Search Swinburne Research Bank
Home List of Titles High signal-to-noise ratio observations and the ultimate limits of precision pulsar timing
Please use this identifier to cite or link to this item: http://hdl.handle.net/1959.3/206324
|Download PDF (Accepted manuscript) (Adobe Acrobat PDF, -1 bytes)|
- High signal-to-noise ratio observations and the ultimate limits of precision pulsar timing
- Oslowski, S.; van Straten, W.; Hobbs, G. B.; Bailes, M.; Demorest, P.
- We demonstrate that the sensitivity of high-precision pulsar timing experiments will be ultimately limited by the broad-band intensity modulation that is intrinsic to the pulsar's stochastic radio signal. That is, as the peak flux of the pulsar approaches that of the system equivalent flux density, neither greater antenna gain nor increased instrumental bandwidth will improve timing precision. These conclusions proceed from an analysis of the covariance matrix used to characterize residual pulse profile fluctuations following the template-matching procedure for arrival time estimation. We perform such an analysis on 25h of high-precision timing observations of the closest and brightest millisecond pulsar, PSR J0437-4715. In these data, the standard deviation of the post-fit arrival time residuals is approximately four times greater than that predicted by considering the system equivalent flux density, mean pulsar flux and the effective width of the pulsed emission. We develop a technique based on principal component analysis to mitigate the effects of shape variations on arrival time estimation and demonstrate its validity using a number of illustrative simulations. When applied to our observations, the method reduces arrival time residual noise by approximately 20 per cent. We conclude that, owing primarily to the intrinsic variability of the radio emission from PSR J0437-4715 at 20cm, timing precision in this observing band better than 30-40ns in 1h is highly unlikely, regardless of future improvements in antenna gain or instrumental bandwidth. We describe the intrinsic variability of the pulsar signal as stochastic wide-band impulse modulated self-noise (SWIMS) and argue that SWIMS will likely limit the timing precision of every millisecond pulsar currently observed by pulsar timing array projects as larger and more sensitive antennas are built in the coming decades.
- Publication type
- Journal article
- Research centre
- Swinburne University of Technology. Faculty of Information and Communication Technologies. Centre for Astrophysics and Supercomputing
- Monthly Notices of the Royal Astronomical Society, Vol. 418, no. 2 (Dec 2011), pp. 1258–1271
- Publication year
- FOR Code(s)
- 0201 Astronomical and Space Sciences
- PSR J0437-4715; Pulsars
- Publisher URL
- Copyright © 2011 The Authors. Journal compilation copyright © 2011 Royal Astronomical Society. The accepted manuscript is reproduced in accordance with the copyright policy of the publisher. The definitive publication is available at www.interscience.wiley.com.
- Research Projects
From nanosecond timing to nanohertz gravitational wave detection, Australian Research Council grant number DP0985272
Gravitational wave detection through millisecond pulsar timing, Australian Research Council grant number DP0878388
- Full text
- Peer reviewed