### Dataset 1: Uniformly sampled data with a stochastic GW background and white noise

- White Noise: 100 nano-seconds for each pulsar
- GW Background: Characteristic strain spectrum is a power law with index -2/3. The amplitude of the strain spectrum at a frequency of 1 year
^{-1}is 1 x 10^{-14} - Cadence: Once every two weeks
- Total Time Span: Five Years

### Dataset 2: Non-uniformly sampled data with a stochastic GW background and white noise

- White Noise: Different for all pulsars, consistent with measured values of residuals for IPTA pulsars. Click here to get the list of the white noise RMS for each pulsar.
- GW Background: Characteristic strain spectrum is a power law with index -2/3. The amplitude of the strain spectrum at a frequency of 1 year
^{-1}is 6 x 10^{-14} - Cadence: Randomly sampled. Average interval of two weeks, ±5 days. Same time base for all pulsars
- Total Time Span: Five Years

### Dataset 3: Non-uniformly sampled data with a stochastic GW background together with white and red noise

- White Noise: Same as in dataset 2
- Red Noise: Same power spectrum for all pulsars, different realization

Red Noise Power Spectrum is of the form: P(f) = A f^{ -α} where f is in Hz, A = 3.66 x 10^{-18} seconds^{1.8} and α= 1.2.

- GW Background: Characteristic strain spectrum is a power law with index -2/3. The amplitude of the strain spectrum at a frequency of 1 year
^{-1}is 5 x 10^{-15} - Cadence: Randomly sampled. Average interval of two weeks, ±5 days. Same time base for all pulsars
- Total Time Span: Five years