# Searching for compact radio sources associated to UCHII regions

## TL;DR

This study used VLA 1.3 cm observations to identify 13 compact radio sources within 9 UCHII regions, revealing two types with different properties and potential roles in the evolution of these early star formation regions.

## Contribution

The paper reports the detection of new compact sources in UCHII regions and classifies them into two types based on their properties, providing insights into their nature and role in UCHII region evolution.

## Key findings

- 13 compact sources found in 9 UCHII regions
- Two types of sources identified with different characteristics
- Potential role of sources in UCHII region lifetime problem

## Abstract

Ultra-Compact (UC)HII regions represent a very early stage of massive star formation whose structure and evolution are not yet fully understood. Interferometric observations in recent years show that some UCHII regions have associated compact sources of uncertain nature. Based on this, we carried out VLA 1.3 cm observations in the A configuration of selected UCHII regions in order to report additional cases of compact sources embedded in UCHII regions. From the observations, we find 13 compact sources associated to 9 UCHII regions. Although we cannot establish an unambiguous nature for the newly detected sources, we assess some of their observational properties. According to the results, we can distinguish between two types of compact sources. One type corresponds to sources that probably are deeply embedded in the dense ionized gas of the UCHII region. These sources are being photo-evaporated by the exciting star of the region and will last for 10$^4-10^5$ yr. They may play a crucial role in the evolution of the UCHII region as the photo-evaporated material could replenish the expanding plasma and might provide a solution to the so-called lifetime problem for these regions. The second type of compact sources is not associated with the densest ionized gas of the region. A few of these sources appear resolved and may be photo-evaporating objects such as those of the first type but with significantly lower mass depletion rates. The rest of sources of this second type appear unresolved and their properties are varied. We speculate on the similarity between the sources of the second type and those of the Orion population of radio sources.