20240816
1. PhD, Searching for pulsars in the Galactic centre and the timing of a massive pulsar
2. The High Time Resolution Universe Pulsar survey - XVIII. The reprocessing of the HTRU-S Low Lat survey around the Galactic Centre using a Fast Folding Algorithm pipeline for accelerated pulsars
https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.3208W/abstract
The HTRU-S Low Latitude survey data within 1° of the Galactic Centre (GC) were searched for pulsars using the Fast Folding Algorithm (FFA). Unlike traditional Fast Fourier Transform (FFT) pipelines, the FFA optimally folds the data for all possible periods over a given range, which is particularly advantageous for pulsars with low-duty cycles. For the first time, a search over acceleration was included in the FFA to improve its sensitivity to binary pulsars.
3. Multi-epoch searches for relativistic binary pulsars and fast transients in the Galactic Centre
https://ui.adsabs.harvard.edu/abs/2021MNRAS.507.5053E/abstract
Here, we present multi-epoch pulsar searches of the Galactic Centre at four observing frequencies, 4.85,8.35,14.6,18.95GHz, using the Effelsberg 100-m radio telescope. Our data analysis features acceleration searches on progressively shorter time series to maintain sensitivity to relativistic binary pulsars. The multi-epoch observations increase the likelihood of discovering transient or nulling pulsars, or ensure orbital phases are observed at which acceleration search methods work optimally. In ∼147h of separate observations, no previously undiscovered pulsars have been detected.
4. The role of FAST in pulsar timing arrays
https://ui.adsabs.harvard.edu/abs/2019RAA....19...20H/abstract
The primary goals for PTAs are to detect (and subsequently study) ultra-low-frequency gravitational waves, to develop a pulsar-based time standard and to improve solar system planetary ephemerides. We describe how FAST will contribute to PTA research and show that jitter- and timing-noise will be the limiting noise processes for FAST data sets. Jitter noise will limit the timing precision achievable over data spans of a few years while timing noise will limit the precision achievable over many years.