Bayesian parameter estimation of stellar-mass black-hole binaries with LISA. (arXiv:2106.05259v1 [astro-ph.HE])

<a href="http://arxiv.org/find/astro-ph/1/au:+Buscicchio_R/0/1/0/all/0/1">Riccardo Buscicchio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klein_A/0/1/0/all/0/1">Antoine Klein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roebber_E/0/1/0/all/0/1">Elinore Roebber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moore_C/0/1/0/all/0/1">Christopher J. Moore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gerosa_D/0/1/0/all/0/1">Davide Gerosa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Finch_E/0/1/0/all/0/1">Eliot Finch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vecchio_A/0/1/0/all/0/1">Alberto Vecchio</a>

We present a Bayesian parameter-estimation pipeline to measure the properties

of inspiralling stellar-mass black hole binaries with LISA. Our strategy (i) is

based on the coherent analysis of the three noise-orthogonal LISA data streams,

(ii) employs accurate and computationally efficient post-Newtonian waveforms

accounting for both spin-precession and orbital eccentricity, and (iii) relies

on a nested sampling algorithm for the computation of model evidences and

posterior probability density functions of the full 17 parameters describing a

binary. We demonstrate the performance of this approach by analyzing the LISA

Data Challenge (LDC-1) dataset, consisting of 66 quasi-circular, spin-aligned

binaries with signal-to-noise ratios ranging from 3 to 14 and times to merger

ranging from 3000 to 2 years. We recover 22 binaries with signal-to-noise ratio

higher than 8. Their chirp masses are typically measured to better than $0.02

M_odot$ at $90%$ confidence, while the sky-location accuracy ranges from 1 to

100 square degrees. The mass ratio and the spin parameters can only be

constrained for sources that merge during the mission lifetime. In addition, we

report on the successful recovery of an eccentric, spin-precessing source at

signal-to-noise ratio 15 for which we can measure an eccentricity of $3times

10^{-3}$.

We present a Bayesian parameter-estimation pipeline to measure the properties

of inspiralling stellar-mass black hole binaries with LISA. Our strategy (i) is

based on the coherent analysis of the three noise-orthogonal LISA data streams,

(ii) employs accurate and computationally efficient post-Newtonian waveforms

accounting for both spin-precession and orbital eccentricity, and (iii) relies

on a nested sampling algorithm for the computation of model evidences and

posterior probability density functions of the full 17 parameters describing a

binary. We demonstrate the performance of this approach by analyzing the LISA

Data Challenge (LDC-1) dataset, consisting of 66 quasi-circular, spin-aligned

binaries with signal-to-noise ratios ranging from 3 to 14 and times to merger

ranging from 3000 to 2 years. We recover 22 binaries with signal-to-noise ratio

higher than 8. Their chirp masses are typically measured to better than $0.02

M_odot$ at $90%$ confidence, while the sky-location accuracy ranges from 1 to

100 square degrees. The mass ratio and the spin parameters can only be

constrained for sources that merge during the mission lifetime. In addition, we

report on the successful recovery of an eccentric, spin-precessing source at

signal-to-noise ratio 15 for which we can measure an eccentricity of $3times

10^{-3}$.

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