High resolution radio recombination line observations

Abstract

Over the last decade sensitive observations of radio recombination line emission using high angular resolution synthesis telescopes have become available. As a result it has now become possible to image the physical parameters deduced from radio recombination lines across individual sources. In the case of HII regions this work has resulted in detailed images of radial velocities, electron temperatures and the abundance of singly ionized helium (Y+). Direct observational evidence has been found for pressure broadening and non-LTE effects. Dramatic variations have been found in the ratio of He+ to H+, from as low as a few percent (the galactic centre) to as high 34% in one region of W3. Detailed images have been obtained of the partially ionized medium (CII and H‡ regions) close to HII regions. Observations of recombination lines at very low frequencies have revealed the existence of very low density ionized gas in all directions in our galaxy. Higher resolution observations have led to a partial understanding of this medium. The first complete velocity field of the ionized gas in the centre of our galaxy has been obtained. Very recently the first images were made of extragalactic radio recombination lines, offering the possibility to study the kinematics of the ionized gas in the central few hundred parsecs of external galaxies.