[Previous] | [Session 112] | [Next]
C. W. Danforth, K. R. Sembach, J. C. Howk, W. P. Blair (JHU)
Since its launch in June 1999, the Far Ultraviolet Spectroscopic Explorer (FUSE) satellite has observed ~72 hot stars in the Magellanic Clouds in the spectral range 905--1187\rmÅ. These observations provide high-resolution (~15-20 km~s-1) absorption line measurements of stellar photosphere and wind material as well as gas along the lines of sight to these stars. A range of ionic species are covered including \ion{O}{6}, which probes T=105-106K gas; \ion{C}{3}, \ion{Fe}{3}, and \ion{S}{3}, which trace photoionized 103-104K gas; \ion{C}{2}, \ion{Fe}{2}, \ion{Si}{2}, \ion{O}{1}, and \ion{Ar}{1}, which probe 102-104K \ion{H}{1}-bearing gas; and H2 from cold clouds. To help understand the morphology and environment in which each FUSE target is located, we have obtained narrow-band H\alpha and other emission-line CCD images with the Curtis Schmidt Telescope at CTIO.
In this poster, we present an atlas of narrow-band images and FUSE spectra for a large subset of the Magellanic Cloud sight lines. The images trace the morphology of the warm (T~04K) H\alpha-emitting material over a 20\arcmin\ field surrounding each target. Selected spectral lines observed by FUSE reveal a variety of velocity components and physical conditions in the gas along these sight lines. This project is the first step in a graduate thesis designed to study the structure and physical conditions of the hot interstellar medium in the Magellanic Clouds.
This work is supported by NASA contract NAS5-32985 to the Johns Hopkins University.
The author(s) of this abstract have provided an email address for comments about the abstract: danforth@pha.jhu.edu