Skip to main content
Revealing the Ionization Properties of the Magellanic Stream Using Optical Emission
The Astrophysical Journal (2017)
  • K. A. Barger, Texas Christian University
  • G. J. Madsen, University of Wisconsin - Madison
  • A. J. Fox, Space Telescope Science Institute
  • B. P. Wakker, University of Wisconsin - Madison
  • J. Bland-Hawthorn, University of Sydney, Australia
  • D. Nidever, National Optical Astronomy Laboratory
  • L. M. Haffner, University of Wisconsin - Madison
  • Jacqueline Antwi-Danso, Texas A & M University - College Station
  • Michael Hernandez, Texas Christian University
  • N. Lehner, University of Notre Dame
  • A. S. Hill, Haverford College
  • A. Curzons, University of Sydney, Australia
  • T. Tepper-García, University of Sydney, Australia
The Magellanic Stream, a gaseous tail that trails behind the Magellanic Clouds, could replenish the Milky Way (MW) with a tremendous amount of gas if it reaches the Galactic disk before it evaporates into the halo. To determine how the Magellanic Stream's properties change along its length, we have conducted an observational study of the Hα emission, along with other optical warm ionized gas tracers, toward 39 sight lines. Using the Wisconsin Hα Mapper telescope, we detect Hα emission brighter than 30–50 mR in 26 of our 39 sight lines. This Hα emission extends over 2 degrees away from the H I emission. (See website for rest of abstract.)
  • galaxies,
  • Magellanic clouds,
  • dwarf galaxies,
  • interstellar medium
Publication Date
December 18, 2017
Citation Information
K. A. Barger, G. J. Madsen, A. J. Fox, B. P. Wakker, et al.. "Revealing the Ionization Properties of the Magellanic Stream Using Optical Emission" The Astrophysical Journal Vol. 851 Iss. 2 (2017) ISSN: 1538-4357
Available at: