Understanding the chemistry of the young stellar object G29.862-0.0044

TL;DR

This paper provides a detailed chemical and physical analysis of the young stellar object G29.862-0.0044, combining multiwavelength observations to better understand high-mass star formation processes.

Contribution

It introduces new molecular line data and temperature measurements, enhancing the understanding of the region’s chemistry and morphology in high-mass star formation.

Findings

Identification of molecular emission lines such as CH₃OH, HC₃N, H₂CO, C³⁴S, H₂CS.

New temperature estimates of the star-forming region.

Insights into the complex morphology and physical processes of G29.

Abstract

In previous works, we have investigated the star-forming region G29.96$-$0.02 where the massive young stellar object (MYSO) G29.862$-$0.0044 (hereafter G29) is embedded in a hot molecular core. In one of them, of multiwavelength nature, using data from the Atacama Submillimeter Telescope Experiment (ASTE), data from the Atacama Large Millimeter Array (ALMA), and photometric data from NIRI-Gemini, G29 was investigated at different spatial scales. However, the intriguing morphology of G29 in the near-infrared, together with the distribution of the associated molecular gas, reveals that the star-formation scenario is far from being understood. This work incorporates the analysis of the emission of several molecular lines acquired with ALMA that were not previously examined (eg.,~CH$_{3}$OH, HC$_{3}$N, H$_{ 2}$CO, C$^{34}$S, H$_{2}$CS) as well as a new determination of the temperature of the region. Additionally, we present the progress of results obtained through new observations in the near-infrared, in this case spectroscopic, using NIFS-Gemini, and in radio continnum obtained with the Karl G. Jansky Very Large Array (JVLA). This research allows us to carry out a detailed chemical study of the region, which will contribute to the understanding of the physical processes involved in the high-mass star formation.