Abstract

Gravitational Waves (GWs) are tiny ripples in the fabric of space-time predicted by Einstein’s theory of General Relativity. Pulsar timing arrays (PTAs) offer a unique opportunity to detect low frequency GWs in the near future. In this frequency band, the expected source of GWs are Supermassive Black Hole Binaries (SMBHBs) and they will most likely form in an ensemble creating a stochastic GW background with the possibility of a few nearby/massive sources that will be individually resolvable. A direct detection of GWs will open a new window into the fields of astronomy and astrophysics by allowing us to constrain the coalescence rate of SMBH Bs, providing further tests on the theory of General Relativity, and giving us access to properties of black holes not accessible by current astronomical techniques. Here we will discuss the development of a several robust detection pipelines for both a stochastic background of GWs and single resolvable sources that are fully tailored to the unique aspects of PTA data analysis. We report on the efficacy of these pipelines with simulated datasets and present preliminary results from the newly released International Pulsar Timing Array (IPTA) data sets.