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

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##### Citation

Agarwal, D., Suresh, J., Mandic, V., Matas, A., & Regimbau, T. (2022). Targeted
search for the stochastic gravitational-wave background from the galactic millisecond pulsar population.*
Physical Review D,* *106*(4): 043019.

Cite as: https://hdl.handle.net/21.11116/0000-000A-589A-6

##### Abstract

The millisecond pulsars, old-recycled objects spinning with high frequency

$\mathcal{O}$(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

$N_{obs}\leq8.8\times10^{4}$ and $\mu_\epsilon\leq1.1\times10^{-7}$, 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

$N_{obs}=40,000$, with the one year of observations, the one-sigma sensitivity

on $\mu_\epsilon$ might reach $10^{-8}$ and $2.7\times10^{-9}$ for the

second-generation detector network having A+ sensitivity and third-generation

detector network respectively.

$\mathcal{O}$(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

$N_{obs}\leq8.8\times10^{4}$ and $\mu_\epsilon\leq1.1\times10^{-7}$, 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

$N_{obs}=40,000$, with the one year of observations, the one-sigma sensitivity

on $\mu_\epsilon$ might reach $10^{-8}$ and $2.7\times10^{-9}$ for the

second-generation detector network having A+ sensitivity and third-generation

detector network respectively.