In practice, we expect the event rate of detectable events to be small, η 1 /N p T , so our analysis includes consideration of the likelihood function for the burst rate that makes

Gravitational wave data analysis, gravitational wave searches with pulsar timing arrays, gravitational wave searches with the Laser Interferometer Gravitational-wave Observatory

Sidery, The effect of small pulsar distance variations in stochastic gravitational wave background searches with Pulsar Timing Arrays”.. I calculated the magnitude of the

The expected number of detectable sources ver- sus data span for idealised data sets containing: (solid line) 20 pulsars with 1µs rms timing residuals sampled every 20 days,

All of the work described so far in this dissertation has kept electromagnetic and gravita- tional wave observations separate using one to inform the other, like taking observations

While average pulse shapes do vary with frequency (Kramer et al. 1998), the pulse shapes of radio pulsars, including those objects having two or more stable shapes associated

We derive significant constraints on the available discovery space based solely on energetic and statistical considerations: we show that a PTA de- tection of GWs at frequencies above

• Understanding regulatory guidances and their level of enforcement is critical for not being under or over compliant. • Incorporate available predictive tools

Searches for stochastic gravitational-wave backgrounds using pulsar timing arrays effectively compare the measured correlations with the expected values from the Hellings and

We also simulated the effects on mock pulsar timing datasets of populations of binaries with random orientation parameters in the TEMPO2 software package (10), and checked that

Although previous pulsar timing array limits on the strength of the GWB (12, 13) were derived assuming Gaussian statistics, a non- Gaussian background, dominated by fewer bi-

Th e eff ects of systemic hypothermia (30°C to 36°C) following fl uid percussion brain injury in rats were fi rst investigated by Clifton and colleagues [8], who showed

Predictions for GW signals from binary SMBHs are based either on physical models for galaxy formation and evolution which predict the binary SMBH population, or on directly

(Top) 95% upper limits from an unparameterised power spectrum analysis for a correlated GWB (red points), and uncorrelated common red noise process (blue points) for the 6

(Top) 95% upper limits from an unparameterised power spectrum analysis for a correlated GWB (red points), and uncorrelated common red noise process (blue points) for the 6

Supermassieve zwarte gaten zijn van belang voor PTAs, omdat aangenomen wordt dat deze objecten verantwoordelijk zijn voor gravitatiegolven die waarneem- baar zijn met

Predictions for GW signals from binary SMBHs are based ei- ther on physical models for galaxy formation and evolution which predict the binary SMBH population or on directly

ground paired with nearby pulsars such as J0437 −4715 which is only L ∼ 160 pc from the Earth [39] (or equiva- lently the SSB), yield a lower bound of 10 on the number of