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Journal Article

#### Detection and characterization of spin-orbit resonances in the advanced gravitational wave detectors era

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##### Citation

Afle, C., Gupta, A., Gadre, B., Kumar, P., Demos, N., Lovelace, G., et al. (2018).
Detection and characterization of spin-orbit resonances in the advanced gravitational wave detectors era.*
Physical Review D,* *98*(8): 083014. doi:10.1103/PhysRevD.98.083014.

Cite as: https://hdl.handle.net/21.11116/0000-0001-40AE-3

##### Abstract

In this paper, we test the performance of templates in detection and

characterization of Spin-orbit resonant (SOR) binaries. We use precessing

SEOBNRv3 waveforms as well as {\it four} numerical relativity (NR) waveforms to

model GWs from SOR binaries and filter them through IMRPhenomD, SEOBNRv4

(non-precessing) and IMRPhenomPv2 (precessing) approximants. We find that

IMRPhenomD and SEOBNRv4 recover only $\sim70\%$ of injections with fitting

factor (FF) higher than 0.97 (or 90\% of injections with ${\rm FF}

>0.9$).However, using the sky-maxed statistic, IMRPhenomPv2 performs

magnificently better than their non-precessing counterparts with recovering

$99\%$ of the injections with FFs higher than 0.97. Interestingly, injections

with $\Delta \phi = 180^{\circ}$ have higher FFs ($\Delta \phi$ is the angle

between the components of the black hole spins in the plane orthogonal to the

orbital angular momentum) as compared to their $\Delta \phi =0^{\circ}$ and

generic counterparts. This implies that we will have a slight observation bias

towards $\Delta \phi=180^{\circ}$ SORs while using non-precessing templates for

searches. All template approximants are able to recover most of the injected NR

waveforms with FFs $>0.95$. For all the injections including NR, the error in

estimating chirp mass remains below $<10\%$ with minimum error for $\Delta \phi

= 180^{\circ}$ resonant binaries. The symmetric mass ratio can be estimated

with errors below $15\%$. The effective spin parameter $\chi_{\rm eff}$ is

measured with maximum absolute error of 0.13. The in-plane spin parameter

$\chi_p$ is mostly underestimated indicating that a precessing signal will be

recovered as a relatively less precessing signal. Based on our findings, we

conclude that we not only need improvements in waveform models towards

precession and non-quadrupole modes but also better search strategies for

precessing GW signals.

characterization of Spin-orbit resonant (SOR) binaries. We use precessing

SEOBNRv3 waveforms as well as {\it four} numerical relativity (NR) waveforms to

model GWs from SOR binaries and filter them through IMRPhenomD, SEOBNRv4

(non-precessing) and IMRPhenomPv2 (precessing) approximants. We find that

IMRPhenomD and SEOBNRv4 recover only $\sim70\%$ of injections with fitting

factor (FF) higher than 0.97 (or 90\% of injections with ${\rm FF}

>0.9$).However, using the sky-maxed statistic, IMRPhenomPv2 performs

magnificently better than their non-precessing counterparts with recovering

$99\%$ of the injections with FFs higher than 0.97. Interestingly, injections

with $\Delta \phi = 180^{\circ}$ have higher FFs ($\Delta \phi$ is the angle

between the components of the black hole spins in the plane orthogonal to the

orbital angular momentum) as compared to their $\Delta \phi =0^{\circ}$ and

generic counterparts. This implies that we will have a slight observation bias

towards $\Delta \phi=180^{\circ}$ SORs while using non-precessing templates for

searches. All template approximants are able to recover most of the injected NR

waveforms with FFs $>0.95$. For all the injections including NR, the error in

estimating chirp mass remains below $<10\%$ with minimum error for $\Delta \phi

= 180^{\circ}$ resonant binaries. The symmetric mass ratio can be estimated

with errors below $15\%$. The effective spin parameter $\chi_{\rm eff}$ is

measured with maximum absolute error of 0.13. The in-plane spin parameter

$\chi_p$ is mostly underestimated indicating that a precessing signal will be

recovered as a relatively less precessing signal. Based on our findings, we

conclude that we not only need improvements in waveform models towards

precession and non-quadrupole modes but also better search strategies for

precessing GW signals.