Pulsar timing arrays (PTAs) are sensitive to oscillations in the gravitational potential along the line-of-sight due to ultralight particle pressure. We calculate the probing power of PTAs for ultralight bosons across all frequencies, from those larger than the inverse observation time to those smaller than the inverse distance to the pulsar. We show that since the signal amplitude grows comparably to the degradation in PTA sensitivity at frequencies smaller than inverse observation time, the discovery potential can be extended towards lower masses by over three decades, maintaining high precision. We demonstrate that, in the mass range $10^{-26} -10^{-23}$ eV, existing 15-year PTA data can robustly detect or rule out an ultralight component down to $O(1 - 10)\%$ of the total dark matter. Non-detection, together with other bounds in different mass ranges, will imply that ultralight scalar/axion can comprise at most $1-10\%$ of dark matter in the $10^{-30}\!-\!10^{-17}$ eV range. With 30 years of observation, current PTAs can extend the reach down to $0.1-1 \%$, while next-generation PTAs such as SKA can attain the $0.01-0.1\%$ precision. We generalize the analysis and derive predictions for ultralight spin-1 vector (i.e. dark photon) and spin-2 tensor dark components.
Angular correlation and deformed Hellings-Downs curve from spin-2 ultralight dark matter
School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, UCAS（基础物理与数学科学学院，杭州高等研究院，中国科学院大学）；School of Physical Science and Technology, Ningbo University（宁波大学物理科学与技术学院）；CAS Key Laboratory of Theoretical Physics, Institute of Theoretical Physics, Chinese Academy of Sciences（中国科学院理论物理研究所，理论物理国家重点实验室）；University of Chinese Academy of Sciences（中国科学院大学）；National Astronomy Observatories, Chinese Academy of Science（中国科学院国家天文台）；International Center for Theoretical Physics Asia-Pacific（亚太理论物理中心）
Probing Ultralight Axion-like Dark Matter: A Pulsar Timing Arrays-Pulsar Polarization Arrays Synergy
Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所）；School of Physics Sciences, University of Chinese Academy of Sciences（中国科学院大学物理科学学院）；Department of Physics and Jockey Club Institute for Advanced Study, The Hong Kong University of Science and Technology（香港科技大学物理系及赛马会高等研究院）；Hunan Normal University（湖南师范大学）；Australia Telescope National Facility, CSIRO, Space and Astronomy（CSIRO空间与天文部澳大利亚望远镜国家设施）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（阿尔伯特·爱因斯坦研究所））；Leibniz Universit¨at Hannover（汉诺威莱布尼茨大学）；School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）；Department of Physics, Faculty of Arts and Sciences, Beijing Normal University, Zhuhai（北京师范大学珠海校区艺术与理学院物理系）；Hangzhou Institute for Advanced Study, UCAS（中国科学院大学杭州高等研究院）；University of Chinese Academy of Sciences（中国科学院大学）；Institute of Theoretical Physics, Chi（理论物理研究所）
Probing Spin-2 Ultralight Dark Matter with Space-based Gravitational Wave Detectors in the mHz Regime
Hangzhou Institute for Advanced Study, UCAS（杭州高等研究院，中国科学院大学）；University of Chinese Academy of Sciences（中国科学院大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Ningbo University（宁波大学）；Institute of Theoretical Physics, Chinese Academy of Sciences（中国科学院理论物理研究所）
Sensitivity of binary pulsar timing to spin-0 and spin-1 ultralight dark matter
Universidad de Buenos Aires, Facultad de Ciencias Exactas y Naturales（布宜诺斯艾利斯大学，理学院）；CONICET, Instituto de Física de Buenos Aires (IFIBA)（阿根廷国家科学研究委员会，布宜诺斯艾利斯物理研究所）
Probing Extragalactic Ultralight Axion Dark Matter with Decade-Long Blazar Optical Polarimetry of 1ES 1959+650
Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；School of Astronomy and Space Sciences, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）
Prospects for probing ultralight primordial black holes using the stochastic gravitational-wave background induced by primordial curvature perturbations
Binary Pulsars as probes for Spin-2 Ultralight Dark Matter
双星可以成为超轻暗物质的优秀探测器。我们考虑的情况下，后者是由一个自旋2场。暗物质场的相干振荡扰动了双星系统的动力学，导致与双星系统共振的质量的长期效应。对于范围$10^{-23}$电子伏特$\lesssim m \lesssim 10^{-17}$电子伏特，我们表明，目前的定时数据可能会限制暗物质的普遍耦合强度，以普通物质在$α\simeq 10^{-5}$的水平。
Correlated signals of ultralight scalar dark matter in pulsar timing
University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of Florida（佛罗里达大学）；University of California Berkeley（加州大学伯克利分校）；University of California, San Diego（加州大学圣迭戈分校）；Imperial College（帝国理工学院）；Swarthmore College（斯沃斯莫尔学院）；University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）
Precision Solar System Dynamics for Ultralight Dark Matter Search
Sapienza Università di Roma（罗马大学）；INFN Roma1（意大利国家核物理研究所罗马第一分部）；Université Paris-Saclay（巴黎萨克雷大学）；CNRS（法国国家科学研究中心）；CEA（法国原子能和替代能源委员会）；Institut de Physique Théorique（理论物理研究所）；Universität Bonn（波恩大学）
Ultralight time-oscillating scalars from magnetized compact stars: electrophilic radiation and photon propagation effects
Durham University（杜伦大学）；INFN, Gruppo collegato di Salerno（意大利国家核物理研究所萨莱诺协作组）；Dipartimento di Fisica E.R. Caianiello, Università di Salerno（萨莱诺大学E.R. Caianiello物理系）
The Atacama Cosmology Telescope: Probing new signatures of ultralight axions with gravitational lensing
University of Pennsylvania（宾夕法尼亚大学）；King’s College London（伦敦国王学院）；Imperial College London（帝国理工学院）；Dunlap Institute for Astronomy and Astrophysics, University of Toronto（多伦多大学邓普天文学与天体物理研究所）；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）；Cardiff University（卡迪夫大学）；Princeton University（普林斯顿大学）；University of Southern California（南加州大学）；Institute for Advanced Study（高等研究院）
Tunneling and tidal stripping in multifield ultralight dark matter halos
Center for Theoretical Physics—a Leinweber Institute, Massachusetts Institute of Technology（麻省理工学院莱因韦伯理论物理中心）；Department of Physics, Harvard University（哈佛大学物理系）；Universidad Autonoma de Madrid（马德里自治大学）；IFT-UAM/CSIC（乌阿姆/西班牙国家科学研究委员会理论物理研究所）
Identifying Monochromatic Signals in LISA and Taiji via Spectral Split: Gravitational Waves versus Ultralight Dark Matter
University of Chinese Academy of Sciences (UCAS)（中国科学院大学）；Hangzhou Institute for Advanced Study, UCAS（杭州高等研究院，中国科学院大学）；Institute of Theoretical Physics, Chinese Academy of Sciences（中国科学院理论物理研究所）；International Center for Theoretical Physics Asia-Pacific（亚太理论物理中心）；School of Astronomy and Space Science, UCAS（天文学与空间科学学院，中国科学院大学）
