The Far Ultraviolet Spectroscopic Explorer Survey of O VI Absorption in and near the Galaxy

By B. Wakker, B. Savage, K. Sembach, P. Richter, M. Meade, E. B. Jenkins, J. Michael Shull, T. Ake, William P. Blair, W. Dixon and 11 more. 2003

153 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/188f82960dbc6a5281b043d02b1f78f95e657e90

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In Astronomy and Astrophysics

Citations in the corpus

A High-Resolution Survey of Low-Redshift QSO Absorption Lines: Statistics and Physical Conditions of O VI Absorbers (2007, background): “The Milky Way O VI HVCs (Sembach et al. 2003; Wakker et al. 2003) suffer a similar problem to the extragalactic systems: the O VI in Galactic HVCs is thought to arise in interfaces (e.g., Sembach et al. 2003; Ganguly et al. 2005), but the observed HVC O VI columns tend to be substantially greater…”
THE STRUCTURE OF THE MILKY WAY'S HOT GAS HALO (2013, background): “In addition to this X-ray emitting/absorbing gas, O vi, the most common ion in ∼105.5 K gas, has been extensively studied with FUSE (Sembach et al. 2003; Wakker et al. 2003; Fox et al. 2004).”
Multiphase High-Velocity Clouds toward HE 0226–4110 and PG 0953+414 (2005, methodology): “Even after the application of the pipeline, velocity shifts have to be determined for each exposure and each detector segment before co-addition of the spectra to obtain accurate wavelength solutions (see x 3.4 in Wakker et al. 2003).”
Distribution and Kinematics of O VI in the Galactic Halo (2002, methodology): “The entire set of observations is found in the O vi catalog paper (Wakker et al. 2003).”
Highly Ionized High-Velocity Gas in the Vicinity of the Galaxy (2002, methodology): “The other two papers include a catalog with basic measurements and illustrations of all of the O vi profiles observed in the survey (Wakker et al. 2003) and a companion study of the O vi absorption associated with the thick disk/halo of the Milky Way (Savage et al. 2003).”
Distances to Galactic High-Velocity Clouds. I. Cohen Stream, Complex GCP, Cloud g1 (2007, methodology): “Since then, Wakker et al. (2003) have reported a lower limit of 8 kpc for Complex A, while Thom et al. (2006) used the star HE 1048+0231 to set an upper limit of 8.8 kpc to cloud WW 35 (vLSR þ100 km s 1).”