Radio Recombination Lines toward the Galactic Center Lobe

TL;DR

This study uses radio recombination line observations to determine that the Galactic Center lobe is located in the GC region, characterized by specific physical conditions, and likely forms a shell around the central galaxy area.

Contribution

It provides new observational evidence constraining the physical conditions and location of the Galactic Center lobe using radio recombination lines.

Findings

Ionized gas morphology matches radio continuum emission.

Electron temperature less than 4000 K.

Gas density approximately 910 cm^{-3}.

Abstract

The Galactic Center lobe is a degree-tall shell seen in radio continuum images of the Galactic center (GC) region. If it is actually located in the GC region, formation models would require massive energy input (e.g., starburst or jet) to create it. At present, observations have not strongly constrained the location or physical conditions of the GC lobe. This paper describes the analysis of new and archival single-dish observations of radio recombination lines toward this enigmatic object. The observations find that the ionized gas has a morphology similar to the radio continuum emission, suggesting that they are associated. We study averages of several transitions from H106alpha to H191epsilon and find that the line ratios are most consistent with gas in local thermodynamic equilibrium. The radio recombination line widths are remarkably narrow, constraining the typical electron temperature to be less than about 4000 K. These observations also find evidence of pressure broadening in the higher electronic states, implying a gas density of n_e=910^{+310}_{-450} cm^{-3}. The electron temperature, gas pressure, and morphology are all consistent with the idea that the GC lobe is located in the GC region. If so, the ionized gas appears to form a shell surrounding the central 100 parsecs of the galaxy with a mass of roughly 10^5 Msun, similar to ionized outflows seen in dwarf starbursts.