标题： 非常高能$γ$-射线从大麦哲伦星云中的年轻大质量星团发射出来 显示英文标题

标题： Very-high-energy $γ$-ray emission from young massive star clusters in the Large Magellanic Cloud

摘要： 蜘蛛星云位于大麦哲伦云中，以其高恒星形成活动而闻名。 其核心处存在年轻的巨大星团 R136，它提供了使星云在许多波长下如此明亮发光的大量能量。 最近，有建议称年轻的巨大星团也可能高效地产生高能宇宙射线，可能超过拍电子伏特的能量。 在此，我们报告通过数据的多组分、基于似然的建模，利用高空能立体系统从 R136 方向检测到非常高的能量 $\gamma$-射线辐射。 这支持了 R136 确实是一个非常强大的宇宙射线加速器的假设。 此外，从同一分析中，我们提供了对 30 Dor C 的 $\gamma$-射线辐射的更新测量，30 Dor C 是目前唯一在太赫兹能量下被探测到的超泡。 两个源在 $0.5\,\mathrm{TeV}$以上的 $\gamma$-射线光度为 $(2-3)\times 10^{35}\,\mathrm{erg}\,\mathrm{s}^{-1}$。 这比与银河系中最巨大的年轻星团 Westerlund 1 相关的 HESS J1646$-$458 的光度高出超过两倍。 Furthermore, the $\gamma$-ray emission from each source is extended with a significance of $>3\sigma$ and a Gaussian width of about $30\,\mathrm{pc}$. For 30 Dor C, a connection between the $\gamma$-ray emission and the nonthermal X-ray emission appears likely. Different interpretations of the $\gamma$-ray signal from R136 are discussed. 显示英文摘要

摘要： The Tarantula Nebula in the Large Magellanic Cloud is known for its high star formation activity. At its center lies the young massive star cluster R136, providing a significant amount of the energy that makes the nebula shine so brightly at many wavelengths. Recently, young massive star clusters have been suggested to also efficiently produce high-energy cosmic rays, potentially beyond PeV energies. Here, we report the detection of very-high-energy $\gamma$-ray emission from the direction of R136 with the High Energy Stereoscopic System, achieved through a multicomponent, likelihood-based modeling of the data. This supports the hypothesis that R136 is indeed a very powerful cosmic-ray accelerator. Moreover, from the same analysis, we provide an updated measurement of the $\gamma$-ray emission from 30 Dor C, the only superbubble detected at TeV energies presently. The $\gamma$-ray luminosity above $0.5\,\mathrm{TeV}$ of both sources is $(2-3)\times 10^{35}\,\mathrm{erg}\,\mathrm{s}^{-1}$. This exceeds by more than a factor of 2 the luminosity of HESS J1646$-$458, which is associated with the most massive young star cluster in the Milky Way, Westerlund 1. Furthermore, the $\gamma$-ray emission from each source is extended with a significance of $>3\sigma$ and a Gaussian width of about $30\,\mathrm{pc}$. For 30 Dor C, a connection between the $\gamma$-ray emission and the nonthermal X-ray emission appears likely. Different interpretations of the $\gamma$-ray signal from R136 are discussed.