We report the Fermi Large Area Telescope (Fermi-LAT) detection of the gamma-ray emission towards the young massive star cluster RSGC 1. Using the latest source catalog and diffuse background models, we found that the diffuse gamma-ray emission in this region can be resolved into three different components. The GeV gamma-ray emission from the region HESS J1837-069 has a photon index of 1.83 $\pm$ 0.08. Combining with the HESS and MAGIC data, we argue that the gamma-ray emission in this region likely originate from a pulsar wind nebula (PWN). The gamma-ray emission from the northwest part (region A) can be modelled by an ellipse with the semimajor and semiminor axis of 0.5$^{\circ}$ and 0.25$^{\circ}$, respectively. The GeV emission has a hard spectrum with a photon index of 2.05 $\pm$ 0.02 and is partially coincide with the TeV source MAGIC J1835-069. The possible origin of the gamma-ray emission in this region is the interaction of the cosmic rays (CRs) accelerated by SNR G24.7+0.6 or/and the OB cluster G25.18+0.26 with the surrounding gas clouds. The GeV gamma-ray emission from the southeast region (region B) can be modeled as an ellipse with the semimajor and semiminor axis of 0.9$^{\circ}$ and 0.5$^{\circ}$, respectively, and also reveals a hard gamma-ray spectrum. We argue that the most probable origin is the interaction of the accelerated protons in the young massive star cluster RSGC 1 with ambient gas clouds, and the total cosmic-ray (CR) proton energy is estimated to be as high as $\sim$ 1x10$^{50}$ erg.
Diffuse gamma-ray emission in the vicinity of open cluster Berkeley 87
Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Shanghai Key Laboratory of Space Navigation and Positioning Techniques（上海市空间导航与定位技术重点实验室）；Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交通大学李政道研究所）
Spectral and spatial variations of the diffuse gamma-ray background in the vicinity of the Galactic plane and possible nature of the feature at 130 GeV
Diffuse neutrino flux from coronal magnetospheric current sheets of accreting black holes
National and Kapodistrian University of Athens（雅典国立卡波迪斯特里安大学）；Institute of Accelerating Systems and Applications（加速系统与应用研究所）；Columbia University（哥伦比亚大学）；Flatiron Institute（平顿研究所）
Diagnosing the AGN population origin of TeV neutrinos with their spatial correlation
School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Key laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education（现代天文学和天体物理学教育部重点实验室（南京大学））；Tianfu Cosmic Ray Research Center（天府宇宙线研究中心）
Extended gamma-ray emission in the vicinity of the Westerlund 1 massive star cluster and Kes 41 supernova remnant seen by the Fermi Large Area Telescope
Univ Toulouse, CNES, CNRS, IRAP（图卢兹大学，法国国家空间研究中心，法国国家科学研究中心，天体物理研究所）；Institut Supérieur de l’Aéronautique et de l’Espace (ISAE-Supaero)（高级航空与航天学院）；Max-Planck-Institut für Kernphysik（马克斯·普朗克核物理研究所）；Université Bordeaux, CNRS, LP2I Bordeaux, UMR 5797（波尔多大学，法国国家科学研究中心，波尔多强相互作用与粒子物理研究所）；INAF Osservatorio Astrofisico Arcetri（意大利国家天体物理研究所阿切特里天文台）
Enhancement of the 6.4 keV line in the inner Galactic ridge: Proton-induced fluorescence?
对于银河系弥漫X射线辐射的起源，特别是来自中性和高度电离原子的铁谱线的起源，一个普遍的想法是许多激变变星和日冕活动双星的叠加。在这种情况下，流量应该对称地分布在相对于人马座A $^*$的平面上的东西之间，因为由红外观测确定的恒星质量分布是近似对称的。这种对称性被确认为高度电离的铁线以及连续发射。然而，在银河系中心的近东侧，中性铁谱线比近西侧明显过剩，过剩辐射的通量分布与分子柱密度有很好的相关性。过量发射的X射线谱由幂律连续谱加上6.4 keV的线描述，该线具有$\sim1.3$ keV的大等效宽度，这很难用低能电子轰击方案来解释。过量辐射的经度和纬度分布不利于X射线辐射，无论是人马座A $^*$还是附近的X射线双星。那么低能质子轰击是最可能的起源，尽管需要0.1-1000 MeV的高能量密度$\sim 80$ eV cm $^{-3}$，并且附近没有常规的质子源。
