An ALMA Study of Molecular Complexity in the Hot Core G336.99-00.03 MM1

TL;DR

This study uses ALMA data to analyze the molecular composition and chemical evolution of hot cores in a high-mass star-forming region, revealing complex organic molecules and isotopic ratios that inform astrochemical models.

Contribution

It provides a detailed molecular inventory of two sources, distinguishing a hot core from an HII region, and compares observed abundances with chemical models.

Findings

MM1 contains 19 molecular species, including isotopologues and excited states.

Isotopic ratios in MM1 are derived, e.g., $^{12}$C/$^{13}$C from 16.0 to 29.2.

Molecular abundances agree with chemical models within an order of magnitude.

Abstract

High-mass star formation involves complex processes, with the hot core phase playing a crucial role in chemical enrichment and the formation of complex organic molecules. However, molecular inventories in hot cores remain limited. Using data from the ALMA Three-millimeter Observations of Massive Star-forming regions survey (ATOMS), the molecular composition and evolutionary stages of two distinct millimeter continuum sources in the high-mass star forming region G336.99-00.03 have been characterized. MM1, with 19 distinct molecular species detected, along with 8 isotopologues and several vibrationally/torsionally excited states, has been identified as a hot core. MM2 with only 5 species identified, was defined as a HII region. Isotopic ratios in MM1 were derived, with $^{12}$C/$^{13}$C ranging from 16.0 to 29.2, $^{16}$O/$^{18}$O at 47.7, and $^{32}$S/$^{34}$S at 19.2. Molecular abundances in MM1 show strong agreement with other sources and three-phase warm-up chemical models within an order of magnitude for most species. Formation pathways of key molecules were explored, revealing chemical links and reaction networks. This study provides a detailed molecular inventory of two millimeter continuum sources, shedding light on the chemical diversity and evolutionary processes in high-mass star-forming regions. The derived molecular parameters and isotopic ratios offer benchmarks for astrochemical models, paving the way for further investigation into the formation and evolution of complex organic molecules during the hot core phase.