The molecular gas around the luminous blue variable star G24.73+0.69

TL;DR

This study investigates the molecular environment of the luminous blue variable star G24.73+0.69, revealing its impact on surrounding gas, associated star formation, and suggesting a common origin with nearby supernova remnant G24.7+0.6.

Contribution

It provides the first detailed analysis of the molecular gas around G24.73+0.69, linking stellar winds to infrared shells and star formation, and proposing a shared origin with a nearby supernova remnant.

Findings

Discovered molecular counterpart of the outer infrared shell.

Found seven young stellar objects possibly triggered by stellar winds.

Suggested G24.73+0.69 and supernova remnant share a common natal cloud.

Abstract

Aims: We study the molecular environment of the luminous blue variable star G24.73+0.69 to investigate the origin of the two infrared shells around this massive star and to determine its effects on the surrounding interstellar medium. Methods: We analyze the distribution of the molecular gas using the 13CO J=1-0 emission extracted from the Galactic Ring Survey. We use near- and mid-infrared data from 2MASS and GLIMPSE to identify the young stellar objects in the field. Results: We discover the molecular counterpart of the outer infrared shell around G24.73+0.69. The CO shell was probably blown by the stellar wind of the star mainly during its main sequence phase. We also find molecular gas that corresponds to the inner infrared shell, although its origin remains uncertain. We find seven young stellar objects upon the molecular material, whose birth might have been triggered by the stellar wind of the luminous blue variable star. We suggest that both G24.73+0.69 and the progenitor of the nearby supernova remnant G24.7+0.6 were formed from the same natal cloud and represent the most evolved members of a so far undetected cluster of other massive stars.