1. Team Lyne Delaney Jeanine Pigott Elizabeth Leigh Schmitz Mariah Francine Gnegy Zachary Filmore Ramey Dana Marie Dawley Thomas Eugene Hillenbrand Team Mentor: Caitlin Joannah Ahrens

2. Objective Search through fifteen data sets to detect possible pulsars Identify RFI sources Identify noise Follow up possible pulsars with observations from GBT

3. Procedure Search through plots and differentiate between RFI, noise, and possible pulsars Observe FFT (double pulse) plots and single pulse plots, Analyze patterns from the time domain, frequency domain, and the dispersion measure plots Compare follow up data from GBT with previous data

4. Noise Plot Reduced chi- squared is less than 1 P(noise) < 1 No distinguishable signal from pulse profile DM plot is not bell shaped

5. RFI Plot Snake bite on frequency domain plot DM Plot peaks at zero No vertical bins on time domain plot

6. Single Pulse RFI Plot All plots peak at a DM signal of zero Possibly not at the right frequency to pick up other signals

7. Pulsar Candidates Clear peaks in pulse profile Clear vertical bins on time domain plot and frequency domain plots P(noise) is near zero

8. Pulsar Candidates (cont) Relatively small error bar Clear and sharp peaks in pulse profile Visible lines in time domain and sub-band plots Bell-curved DM plot

9. Pulsar Candidates (cont) Small error bar Two clear distinguishable peaks on pulse profile Visible vertical bins on time domain plot DM plot has a clear distinct bell shape Reduced chi- squared is 5.2 P(noise) ~ zero

10. Follow Up Known pulsar in drift scan survey Interrupted by RFI DM plot has a peak at zero Snake bites are apparent in frequency domain plot and it is white Reduced chi- squared is 93 P(noise) ~ zero

11. Discussion Lack of sufficient follow up data from GBT Unable to draw conclusions Remaining Questions: Has there been any changes to J1736-0241 since the last follow up?