EAS Publications Series
Volume 56, 2012The Role of the Disk-Halo Interaction in Galaxy Evolution: Outflow vs. Infall?
|Page(s)||77 - 80|
|Section||Structure and Components of the ISM in Galaxies|
|Published online||17 September 2012|
Miguel A. de Avillez (ed)
EAS Publications Series, 56 (2012) 77–80
Density variations in Milky Way gas
1 Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
2 Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476 Golm, Germany
Recent studies at optical and radio wavelengths have shown that interstellar clouds have density structures on scales smaller than 1 pc. These have been identified in form of temporal variations or differences in column density within small angular separations. Despite the number of detections with various methods, the nature and ubiquity of the small-scale structure in the ISM is not yet fully understood. Using UV absorption data from FUSE of six LMC stars with small angular separations we study these small-scale structures in the Galactic disk and IV gas at spatial scales less than 1 pc. Based on H2 and O I we find that the differences in column densities represent small density structures in the disk and halo gas.
© EAS, EDP Sciences, 2012