The Chinese Pulsar Timing Array Data Release I Single pulsar noise analysis
文献类型：期刊论文
| 作者 | Chen, Siyuan1,12; Xu, Heng2; Guo, Yanjun2,12; Wang, Bojun2; Caballero, R. Nicolas3,4; Jiang, Jinchen2; Xu, Jiangwei2,3,5; Xue, Zihan2,3,5; Lee, Kejia2,5,6,12; Yuan, Jianping7 |
| 刊名 | ASTRONOMY & ASTROPHYSICS
 |
| 出版日期 | 2025-07-07 |
| 卷号 | 699页码:A165 |
| 关键词 | gravitational waves methods: data analysis pulsars: general |
| ISSN号 | 0004-6361 |
| DOI | 10.1051/0004-6361/202452550 |
| 产权排序 | 8 |
| 英文摘要 | The Chinese Pulsar Timing Array (CPTA) has collected observations from 57 millisecond pulsars using the Five-hundred-meter Aperture Spherical Radio Telescope (FAST) for close to three years, for the purpose of searching for gravitational waves (GWs). To robustly search for ultra-low-frequency GWs, pulsar timing arrays (PTAs) need to use models to describe the noise from the individual pulsars. We report on the results from the single pulsar noise analysis of the CPTA data release I (DR1). Conventionally, power laws in the frequency domain are used to describe pulsar red noise and dispersion measurement (DM) variations over time. Employing Bayesian methods, we found the choice of number and range of frequency bins with the highest evidence for each pulsar individually. A comparison between a dataset using DM piecewise measured (DMX) values and a power-law Gaussian process to describe the DM variations shows strong Bayesian evidence in favour of the power-law model. Furthermore, we demonstrate that the constraints obtained from four independent software packages are very consistent with each other. The short time span of the CPTA DR1, paired with the large sensitivity of FAST, has proved to be a challenge for the conventional noise model using a power law. This mainly shows in the difficulty to separate different noise terms due to their covariances with each other. Nineteen pulsars are found to display covariances between the short-term white noise and long-term red and DM noise. With future CPTA datasets, we expect that the degeneracy can be broken. Finally, we compared the CPTA DR1 results against the noise properties found by other PTA collaborations. While we can see broad agreement, there is some tension between different PTA datasets for some of the overlapping pulsars. This could be due to the differences in the methods used to obtain the constraints or the different frequency range that is probed with the CPTA DR1, which probes a higher frequency range compared to the other PTAs. |
| WOS关键词 | LIMITS |
| 资助项目 | National SKA Program of China ; FAST Key project ; Chinese Academy of Sciences (NAOC) ; National Key Research and Development Program of China[2022YFC2205203] ; National Natural Science Foundation of China[12041303] ; National Natural Science Foundation of China[12250410246] ; National Natural Science Foundation of China[12173087] ; National Natural Science Foundation of China[12063003] ; China Postdoctoral Science Foundation[2023M743518] ; China Postdoctoral Science Foundation[2023M743516] ; Major Science and Technology Program of Xinjiang Uygur Autonomous Region[2022A03013-4] ; CAS-MPG LEGACY project ; Max-Planck Partner Group ; C*-SYSTEM of PSR@pku ; [2020SKA0120100] |
| WOS研究方向 | Astronomy & Astrophysics |
| 语种 | 英语 |
| WOS记录号 | WOS:001523444300003 |
| 出版者 | EDP SCIENCES S A |
| 资助机构 | National SKA Program of China ; FAST Key project ; Chinese Academy of Sciences (NAOC) ; National Key Research and Development Program of China ; National Natural Science Foundation of China ; China Postdoctoral Science Foundation ; Major Science and Technology Program of Xinjiang Uygur Autonomous Region ; CAS-MPG LEGACY project ; Max-Planck Partner Group ; C*-SYSTEM of PSR@pku |
| 源URL | [http://ir.xao.ac.cn/handle/45760611-7/7984]  |
| 专题 | 脉冲星研究团组 |
| 通讯作者 | Chen, Siyuan; Xu, Heng; Guo, Yanjun |
| 作者单位 | 1.Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China 2.Chinese Acad Sci, Natl Astron Observ, Beijing 100101, Peoples R China 3.Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China 4.Hellen Open Univ, Sch Sci & Technol, Patras 26335, Greece 5.Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China 6.Beijing Laser Accelerat Innovat Ctr, Beijing 101400, Peoples R China 7.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Xinjiang, Peoples R China 8.Chinese Acad Sci, Yunnan Astron Observ, Kunming 650216, Yunnan, Peoples R China 9.Lishui Univ, Inst Optoelect Technol, Lishui 323000, Zhejiang, Peoples R China 10.Chinese Acad Sci, Natl Time Serv Ctr, Xian 710600, Peoples R China |
| 推荐引用方式 GB/T 7714 | Chen, Siyuan,Xu, Heng,Guo, Yanjun,et al. The Chinese Pulsar Timing Array Data Release I Single pulsar noise analysis[J]. ASTRONOMY & ASTROPHYSICS,2025,699:A165. |
| APA | Chen, Siyuan.,Xu, Heng.,Guo, Yanjun.,Wang, Bojun.,Caballero, R. Nicolas.,...&Zhu, Yan.(2025).The Chinese Pulsar Timing Array Data Release I Single pulsar noise analysis.ASTRONOMY & ASTROPHYSICS,699,A165. |
| MLA | Chen, Siyuan,et al."The Chinese Pulsar Timing Array Data Release I Single pulsar noise analysis".ASTRONOMY & ASTROPHYSICS 699(2025):A165. |
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来源：新疆天文台
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