Constraining GW signatures in pulsar timing: A multi-frequency timing analysis

Pulsars are extremely accurate clocks that allow us to explore certain unanswered questions in the fields of nuclear and gravitational wave astrophysics. Pulsars that form part of a timing array can be used to detect stochastic gravitational wave (GW) backgrounds produced by merging supermassive black holes. However, these backgrounds produce a small amplitude variation in the timing residuals of a pulsar over decades. A number of elements influence the accuracy of the observed times of arrival (TOA); of which "timing noise" contributes to the noise budget due to elements of the pulsar model that we do not understand, as well as the dispersive nature of the ISM through which the pulse propagates. We analyze two decades of data of the pulsar PSR J1326-5859 to observe possible magnetospheric switches that influence the pulsar spin-down which could lead to a deeper understanding of the timing noise phenomena. Here we present the necessary analysis pipeline to investigate the long term stability of the pulsar timing noise, which may lead us to a better understanding of all the contributing factors influencing timing noise. This may then allow possible identification of GW signatures in the pulsar timing noise data.