Targeted search for the stochastic gravitational-wave background from the galactic millisecond pulsar population

被引：13

作者：

Agarwal, Deepali ^{[1
]}

Suresh, Jishnu ^{[2
]}

Mandic, Vuk ^{[3
]}

Matas, Andrew ^{[4
]}

Regimbau, Tania ^{[5
]}

机构：

[1] Inter Univ Ctr Astron & Astrophys IUCAA, Pune 411007, India

[2] Catholic Univ Louvain, Ctr Cosmol, Particle Phys & Phenomenol (CP3), B-1348 Louvain La Neuve, Belgium

[3] Univ Minnesota, Minneapolis, MN 55455 USA

[4] Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-14476 Potsdam, Germany

[5] Lab Annecy Le Vieux Phys Particules, CNRS, 9 Chemin Bellevue, F-74941 Annecy, France

来源：

PHYSICAL REVIEW D | 2022年 / 106卷 / 04期

基金：

新加坡国家研究基金会; 美国国家科学基金会; 澳大利亚研究理事会; 英国科学技术设施理事会; 日本学术振兴会;

关键词：

RADIO;

D O I：

10.1103/PhysRevD.106.043019

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The millisecond pulsars, old-recycled objects spinning with high frequency O (kHz) sustaining the deformation from their spherical shape, may emit gravitational waves (GW). These are one of the potential candidates contributing to the anisotropic stochastic gravitational-wave background (SGWB) observable in the ground-based GW detectors. Here, we present the results from a likelihood-based targeted search for the SGWB due to millisecond pulsars in the Milky Way, by analyzing the data from the first three observing runs of Advanced LIGO and Advanced Virgo detector. We assume that the shape of SGWB power spectra and the sky distribution is known a priori from the population synthesis model. The information of the ensemble source properties, i.e., the in-band number of pulsars, N-obs and the averaged ellipticity, mu epsilon is encoded in the maximum likelihood statistic. We do not find significant evidence for the SGWB signal from the considered source population. The best Bayesian upper limit with 95% confidence for the parameters are N-obs <= 8.8 x 10(4) and mu(epsilon) <= 1.4 x 10(-6), which is comparable to the bounds on mean ellipticity with the GW observations of the individual pulsars. Finally, we show that for the plausible case of N-obs 1/4 40000, with the one year of observations, the one-sigma sensitivity on mu epsilon might reach 1.5 x 10(-7) and 4.1 x 10(-8) for the second-generation detector network having A thorn sensitivity and third-generation detector network, respectively.

引用

页数：13

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