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#### Testing the Kerr nature of intermediate-mass and supermassive black hole binaries using spin-induced multipole moment measurements

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1904.12712.pdf

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Krishnendu_2020_Class._Quantum_Grav._37_205019.pdf

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##### Citation

Krishnendu, N. V., & Yelikar, A. B. (2020). Testing the Kerr nature of intermediate-mass
and supermassive black hole binaries using spin-induced multipole moment measurements.* Classical and
Quantum Gravity,* *37*(20): 205019. doi:10.1088/1361-6382/ababb1.

Cite as: https://hdl.handle.net/21.11116/0000-0007-4663-B

##### Abstract

The gravitational wave measurements of spin-induced multipole moment

coefficients of a binary black hole system can be used to distinguish black

holes from other compact objects [N. V. Krishnendu et al., PRL 119, 091101

(2017)]. Here, we apply the idea proposed in [N. V. Krishnendu et al., PRL 119,

091101 (2017)] to binary systems composed of intermediate-mass and supermassive

black holes and derive the expected bounds on their Kerr nature using future

space-based gravitational wave detectors. Using astrophysical models of binary

black hole population, we study the measurability of the spin-induced

quadrupole and octupole moment coefficients using LISA and DECIGO. The errors

on spin-induced quadrupole moment parameter of the binary system are found to

be { $\leq 0.1$ for almost $3\%$ of the total supermassive binary black hole

population which is detectable by LISA whereas it is $\sim 46\%$ for the

intermediate-mass black hole binaries observable by DECIGO at its design

sensitivity.} We find that { errors on} {\it both} the quadrupole and octupole

moment parameters can be estimated to { be} $\leq 1$ for $\sim 2\%$ and $\sim

50\%$ {of the population} respectively for LISA and DECIGO detectors. { Our

findings suggest that a subpopulation of binary black hole events, with the

signal to noise ratio thresholds greater than 200 and 100 respectively for LISA

and DECIGO detectors, would permit tests of black hole nature to 10\%

precision.}

coefficients of a binary black hole system can be used to distinguish black

holes from other compact objects [N. V. Krishnendu et al., PRL 119, 091101

(2017)]. Here, we apply the idea proposed in [N. V. Krishnendu et al., PRL 119,

091101 (2017)] to binary systems composed of intermediate-mass and supermassive

black holes and derive the expected bounds on their Kerr nature using future

space-based gravitational wave detectors. Using astrophysical models of binary

black hole population, we study the measurability of the spin-induced

quadrupole and octupole moment coefficients using LISA and DECIGO. The errors

on spin-induced quadrupole moment parameter of the binary system are found to

be { $\leq 0.1$ for almost $3\%$ of the total supermassive binary black hole

population which is detectable by LISA whereas it is $\sim 46\%$ for the

intermediate-mass black hole binaries observable by DECIGO at its design

sensitivity.} We find that { errors on} {\it both} the quadrupole and octupole

moment parameters can be estimated to { be} $\leq 1$ for $\sim 2\%$ and $\sim

50\%$ {of the population} respectively for LISA and DECIGO detectors. { Our

findings suggest that a subpopulation of binary black hole events, with the

signal to noise ratio thresholds greater than 200 and 100 respectively for LISA

and DECIGO detectors, would permit tests of black hole nature to 10\%

precision.}