Estimation of far-field wavefront error of tilt-to-length distortion coupling in space-based gravitational wave detection  

作　　者：陶雅正 金洪波 吴岳良 Ya-Zheng Tao;Hong-Bo Jin;Yue-Liang Wu(The School of Physical Sciences,University of Chinese Academy of Sciences,Beijing 100049,China;National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China;The International Centre for Theoretical Physics Asia-Pacific,University of Chinese Academy of Sciences,Beijing 100190,China;CAS Key Laboratory of Theoretical Physics,Institute of Theoretical Physics,Chinese Academy of Sciences,Beijing 100190,China;Hangzhou Institute for Advanced Study,University of Chinese Academy of Sciences,Hangzhou 310024,China)

机构地区：[1]The School of Physical Sciences,University of Chinese Academy of Sciences,Beijing 100049,China [2]National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China [3]The International Centre for Theoretical Physics Asia-Pacific,University of Chinese Academy of Sciences,Beijing 100190,China [4]CAS Key Laboratory of Theoretical Physics,Institute of Theoretical Physics,Chinese Academy of Sciences,Beijing 100190,China [5]Hangzhou Institute for Advanced Study,University of Chinese Academy of Sciences,Hangzhou 310024,China

出　　处：《Chinese Physics B》2023年第2期20-26,共7页中国物理B（英文版）

基　　金：supported in part by the National Key Research and Development Program of China (Grant No. 2020YFC2201501);the National Natural Science Foundation of China (Grant No. 12147103, special fund to the center for quanta-to-cosmos theoretical physics) (Grant No. 11821505);the Strategic Priority Research Program of the Chinese Academy of Sciences (Grant No. XDB23030100);the Chinese Academy of Sciences (CAS)。

摘　　要：In space-based gravitational wave detection, the estimation of far-field wavefront error of the distorted beam is the precondition for the noise reduction. Zernike polynomials are used to describe the wavefront error of the transmitted distorted beam. The propagation of a laser beam between two telescope apertures is calculated numerically. Far-field wavefront error is estimated with the absolute height of the peak-to-valley phase deviation between the distorted Gaussian beam and a reference distortion-free Gaussian beam. The results show that the pointing jitter is strongly related to the wavefront error. Furthermore, when the jitter decreases 10 times from 100 nrad to 10 nrad, the wavefront error reduces for more than an order of magnitude. In the analysis of multi-parameter minimization, the minimum of wavefront error tends to Z[5,3] Zernike in some parameter ranges. Some Zernikes have a strong correlation with the wavefront error of the received beam. When the aperture diameter increases at Z[5,3] Zernike, the wavefront error is not monotonic and has oscillation.Nevertheless, the wavefront error almost remains constant with the arm length increasing from 10-1Mkm to 10~3Mkm.When the arm length decreases for three orders of magnitude from 10-1Mkm to 10-4Mkm, the wavefront error has only an order of magnitude increasing. In the range of 10-4Mkm to 10~3Mkm, the lowest limit of the wavefront error is from 0.5 fm to 0.015 fm at Z[5,3] Zernike and 10 nrad jitter.

关 键 词：laser optical systems space mission gravitational wave 

分 类 号：P111[天文地球—天文学] P142.84