1. An In-depth Analysis of Radio Astronomy
A Quest for Pulsars
An In-depth Analysis of Radio Astronomy
Team Disney
Alan Booth, Susan Chen, Blake Delle Fave, Madison Doehler, Yekaterina Gilbo
40 Ft. Telescope Results
Analysis Cont.
Example of RFI (from PSC Database)
Looks like a pulsar candidate except for the frequency graph.
Shows narrowband ‘snake bites’ indicating a man made object from one source.
Mission Statement
500 Jy
~33 Jy
To gain proficiency in the analysis of radio datasets, in order to identify pulsar candidates for the study of gravitational waves.
Introduction
Radio astronomy is the study of electromagnetic emissions from celestial bodies. To collect data, researchers aim radio telescopes at various locations in space , known as pointings, to search for signals. However, man-made objects, such as telephone lines, also produce electromagnetic waves which interfere with the frequency of the waves. As such, researchers must sort through pointings and eliminate radio frequency interference and noise from the results to find pulsars, a type of rapidly rotating neutron star.
Forty-foot Telescope
Object: Galaxy 3c 295
Distance: 5.6 billion light
years or 1.73 billion pc
RA: 14:09:33
DEC: 52:26:13
*Actual Jansky (brightness) is 23 JY
*The galaxy appeared earlier than
expected; we were not able to view the
entire galaxy.
Completed Prerequisites
Understand the concept of radio astronomy using a 40ft telescope
Analyze the signal of Galaxy 3C 295
Brief Intro to Gravitational Waves and Electromagnetic Waves
Intro to Stellar Evolution
Distinguish pulsars from noise and RFI (interference)
Review 15 pointings (525 datasets)
GBT Results
Candidates chosen for GBT: 19:21-16:11, 22:43+69:39, 21:07-16:12
Conclusion
Despite our best efforts, problems still occurred. As such, the researchers were forced to be prepared for any situations It was extremely important, while examining data, to be open minded and through in approach.
We believe that for future trials and research, longer and earlier start times should be used to attain a better dataset. Also, datasets should not be dismissed immediately as noise, as there may be underlying trends. The students of the Pulsar Search Collaboratory will continue their analysis of pointings and datasets, well through the next year.
Identifying Pulsar Candidates
Examine the characteristics of pulse datasets:
Our sun
Candidates 19:21-16:11 and 21:07-16:12 were both observed to be noise. 22:43+69:39 could not be viewed due to circumstances.
Known Pulsar J01:08 -14:31
Frequencies: Must be a Broadband Range for Pulsars
Phase vs. Time: Corresponds with pulse profile.
Chi squared:
Term used to determine probability of being a pulsar
Pulse profile: periodic and distinguishable from noise
Analysis
Examples of Noise (from PSC Database)
Pulse profile: No specific and clean pulses.
Chi squared: Relatively low. X2 <2
Frequency: Narrowband because there is one horizontal band of strong signal.
Dispersion Measure: DM is larger than 0 which is fine
Phase vs. Time: Jagged, erratic slope
Acknowledgements
Sue Ann Heatherly
Sean Leake and all student mentors
Sarah Scoles
TO ALL TEACHERS!
Duncan and Maura
Ryan Lynch
The GBT for being the coolest telescope EVER
NRAO for making this possible and tolerating us in our wildest moments 
Dispersion Measure: Number of electrons between earth and the object; DM peak >0