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We report on Mopra observations toward the young massive star cluster RSGC 1,adjoined by, and possibly associated with the gamma-ray source HESS J1837-069.We measure the CO (J=1-0) distribution around the cluster and gamma-ray source,and find that the cluster is slightly higher than the velocity rangesassociated with the Crux-Scutum arm. We reveal the cluster is associated withmuch less molecular gas compared with other young massive clusters in theGalaxy, Westerlund 1 (Wd 1) and 2 (Wd 2), which also radiate gamma-rays. Wefind no other structures that would otherwise indicate the action of supernovaremnants, and due to the lack of material which may form gamma-rays by hadronicinteraction, we conclude that the gamma-rays detected from HESS J1837-069 arenot created through proton-proton interactions, and may more plausiblyoriginate from the pulsar that was recently found near RSGC 1.

The Environment around the Young Massive Star Cluster RSGC 1 and HESS J1837-069