Parkes observations for project P456 semester 2019OCTS_04

  • George Hobbs (Contributor)
  • Dick Manchester (Contributor)
  • John Sarkissian (Contributor)
  • Matthew Bailes (Creator)
  • Ramesh Bhat (Contributor)
  • Michael J. Keith (Contributor)
  • William Coles (Contributor)
  • Willem Van Straten (Contributor)
  • Chris Russell (Contributor)
  • Stefan Oslowski (Contributor)
  • Matthew Kerr (Contributor)
  • James M. Dempsey (Contributor)
  • Ryan Shannon (Contributor)
  • Jingbo Wang (Creator)
  • Jane F. Kaczmarek (Contributor)
  • Yuri Levin (Contributor)
  • Linqing Wen (Creator)
  • Xingjiang Zhu (Creator)
  • Shi Dai (Contributor)
  • Daniel John Reardon (Contributor)
  • RenĂ©e Spiewak (Contributor)
  • Lei Zhang (Creator)
  • Songbo Zhang (Contributor)
  • Aditya Parthasarathy (Contributor)



The Parkes Pulsar Timing Array (PPTA) project has three primary goals: (a) detection of gravitational waves from astronomical sources, (b) establishment of a pulsar timescale, and (c) improvement of our understanding of Solar-system dynamics. The PPTA is the oldest of three international pulsar timing groups. We have the smallest telescope and the smallest group, but the best measurements and the best results. Our bound on the strength of the incoherent gravitational wave background is the only bound which significantly constrains theoretical models. We have maintained our leading position because: we have the southern sky; we have a small but well-focussed group; we have the best-calibrated receivers; and we have been able to observe with an almost regular cadence of 15 to 20 days over a wide bandwidth. With this proposal we aim to maintain our pre-eminent position in the field. Unlike most observing proposals, this is a continuing proposal for which the observations will continue to improve bounds on ultra-low-frequency gravitational waves until they are finally detected. Continued Parkes observations will remain valuable at least until the first stage of the SKA is able to improve on our sensitivity and observing cadence. Even after the gravitational wave background is detected we will want to continue observations in support of the nascent field of gravitational wave astronomy!
Date made available13 Nov 2019
PublisherCSIRO Publishing

Cite this