Galactic halo toward the LMC and SMC are log=14.52+0.10-0.14 and 14.13+0.14-0.20, respectively, where the uncertainties represent the standard deviations of the individual measurements about the means. Significant variations in the O VI column densities are observed over all of the angular scales probed by our observations: 0.5d-5.0d toward the LMC and 0.05d-3.3d toward the SMC. The maximum factors by which the O VI varies between sight lines toward the LMC and SMC are ~2.8 and ~4.2, respectively. Although low-, intermediate-, and high-velocity clouds are present along most of the sight lines toward the LMC, the variations in O VI column densities are found in all of these O VI absorbing structures. The column density variations trace the structure of the hot ionized medium in the Galactic halo on scales of <<80-800 pc toward the LMC and <<6-400 pc toward the SMC (assuming that the absorption arises within the first 5 kpc above the Galactic plane).

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