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Aims: We study the molecular environment of the luminous blue variable starG24.73+0.69 to investigate the origin of the two infrared shells around thismassive star and to determine its effects on the surrounding interstellarmedium. Methods: We analyze the distribution of the molecular gas using the13CO J=1-0 emission extracted from the Galactic Ring Survey. We use near- andmid-infrared data from 2MASS and GLIMPSE to identify the young stellar objectsin the field. Results: We discover the molecular counterpart of the outerinfrared shell around G24.73+0.69. The CO shell was probably blown by thestellar wind of the star mainly during its main sequence phase. We also findmolecular gas that corresponds to the inner infrared shell, although its originremains uncertain. We find seven young stellar objects upon the molecularmaterial, whose birth might have been triggered by the stellar wind of theluminous blue variable star. We suggest that both G24.73+0.69 and theprogenitor of the nearby supernova remnant G24.7+0.6 were formed from the samenatal cloud and represent the most evolved members of a so far undetectedcluster of other massive stars.

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