The rotation curves of regularly rotating disc galaxies are a unique probe of the gravitational potential and dark matter distribution. Until recently, matter decomposition of rotation curves at $z>0.5$ was challenging, not only due to the lack of high resolution kinematic data but also of both suitable photometry to accurately trace the stellar surface density and spatially-resolved sub-mm observations to trace the cold gas distribution. In this paper, we analyse three galaxies from the Archival Large Program to Advance Kinematic Analysis (ALPAKA) sample, combining highly resolved cold gas observations from ALMA with rest-frame near-infrared imaging from JWST to investigate their dynamical properties and constrain their dark matter halos. The galaxies, initially classified as regularly rotating discs based on ALMA observations alone, appear in JWST as extended and symmetric stellar discs with spiral arms. Our dynamical models reproduce the rotation of the discs in the outer parts well, but they systematically underpredict the inner rotation velocities, revealing a deficit of central mass relative to the data. This discrepancy indicates either an underestimation of the bulge masses due to variations in the stellar mass-to-light ratio or dust attenuation or the presence of overmassive black holes. Alternatively, it may suggest departures from standard dark-matter halo profiles, including enhanced central concentrations.
JWST Discovery of Strong Lensing from a Galaxy Cluster at Cosmic Noon: Giant Arcs and a Highly Concentrated Core of XLSSC 122
California Institute of Technology（加州理工学院）；Yonsei University（延世大学）；University of California, Davis（加州大学戴维斯分校）；Korea Astronomy and Space Science Institute（韩国天体宇宙科学研究所）；University of California, Los Angeles（加州大学洛杉矶分校）
An Active Galaxy Cluster Merger at Cosmic Noon Revealed by JWST Weak Lensing and Multiwavelength Probes
Yonsei University（延世大学）；California Institute of Technology（加州理工学院）；University of California Davis（加州大学戴维斯分校）；University of Oxford（牛津大学）；University of California, Los Angeles（加州大学洛杉矶分校）
INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所-布拉拉天文台）；Como Lake centre for AstroPhysics (CLAP)（科莫湖天体物理中心）；INFN, Sezione di Milano-Bicocca（意大利国家核物理研究所-米兰比可卡分校分部）
The onset of stellar bars at Cosmic Noon. Bar-driven quenching and AGN co-evolution in a mature disc galaxy
Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心）；Departamento de Astronomía, Universidad de La Serena（拉塞雷纳大学天文系）；Instituto de Astrofísica de Canarias（加那利群岛天体物理学研究所）；Departamento de Astrofísica de la Universidad de La Laguna（拉古纳大学天体物理学系）；Department of Physics, Faculty of Science, Ferdowsi University of Mashhad（马什哈德菲尔道西大学理学院物理系）；INAF – Osservatorio Astronomico di Padova（帕多瓦天文台）；Dipartimento di Fisica e Astronomia “G. Galilei”, Università di Padova（帕多瓦大学伽利略物理与天文学系）
Resolving the Assembly of Disk Galaxies from the Epoch of Reionisation to Cosmic Noon
Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天体物理与天文学研究学院）；Istituto Nazionale di Astrofisica (INAF)（意大利国家天体物理研究所）；Scuola Normale Superiore（比萨高等师范学院）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天体物理研究所）；DARK, Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯玻尔研究所DARK中心）
Constraining dark matter halo profiles and galaxy formation models using spiral arm morphology. II. Dark and stellar mass concentrations for 13 nearby face-on galaxies
NIHAO XXVIII: Collateral effects of AGN on dark matter concentration and stellar kinematics
虽然活动星系核（AGN）的反馈需要在星系的模拟，以调节恒星的形成，进一步的下游效应的暗物质分布的晕和恒星运动学的中央星系可以预期。我们结合数值模拟的星系和无AGN物理的一百天体（NIHAO）研究AGN的暗物质轮廓和中央恒星旋转的宿主星系的影响。具体地说，我们研究了活动星系核反馈如何影响浓度-晕质量（$c-M$）关系和恒星自旋参数（$λ_R$）。我们发现活动星系核物理是至关重要的，以减少模拟的大质量（$\gtrsim 10^{12}$ M $_\odot$）星系的中心密度，并使其浓度与斯皮策测光和精确旋转曲线（SPITZER）样品的结果一致。同样地，活动星系核反馈在复制ATLAS $^{3\text{D}}$巡天观测到的慢旋子和快旋子之间的二分法中起着关键作用。由于AGN反馈，没有恒星形成抑制，快速旋转的数量大大超过了观测限制。我们的研究表明，有几个附带的影响，支持活动星系核反馈在星系形成的重要性，这些影响可以用来限制其实施的数值模拟。
Do halos that form early, have high concentration, are part of a pair, or contain a central galaxy potential host more pronounced planes of satellite galaxies?
NOEMA3D: Resolving radial gas flows in disk galaxies at z~1.1-1.6 with high-resolution CO observations
Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理研究所）；Departments of Physics and Astronomy, University of California, Berkeley（加州大学伯克利分校物理与天文学系）；Institut de Radioastronomie Millimétrique (IRAM)（毫米波射电天文研究所）；Max-Planck-Institut für Astrophysik (MPA)（马克斯·普朗克天体物理研究所）；Department of Physics and Astronomy “Augusto Righi”, University of Bologna（博洛尼亚大学“奥古斯托·里吉”物理与天文学系）；INAF – Astrophysics and Space Science Observatory of 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）
