The role of FAST in pulsar timing arrays

被引：42

作者：

Hobbs, George ^{[1
]}

Dai, Shi ^{[1
,2
]}

Manchester, Richard N. ^{[1
]}

Kerr, Matthew ^{[1
]}

Lee, Ke-Jia ^{[3
,4
]}

Xu, Ren-Xin ^{[2
,3
]}

机构：

[1] CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia

[2] Peking Univ, Dept Astron, Sch Phys, Beijing 100871, Peoples R China

[3] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China

[4] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany

来源：

RESEARCH IN ASTRONOMY AND ASTROPHYSICS | 2019年 / 19卷 / 02期

基金：

澳大利亚研究理事会; 中国国家自然科学基金;

关键词：

stars: pulsars; gravitational waves; GRAVITATIONAL-WAVE MEMORY; EXTREME SCATTERING EVENT; MILLISECOND PULSAR; PRECISION; BINARY; LIMITS; DISCOVERY; PLANETS; NOISE; DISPERSION;

D O I：

10.1088/1674-4527/19/2/20

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Five-hundred-meter Aperture Spherical radio Telescope (FAST) will become one of the world-leading telescopes for pulsar timing array (PTA) research. The primary goals for PTAs are to detect (and subsequently study) ultra-low-frequency gravitational waves, to develop a pulsar-based tune standard and to improve solar system planetary ephemerides. FAST will have the sensitivity to observe known pulsars with significantly improved signal-to-noise ratios and will discover a large number of currently unknown pulsars. We describe how FAST will contribute to PTA research and show that jitter- and timing-noise will be the limiting noise processes for FAST data sets. Jitter noise will limit the timing precision achievable over data spans of a few years while timing noise will limit the precision achievable over many years.

引用

页数：16

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