Abstract Details
| Name: Chaitanya Afle Affiliation: Indian Institute of Science Education and Research Pune Conference ID: ASI2017_453 Title : Detection and characterization of spin-orbit resonances in the advanced gravitational wave detectors era Authors and Co-Authors : Anuradha Gupta (IUCAA), Bhooshan Gadre (IUCAA), Prayush Kumar (CITA, Toronto), Han Gil (Seoul National University, Korea), Sanjit Mitra (IUCAA) Abstract Type : Poster Abstract Category : General Relativity and Cosmology Abstract : The spin-orbit resonances have important astrophysical implications as the evolution and subsequent coalescence of supermassive black hole binaries in this configuration leads to low recoil velocity of merger remnants. Also, it has been shown that the black hole spins in comparable mass stellar mass black hole binaries would preferentially lie in a resonant plane when their gravitational waves (GWs) enter the advanced LIGO frequency band. Therefore, it is highly desirable to investigate the possibility of detection and subsequent characterization of such GW sources in advanced detector era which can, in turn, improve our perception of their high mass counterparts. The current detection pipelines involve only non-precessing template banks (namely, IMRPhenomD and SEOBNRv2) for compact binary searches whereas parameter estimation pipelines can afford to use computationally cheaper though approximate precessing templates (e.g., IMRPhenomPv2). In this paper, we test the performance of these templates in detection and characterization of spin-orbit resonant binaries. We use fully precessing time-domain SEOBNRv3 waveforms as well as four numerical relativity (NR) waveforms to model GWs from spin-orbit resonant binaries. We find that all these approximants are performing well in recovering resonant signals (recovering ∼ 95% injections with fitting factor (FF) higher that 0.97) with IMRPhenomPv2 performing marginally better than IMRPhenomD and SEOBNRv2. Interestingly, injections with ∆φ = 180◦ have higher FF as compared to their ∆φ = 0◦ and generic counterparts (∆φ is the angle between the components of the black hole spins in the plane orthogonal to the orbital angular momentum). This is because most of the low FFs are for binaries with high precession and negative aligned spins. Moreover, all template approximants are able to recover the NR waveforms mainly with FFs > 0.98. For all the injections including NR, the error in estimating chirp mass is < 10% with minimum error for ∆Φ = 180◦ resonant binaries. The symmetric mass ratio can be estimated with errors up to 10%. The aligned spin parameters have absolute error in the range [-0.1, 0.1] while the in-plane spins can be estimated with absolute error as large as -0.6. |