Ultra- and Hyper-compact HII regions at 20 GHz

TL;DR

This study conducts the first blind radio survey of hyper- and ultra-compact HII regions at 20 GHz, providing detailed spectral and physical characterizations, and identifies potential calibrator sources for high-frequency astronomical instruments.

Contribution

It introduces a novel blind survey method for hyper- and ultra-compact HII regions and provides comprehensive spectral and physical data for these sources.

Findings

Identified 4 hyper-compact and 4 ultra-compact HII regions.

Determined sizes, temperatures, and emission measures of the sources.

Found excess emission at 95 GHz not explained by current models.

Abstract

We present radio and infrared observations of 4 hyper-compact HII regions and 4 ultra-compact HII regions in the southern Galactic plane. These objects were selected from a blind survey for UCHII regions using data from two new radio surveys of the southern sky; the Australia Telescope 20 GHz survey (AT20G) and the 2nd epoch Molonglo Galactic Plane Survey (MGPS-2) at 843 MHz. To our knowledge, this is the first blind radio survey for hyper- and ultra-compact HII regions. We have followed up these sources with the Australia Telescope Compact Array to obtain H70-alpha recombination line measurements, higher resolution images at 20 GHz and flux density measurements at 30, 40 and 95 GHz. From this we have determined sizes and recombination line temperatures as well as modeling the spectral energy distributions to determine emission measures. We have classified the sources as hyper-compact or ultra-compact on the basis of their physical parameters, in comparison with benchmark parameters from the literature. Several of these bright, compact sources are potential calibrators for the Low Frequency Instrument (30-70 GHz) and the 100-GHz channel of the High Frequency Instrument of the Planck satellite mission. They may also be useful as calibrators for the Australia Telescope Compact Array, which lacks good non-variable primary flux calibrators at higher frequencies and in the Galactic plane region. Our spectral energy distributions allow the flux densities within the Planck bands to be determined, although our high frequency observations show that several sources have excess emission at 95 GHz (3 mm) that can not be explained by current models.