期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 502, 期 1, 页码 478-493出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/staa3411
关键词
gravitational waves; methods: data analysis; pulsars: general
资金
- Commonwealth Government
- Australian Research Council [FL150100148]
- Australian Research Council Future Fellowship [FL150100148, FT150100281, FT190100155]
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav) [CE170100004]
- Youth Innovation Promotion Association of Chinese Academy of Sciences
- National Aeronautics and Space Administration (NASA)
- Australian Research Council [FL150100148] Funding Source: Australian Research Council
Pulsar timing array projects measure pulse arrival times of millisecond pulsars to detect nanohertz-frequency gravitational waves. Besides known noise sources, new sources have been identified, requiring robust statistical and physical models to improve sensitivity in gravitational wave detection. The detection of pulse profile variations emphasizes the need for efficient profile domain timing methods.
Pulsar timing array projects measure the pulse arrival times of millisecond pulsars for the primary purpose of detecting nanohertz-frequency gravitational waves. The measurements include contributions from a number of astrophysical and instrumental processes, which can either be deterministic or stochastic. It is necessary to develop robust statistical and physical models for these noise processes because incorrect models diminish sensitivity and may cause a spurious gravitational wave detection. Here we characterize noise processes for the 26 pulsars in the second data release of the Parkes Pulsar Timing Array using Bayesian inference. In addition to well-studied noise sources found previously in pulsar timing array data sets such as achromatic timing noise and dispersion measure variations, we identify new noise sources including time-correlated chromatic noise that we attribute to variations in pulse scattering. We also identify 'exponential dip' events in four pulsars, which we attribute to magnetospheric effects as evidenced by pulse profile shape changes observed for three of the pulsars. This includes an event in PSR J1713+0747, which had previously been attributed to interstellar propagation. We present noise models to be used in searches for gravitational waves. We outline a robust methodology to evaluate the performance of noise models and identify unknown signals in the data. The detection of variations in pulse profiles highlights the need to develop efficient profile domain timing methods.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据