Self-interacting dark matter (SIDM) is an able alternative to collisionless dark matter. If dark matter does have self-interactions, we would expect this to cause a separation between the collisionless stars and the dark matter halo of a galaxy as it falls through a dark matter medium. For stars arranged in a disk, this would generate a U-shaped warp. The magnitude of this warping depends on the SIDM cross section, type of self-interaction, relative velocity of galaxy and background, halo structure, and density of the dark matter medium. In this paper, we set constraints on long-range (light mediator) dark matter self-interaction by means of this signal. We begin by measuring U-shaped warps in $3,213$ edge-on disk galaxies within the Sloan Digital Sky Survey. We then forward-model the expected warp from SIDM on a galaxy-by-galaxy basis by combining models of halo structure, density and velocity field reconstructions, and models for the dark matter interactions. We find no evidence for a contribution to the warps from SIDM. Our constraints are highly dependent on the uncertain velocities of our galaxies: for a normalized Rutherford-like cross section we find $\tildeσ/m_{\rm{DM}} \lesssim 3\times 10^{-13}~\rm{cm}^2/\rm{g}$ at fixed velocity $v = 300~\rm{km/s}$ -- a bound that scales roughly linearly with increasing $v$. In the appendix we translate these bounds into limits on the momentum transfer cross section, finding $σ_T(300~\rm{km/s})/m_{\rm{DM}} \lesssim 0.1~\rm{cm}^2/\rm{g}$. [abridged]
Testing the isothermal Jeans model for self-interacting dark matter halos in the collapse phase
School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；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）；Donostia International Physics Center (DIPC)（圣塞巴斯蒂安国际物理中心）；Department of Astronomy, Peking University（北京大学天文学系）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究所）；Department of Physics and Astronomy, University of California, Riverside（加州大学河滨分校物理与天文学系）
Survival of the most compact: the life and death of satellite halos in self-interacting dark matter
Goethe University（法兰克福歌德大学）；Donostia International Physics Center (DIPC)（圣塞巴斯蒂安国际物理中心）；Ludwig-Maximilians-Universität München（慕尼黑路德维希-马克西米利安大学）；Excellence Cluster ORIGINS（ORIGINS卓越集群）；The University of Texas at Austin（得克萨斯大学奥斯汀分校）；University of California - Irvine（加州大学尔湾分校）
Beyond $w_0-w_a$ and Phantom Crossing: Testing Models of Coupled Dark Sector
Instituto de Física Teórica da Universidade Estadual Paulista（圣保罗州立大学理论物理研究所）；ICTP South American Institute for Fundamental Research（国际理论物理中心南美基础研究所）；Department of Astronomy/Steward Observatory, University of Arizona（亚利桑那大学天文学系/斯图尔德天文台）
Testing the Direction of Dark Sector Interaction Using Late-Time Datasets
Department of Physics, St.Xavier’s College, Tribhuvan University（特莱布万大学圣泽维尔学院物理系）；School of Science & College of Graduate Studies, Walailak University（瓦拉柴拉科大学理学院及研究生院）；Department of Physics, Faculty of Science, Istanbul University（伊斯坦布尔大学理学院物理系）；Kimyo International University in Tashkent（塔什干金宇国际大学）
