Mass models of galactic disks traditionally rely on axisymmetric density and rotation curves, paradoxically acting as if their most remarkable asymmetric features, such as lopsidedness or spiral arms, were not important. In this article, we relax the axisymmetry approximation and introduce a methodology that derives 3D gravitational potentials of disk-like objects and robustly estimates the impacts of asymmetries on circular velocities in the disk midplane. Mass distribution models can then be directly fitted to asymmetric line-of-sight velocity fields. Applied to the grand-design spiral M99, the new strategy shows that circular velocities are highly nonuniform, particularly in the inner disk of the galaxy, as a natural response to the perturbed gravitational potential of luminous matter. A cuspy inner density profile of dark matter is found in M99, in the usual case where luminous and dark matter share the same center. The impact of the velocity nonuniformity is to make the inner profile less steep, although the density remains cuspy. On another hand, a model where the halo is core dominated and shifted by 2.2-2.5 kpc from the luminous mass center is more appropriate to explain most of the kinematical lopsidedness evidenced in the velocity field of M99. However, the gravitational potential of luminous baryons is not asymmetric enough to explain the kinematical lopsidedness of the innermost regions, irrespective of the density shape of dark matter. This discrepancy points out the necessity of an additional dynamical process in these regions: possibly a lopsided distribution of dark matter.
Mapping the Asymmetric Thick Disk: II Distance, Size and Mass of the Hercules Thick Disk Cloud
武仙座厚盘云（Larsen et al. 2008）最初被发现是银河系象限1和象限4之间数量过多的微弱蓝色恒星。云的起源可能是与盘条、三轴厚盘或合并残余物或流的相互作用。为了更好地绘制云沿视线的空间范围，我们已经获得了63个区域中120万颗恒星的多色UBVR测光，每个区域约为1平方度。我们对超出明显边界的场的分析已经排除了三轴厚盘作为可能的解释（Larsen，Humphreys和Cabanela 2010）在本文中，我们提出了我们所有场的恒星计数结果，确定了视线上和视线上的过密度的空间范围，并估计了云的大小和质量。使用测光表，造成过量的恒星距离太阳在1到6千秒差距之间，在银河平面上方0.5 - 4千秒差距，在我们的视线上延伸大约3-4千秒差距。因此，它是银河系中的一个主要的底层结构。沿着我们视线的过剩分布与圆盘中棒的密度轮廓相对应，它最远的恒星直接在棒的上方。我们也透过云看到了它的另一面。在包含云的整个500平方度的天空中，我们估计有超过560万颗恒星和190万个太阳质量的物质。如果超密度与棒有关，它将超过14亿颗恒星和超过5000万个太阳质量。最后，我们认为武仙座-天鹰座云（Belokurov et al. 2007）实际上是武仙座厚盘云。
Twisted Pseudodisk and Asymmetric Mass Accretion on the Circumstellar Disk
Kyushu University（九州大学）；University of Western Ontario（韦仕敦大学）；Canadian Institute for Theoretical Astrophysics, University of Toronto（多伦多大学理论天体物理研究所）；Kanagawa University（神奈川大学）
Early Planet Formation in Embedded Disks (eDisk). XVIII. Indication of a possible spiral structure in the dust-continuum emission of the protostellar disk around IRAS 16544-1604 in CB 68
Kagoshima University（鹿儿岛大学）；National Astronomical Observatory of Japan（日本国立天文台）；Academia Sinica Institute of Astronomy & Astrophysics（中央研究院天文及天文物理学研究所）
Mapping the Milky Way with Gaia Bp/Rp spectra-IV: the broken and asymmetric density profile of the stellar disk traced by a large sample of red clumps
Institute of Astronomy and Physics, Inner Mongolia University（内蒙古大学天文与物理学院）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Universidad de La Laguna（拉各纳大学）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；Key Laboratory of Survey Science of Yunnan Province, Yunnan University（云南省测绘科学重点实验室）
Twisted Pseudodisk and Asymmetric Mass Accretion on the Circumstellar Disk II: Parameter Survey
Kyushu University（九州大学）；University of Western Ontario（韦仕敦大学）；Kanagawa University（神奈川大学）；University of Tokyo（东京大学）；Canadian Institute for Theoretical Astrophysics, University of Toronto（多伦多大学加拿大理论天体物理研究所）
Twisted doughnuts: Thick disk torus around equatorial asymmetric black hole
RIKEN iTHEMS（理化学研究所 iTHEMS）；Center of Applied Space Technology and Microgravity (ZARM), University of Bremen（不来梅大学应用空间技术与微重力中心（ZARM））；Gauss-Olbers Space Technology Transfer Center, University of Bremen（不来梅大学高斯-奥尔伯斯空间技术转移中心）；Leibniz University of Hannover（汉诺威莱布尼茨大学）
Discovery of Asymmetric Spike-like Structures of the 10 au Disk around the Very Low-luminosity Protostar Embedded in the Taurus Dense Core MC 27/L1521F with ALMA
Early Planet Formation in Embedded Disks (eDisk) XVI: An asymmetric dust disk driving a multi-component molecular outflow in the young Class 0 protostar GSS30 IRS3
