We present the results of a new, non-parametric method to reconstruct the Galactic dark matter profile directly from observations. Using the latest kinematic data to track the total gravitational potential and the observed distribution of stars and gas to set the baryonic component, we infer the dark matter contribution to the circular velocity across the Galaxy. The radial derivative of this dynamical contribution is then estimated to extract the dark matter profile. The innovative feature of our approach is that it makes no assumption on the functional form nor shape of the profile, thus allowing for a clean determination with no theoretical bias. We illustrate the power of the method by constraining the spherical dark matter profile between 2.5 and 25 kpc away from the Galactic centre. The results show that the proposed method, free of widely used assumptions, can already be applied to pinpoint the dark matter distribution in the Milky Way with competitive accuracy, and paves the way for future developments.
Globular clusters in \textsc{OrbIT}: complete dynamical characterisation of the globular cluster population of the Milky Way through updated orbital reconstruction
Università degli Studi di Bologna（博洛尼亚大学）；INAF（意大利国家天体物理研究所）；Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Instituto Milenio de Astrofísica MAS（MAS 天体物理研究所）；Université Côte d’Azur（蔚蓝海岸大学）；Observatoire de la Côte d’Azur（蔚蓝海岸天文台）
Chemo-dynamical reconstruction of Milky Way globular cluster progenitors: Age-metallicity relations and the universality of multiple stellar populations
Dipartimento di Fisica e Astronomia “Augusto Righi”–Università di Bologna（博洛尼亚大学）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天文与空间科学观测站）；Berkeley Center for Cosmological Physics and Department of Physics, University of California, Berkeley（加州大学伯克利分校）；ICC, University of Barcelona（巴塞罗那大学）；ICREA（加泰罗尼亚高级研究学院）
Milky Way Dynamics Favor Dark Matter over Modified Gravity Models
Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；University of Science and Technology of China（中国科学技术大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Chinese Academy of Sciences（中国科学院大学）；University of Saint Andrews（圣安德鲁斯大学）
Detection of the Milky Way spiral arms in dust from 3D mapping
大型恒星巡天通过红化效应对星际尘埃很敏感。利用光度学和光谱学测量的反射率，以及单个恒星的三维（3D）位置，可以构建一个三维尘埃图。我们提出了第一个连续的尘埃分布图在银河系盘7千秒差距内100秒差距的银河系中平面，使用红团和巨星从SDSS APOGEE DR 14。我们使用基于高斯过程的非参数方法来映射灰尘密度，这是ISM的局部属性，而不是一个完整的量。该方法对3D空间中的点之间的灰尘相关性进行建模，并且可以捕获任意变化，不受预先指定的函数形式的约束。这产生了没有视线伪影的连续图。我们得到的地图追踪了当地银河系旋臂的一些特征，尽管该模型没有包含旋臂的先验建议，也没有任何银河系结构的基础模型。这是第一次在银河系的尘埃密度图中捕捉到如此明显的手臂结构。我们得到的地图还追踪了银河系中一些已知的巨大分子云，并对它们的距离进行了一些限制，其中一些距离迄今为止相对不确定。
