Aims. To validate the Einstein equivalence principle (local position invariance) by limiting the fractional changes in the electron-to-proton mass ratio, mu = m_e/m_p, measured in Galactic plane objects. Methods. High resolution spectral observations of dark clouds in the inversion line of NH3(1,1) and pure rotational lines of other molecules (the so-called ammonia method) were performed at the Medicina 32-m and the Effelsberg 100-m radio telescopes to measure the radial velocity offsets, Delta RV = V_rot - V_inv, between the rotational and inversion transitions which have different sensitivities to the value of mu. Results. In our previous observations (2008-2010), a mean offset of <Delta RV> = 0.027+/-0.010 km/s [3 sigma confidence level (C.L.)] was measured. To test for possible hidden errors, we carried out additional observations of a sample of molecular cores in 2010-2013. As a result, a systematic error in the radial velocities of an amplitude ~0.02 km/s was revealed. The averaged offset between the radial velocities of the rotational transitions of HC3N(2-1), HC5N(9-8), HC7N(16-15), HC7N(21-20), and HC7N(23-22), and the inversion transition of NH3(1,1) <Delta RV> = 0.003+/-0.018 km/s (3 sigma C.L.). This value, when interpreted in terms of Delta mu/mu= (mu_obs - mu_lab)/mu_lab, constraints the mu-variation at the level of Delta mu/mu < 2*10^{-8} (3 sigma C.L.), which is the most stringent limit on the fractional changes in mu based on astronomical observations.
Evidence for an extended Galactic proton component beyond the cosmic-ray knee
State Key Laboratory of Dark Matter Physics, Tsung-Dao Lee Institute & School of Physics and Astronomy, Shanghai Jiao Tong University（暗物质物理国家重点实验室、李政道研究所及上海交通大学物理与天文学院）
The Effects of Cosmic Ray Protons on Galactic Nonthermal Filaments
University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；Joint ALMA Observatory（ALMA联合天文台）；National Radio Astronomy Observatory（美国国家射电天文台）；Villanova University（维拉诺瓦大学）
Interplay between Escaping Cosmic Rays and Interstellar Medium: Driving of Galactic Winds and Shaping the Local Proton Spectrum
Institute for Cosmic Ray Research, The University of Tokyo（东京大学宇宙射线研究所）；Department of Physics, Graduate School of Science, Nagoya University（名古屋大学理学研究科物理学系）
Particle Propagation in the Galactic Center and Spatial Distribution of Non-Thermal X-rays
我们表明，如果在14-40 keV范围内的银河系中心的非热辐射是由于逆韧致辐射的亚相对论质子，它们与热和冷馏分的星际介质的相互作用是同样重要的。我们的估计表明，在14-40 keV的范围内，从GC的总非热通量的约30%是在冷气体区域产生的，而其余的是由质子与热等离子体相互作用产生的。从6.7keV铁谱线的空间分布可以看出，热等离子体的空间分布具有很强的非均匀性，在分析质子在气相色谱中的传输时应考虑到这一点。从朱雀实验数据中我们得到了GC中次相对论质子扩散系数的独立估计值，其范围为$ 10^{26} - 10^{27}$ cm $^2$ s $^{-1}$
A Three-Dimensional Tomographic Reconstruction of the Galactic Cosmic-Ray Proton Density
Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）；Ludwig Maximilian University of Munich（慕尼黑路德维希-马克西米利安大学）；Max Planck Computing and Data Facility（马克斯·普朗克计算与数据中心）；Sorbonne Université（索邦大学）；Observatoire de Paris（巴黎天文台）；PSL Research University（PSL研究大学）；CNRS（法国国家科学研究中心）；Kavli Institute for Particle Astrophysics and Cosmology（卡弗里粒子天体物理与宇宙学研究所）；Stanford University（斯坦福大学）；RWTH Aachen University（亚琛工业大学）；Universität Innsbruck（因斯布鲁克大学）
Revisiting Rotation Measures from the Canadian Galactic Plane Survey: the Magnetic Field in the Disk of the Outer Galaxy
法拉第旋转提供了星际介质中磁场的有价值的示踪剂;法拉第旋转测量的目录为研究银河系磁场提供了关键的观测结果。我们提出了一个新的星表的旋转措施，来自加拿大银河平面调查，涵盖了大范围的银河平面跨越52度< l < 192度，-3度< b < 5度，以及南北纬度扩展约l ~ 105度。我们已经推导出旋转措施2234源（其中4个是已知的卫星），其中75%没有以前的测量，在一个面积约1300平方度。这些新的旋转测量将银河平面这一区域的测量密度增加了两倍。
Variable stars in the northern Galactic plane from KISOGP
我们使用木曾天文台施密特望远镜上的木曾宽视场照相机对北平面进行了大规模的调查。KISOGP（KWFC Intensive Survey of the Galactic Plane）计划在约320平方米的I波段进行了40-70历元的观测。从2012年开始的5年。极限星等约为16.5 in I。在迄今为止的数据分析中，我们探测到了数千颗变星，包括大约100颗造父变星和700多颗Miras。其中大约90%以前没有被报道为变星，这表明在银河系平面上仍然有许多相对明亮的变星。
