Institutional Repository of Radio Astronomy Research Laboratory
| High-precision search for dark photon dark matter with the Parkes Pulsar Timing Array | |
Xue, Xiao1; Xia, Zi-Qing2; Zhu, Xingjiang3,4,5; Zhao, Yue6; Shu, Jing7,8,9,10,11,12; Yuan, Qiang2,10,13; Bhat, N. D. Ramesh14; Cameron, Andrew D.5,15,16; Dai, Shi15,17; Feng, Yi18; Goncharov, Boris4,5; Hobbs, George15; Howard, Eric15,19; Manchester, Richard N.15; Parthasarathy, Aditya16,20; Reardon, Daniel J.5,16; Russell, Christopher J.21; Shannon, Ryan M.5,16; Spiewak, Renee16,22; Thyagarajan, Nithyanandan23; Wang, Jingbo24 ; Zhang, Lei25; Zhang, Songbo26
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| 2022-02-22 | |
| Source Publication | Physical Review Research
 |
| ISSN | 2643-1564 |
| Volume | 4Issue:1Pages:L012022 |
| Contribution Rank | 24 |
| Abstract | The nature of dark matter remains obscure in spite of decades of experimental efforts. The mass of dark matter candidates can span a wide range, and its coupling with the Standard Model sector remains uncertain. All these unknowns make the detection of dark matter extremely challenging. Ultralight dark matter, with m10-22 eV, is proposed to reconcile the disagreements between observations and predictions from simulations of small-scale structures in the cold dark matter paradigm while remaining consistent with other observations. Because of its large de Broglie wavelength and large local occupation number within galaxies, ultralight dark matter behaves like a coherently oscillating background field with an oscillating frequency dependent on its mass. If the dark matter particle is a spin-1 dark photon, such as the U(1)B or U(1)B-L gauge boson, it can induce an external oscillating force and lead to displacements of test masses. Such an effect would be observable in the form of periodic variations in the arrival times of radio pulses from highly stable millisecond pulsars. In this study, we search for evidence of ultralight dark photon dark matter (DPDM) using 14-year high-precision observations of 26 pulsars collected with the Parkes Pulsar Timing Array. While no statistically significant signal is found, we place constraints on coupling constants for the U(1)B and U(1)B-L DPDM. Compared with other experiments, the limits on the dimensionless coupling constant achieved in our study are improved by up to two orders of magnitude when the dark photon mass is smaller than 310-22 eV (10-22 eV) for the U(1)B (U(1)B-L) scenario. 2022 authors. Published by the American Physical Society. |
| Keyword | Photons Bosons Dark Matter Galaxies Pulsars Timing circuits |
| DOI | 10.1103/PhysRevResearch.4.L012022 |
| URL | 查看原文 |
| Indexed By | EI |
| Language | 英语 |
| Citation statistics | |
| Document Type | 期刊论文 |
| Identifier | http://ir.xao.ac.cn/handle/45760611-7/5147 |
| Collection | 射电天文研究室_脉冲星研究团组 |
| Affiliation | 1.II. Institut für Theoretische Physik, Universität Hamburg, Luruper Chaussee 149, D-22761 Hamburg, Germany; 2.Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China; 3.Advanced Institute of Natural Sciences, Beijing Normal University at Zhuhai 519087, China; 4.School of Physics and Astronomy, Monash University, Clayton, Victoria 3800, Australia; 5.OzGrav: The ARC Centre of Excellence for Gravitational Wave Discovery, Hawthorn, Victoria 3122, Australia; 6.Department of Physics and Astronomy, University of Utah, Salt Lake City, Utah 84112, USA; 7.CAS Key Laboratory of Theoretical Physics, Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100190, China; 8.School of Physical Sciences, University of Chinese Academy of Sciences, Beijing 100049, China; 9.CAS Center for Excellence in Particle Physics, Beijing 100049, China; 10.Center for High Energy Physics, Peking University, Beijing 100871, China; 11.School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, University of Chinese Academy of Sciences, Hangzhou 310024, China; 12.International Centre for Theoretical Physics Asia-Pacific, Beijing/Hangzhou, China; 13.School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China; 14.International Centre for Radio Astronomy Research, Curtin University, Bentley, Western Australia 6102, Australia; 15.Australia Telescope National Facility, CSIRO Astronomy and Space Science, Epping, New South Wales 1710, Australia; 16.Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia; 17.School of Science, Western Sydney University, Locked Bag 1797, Penrith South DC, NSW 2751, Australia; 18.Research Institute of Artificial Intelligence, Zhejiang Lab, Hangzhou, Zhejiang 311121, China; 19.Macquarie University, Department of Physics and Astronomy, Sydney, New South Wales 2109, Australia; 20.Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany; 21.CSIRO Scientific Computing, Australian Technology Park, Alexandria, New South Wales 1435, Australia; 22.Jodrell Bank Centre for Astrophysics, University of Manchester, Manchester M13 9PL, United Kingdom; 23.National Radio Astronomy Observatory, Socorro, New Mexico 87801, USA; 24.Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, Xinjiang 830011, China; 25.School of Physics and Technology, Wuhan University, Wuhan 430072, China; 26.Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China |
| Recommended Citation GB/T 7714 | Xue, Xiao,Xia, Zi-Qing,Zhu, Xingjiang,et al. High-precision search for dark photon dark matter with the Parkes Pulsar Timing Array[J]. Physical Review Research,2022,4(1):L012022. |
| APA | Xue, Xiao.,Xia, Zi-Qing.,Zhu, Xingjiang.,Zhao, Yue.,Shu, Jing.,...&Zhang, Songbo.(2022).High-precision search for dark photon dark matter with the Parkes Pulsar Timing Array.Physical Review Research,4(1),L012022. |
| MLA | Xue, Xiao,et al."High-precision search for dark photon dark matter with the Parkes Pulsar Timing Array".Physical Review Research 4.1(2022):L012022. |
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| Xue-2022-High-precis（318KB） | 期刊论文 | 出版稿 | 开放获取 | CC BY-NC-SA | View Application Full Text | |
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