Abstract Details
| Name: Chandra Kant Mishra Affiliation: International Centre for Theoretical Sciences - Tata Institute of Fundamental Research (ICTS-TIFR)) Conference ID: ASI2016_673 Title : Waveform modelling for binary black hole coalescences Authors and Co-Authors : P. Ajith, Nathan Johnson-McDaniel (ICTS-TIFR, Bangalore, India) K. G. Arun (Chennai Mathematical Institute, Chennai, India) Abstract Type : Poster Abstract Category : General Relativity and Cosmology Abstract : We expect binary black hole (BBH) coalescences to be a prominent source for advanced ground-based gravitational-wave (GW) detectors, such as Advanced LIGO, with possibly tens or more events per year when the detectors are operating at design sensitivities. Both the detection and the subsequent analysis of these signals requires accurate modelling of the source. Even small deviations from the true signal can lead to a significant loss in detection rates and poor measurement of the source properties. The most accurate models for these signals are provided by numerical relativity (NR) simulations. However, these simulations are computationally expensive, and are thus only able to be carried out for a sparse sampling of the parameter space. Moreover, most NR simulations are not able to cover many orbits before merger. One thus uses as much information from approximation/perturbation techniques in general relativity as possible to make fast-to-evaluate models for the waveforms, which one calibrates to NR simulations. Currently, there are a number of such models, though they mostly focus on modelling the dominant quadrupolar mode of the waveform, though the real signal might have significant contributions from higher order modes. Neglecting the contributions from higher order modes might result in significant loss of detection rates or in biases in the recovery of the system's parameters. In this presentation I shall discuss the scheme we have developed to efficiently use available inputs from various approximation techniques/perturbation theory results in general relativity along with recent NR simulations to construct analytical waveform models including the effect of higher modes. These waveform models can be used to efficiently detect/analyse GW signals from BBH coalescences. |