Studying a hot molecular core embedded in a photodissociation region

TL;DR

This study investigates the chemical composition and physical properties of a hot molecular core embedded in a photodissociation region using multi-scale observations, revealing insights into star formation environments.

Contribution

It provides high-resolution characterization of the hot core G33.133-mm3 and analyzes its molecular chemistry and UV radiation effects, advancing understanding of star-forming regions.

Findings

Identified molecular abundance ratios related to UV radiation effects.

Characterized the chemical composition of the hot core, including complex molecules.

Measured the core's size and structure at high spatial resolution.

Abstract

At the first Galactic quadrant, at l=33.134, b=-0.091, an extended photodissociation region generated by an HII region complex lies. This region is related to abundant molecular gas, and particularly, a hot molecular core, known as G33.133-mm3, appears embedded in a molecular clump. Using data from the James Clerk Maxwell Telescope with an angular resolution of about 15", we studied the 13CO/C18O abundance ratio towards the mentioned molecular clump and its relation with the ultraviolet radiation. At smaller spatial scales, using data from the Atacama Large Millimeter Array (angular resolution about 0.7\arcsec), the hot molecular core G33.133-mm3, that has a size of about 2600 au, and is an appropriate site to form stars, was characterized. In particular, some points about its chemistry are mentioned based on the emission of the cyanide or nitrile radical (CN) and others more complex molecules, such as CH3OH, CH3CN, CH3OCHO, and CH3CCH.