Searching for gravitational waves emitted by binaries with spinning components

TL;DR

This thesis develops methods for detecting gravitational waves from binary systems with spinning components, including a dedicated search with LIGO data and a new approach for future space-based detectors like LISA.

Contribution

It presents the first dedicated search for spinning binary systems in LIGO data and introduces a computationally efficient method for detecting extreme mass ratio inspirals for LISA.

Findings

No gravitational wave detection in LIGO S3 data for spinning binaries.

Set an upper limit on binary coalescence rates.

Developed a new method for detecting extreme mass ratio inspirals.

Abstract

In this thesis we consider the data analysis problem of detecting gravitational waves emitted by inspiraling binary systems. Detection of gravitational waves will open a new window on the Universe enabling direct detection of systems such as binary black holes for the first time. In the first Chapter we show how gravitational waves are derived from Einstein's General theory of Relativity and discuss the emission of gravitational waves from inspiraling binaries and how this radiation may be detected using laser interferometers. Around two thirds of stars inhabit binary systems. As they orbit each other they will emit both energy and angular momentum in the form of gravitational waves which will inevitably lead to their inspiral and eventual merger. To date, searches for gravitational waves emitted during the inspiral of binary systems have concentrated on systems with non-spinning components. In Chapter 2 we detail the first dedicated search for binaries consisting of spinning stellar mass compact objects. We analysed 788 hours of data collected during the third science run (S3) of the LIGO detectors, no detection of gravitational waves was made and we set an upper limit on the rate of coalescences of stellar mass binaries. The inspiral of stellar mass compact objects into super massive black holes will radiate gravitational waves at frequencies detectable by the planned space-based LISA mission. In Chapter 3 we describe the development and testing of a computationally cheap method to detect the loudest few extreme mass ratio inspiral events that LISA will be sensitive to.