Bose-Einstein-condensed dark matter, also called scalar-field dark matter (SFDM), has become a popular alternative to cold dark matter (CDM), because it predicts galactic cores, in contrast to the cusps of CDM halos ("cusp-core problem"). We continue the study of SFDM with a strong, repulsive self-interaction; the Thomas-Fermi regime of SFDM (SFDM-TF). In this model, structure formation is suppressed below a scale related to the TF radius $R_\text{TF}$, which is close to the radius of central cores in these halos. We investigate for the first time the impact of baryons onto realistic galactic SFDM-TF halo profiles by studying the process of adiabatic contraction (AC) in such halos. In doing so, we first analyse the underlying quantum Hamilton-Jacobi framework appropriate for SFDM and calculate dark matter orbits, in order to verify the validity of the assumptions usually required for AC. Then, we calculate the impact of AC onto SFDM-TF halos of mass $\sim 10^{11}~M_{\odot}$, with various baryon fractions and core radii, $R_\text{TF} \sim (0.1 - 4)$ kpc, and compare our results with observational velocity data of dwarf galaxies. We find that AC-modified SFDM-TF halos with kpc-size core radii reproduce the data well, suggesting stellar feedback may not be required. On the other hand, halos with sub-kpc core radii face the same issue than CDM, in that they are not in accordance with galaxy data in the central halo parts.
Revisiting the X-ray - Mass scaling relations of Early-type Galaxies with the Mass of their Globular Cluster Systems as a Proxy for the Total Galaxy Mass
CROCODILE-SIDM: Tidal Formation of Dark Matter-Deficient Galaxies as a Test Case
The University of Osaka（大阪大学）；The University of Tokyo（东京大学）；University of Nevada, Las Vegas（内华达大学拉斯维加斯分校）；EPFL（洛桑联邦理工学院）；Excellence Cluster ORIGINS（ORIGINS卓越集群）；European Southern Observatory (ESO)（欧洲南方天文台）；Universitäts-Sternwarte, Fakultät für Physik（大学天文台，物理学院）
NIHAO-XXIII: Dark Matter density shaped by Black Hole feedback
我们提出了一个系统的分析反应的暗物质分布到星系形成跨越超过八个数量级的恒星质量。我们扩展了NIHAO-IV论文（Tollet等人）中提出的先前工作。通过增加46个新的高分辨率模拟的大质量星系进行列入黑洞反馈。我们表明，外流产生的活动星系核能够部分抵消暗物质收缩，由于大型中央恒星组成的大规模晕。净效应是放松的中央暗物质分布，移动到一个不太尖的密度分布在晕质量大于$\approx 3 \times 10^{12}$ M $_{\odot}$。密度剖面斜率平均值（$α$）周围的散射是相当恒定的（$Δα\approx 0.3$），除了在$10^{12}$ M $_{\odot}$周围有晕质量的星系，在从恒星到活动星系核反馈主导系统的过渡中，散射几乎增加了三倍。我们提供了有用的拟合公式的斜率的暗物质密度剖面的维里半径的百分之几为整个恒星质量范围：$10^5-10^{12}$ M $_{\odot}$（$2 \times 10^9-5 \times 10^{13}$ M $_{\odot}$晕质量）。
Lower central dark matter densities in nearby galaxies than predicted by simulations
Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；School of Astronomy and Space Sciences, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；Dipartimento di Fisica e Astronomia “Augusto Righi”, Alma Mater Studiorum Università di Bologna（博洛尼亚大学物理与天文学系）；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空间科学与天体物理观测站）；INFN-Sezione di Bologna（意大利国家核物理研究所博洛尼亚分部）；State Key Laboratory of Radio Astronomy and Technology, National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台射电天文与技术重点实验室）；School of Physics and Astronomy, Beijing Normal University（北京师范大学物理学部）；Department of Astronomy, Tsinghua University（清华大学天文系）
The dark side of early galaxies: $\texttt{geko}$ uncovers dark-matter fractions at $z\sim4-6$
University of Cambridge（剑桥大学）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Cavendish Laboratory, University of Cambridge（剑桥大学卡文迪许实验室）；Department of Physics, University of Oxford（牛津大学物理系）；University of Oxford（牛津大学）；Centre for Astrophysics Research, Department of Physics, Astronomy and Mathematics, University of Hertfordshire（赫特福德大学物理、天文与数学系天体物理学研究中心）；University of Hertfordshire（赫特福德大学）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；University of Arizona（亚利桑那大学）
