Gamma-ray observation towards the young massive star cluster NGC 6618 in the M17 region. (arXiv:2205.06430v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Liu_B/0/1/0/all/0/1">Bing Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_R/0/1/0/all/0/1">Rui-zhi Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Z/0/1/0/all/0/1">Zhiwei Chen</a>
Young massive clusters have been established as a new population of gamma-ray
sources and potential cosmic ray (CR) accelerators. In this paper, we report
the detection of gamma-ray emissions near the young star cluster NGC 6618,
which is one of the youngest star clusters in our Galaxy. The detected
gamma-ray emissions can be divided into two components. One component is
point-like and reveals harder spectrum, while the other is extended and with
softer spectrum. Such spectral features are significantly different from other
young massive clusters and may be due to the propagation effects of CRs
accelerated in NGC 6618.
Young massive clusters have been established as a new population of gamma-ray
sources and potential cosmic ray (CR) accelerators. In this paper, we report
the detection of gamma-ray emissions near the young star cluster NGC 6618,
which is one of the youngest star clusters in our Galaxy. The detected
gamma-ray emissions can be divided into two components. One component is
point-like and reveals harder spectrum, while the other is extended and with
softer spectrum. Such spectral features are significantly different from other
young massive clusters and may be due to the propagation effects of CRs
accelerated in NGC 6618.
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