Pulsar Presentation

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Pulsar Presentation
Team Hewish Andy Marx Jason Granstedt Jeremy
Thorley Robbie Culbertson

• Background
• Pulsars are neutron stars that generally exhibit
  these qualities
• Their radius is approximately 10 km in size
• They have mass equal to 1.4 solar mass
• Extremely dense, comparable to that of an atomic
  nucleus
• Extremely rapid spin, can exceed rates of 700Hz
• Extreme magnetic fields 1x1012 than that of the
  earth

Known Pulsar J1311-1228

Below Known Pulsar J0944-1354
Introduction During our dataset evaluation, our
team found 3 previously Known Pulsars J1903-0632
J0944-1354 J1311-1228
In the data below, there are two distinct pulses
at the DMs of 65 and 75. From this, our group
hypothesized that there are two pulsars emitting
from this RA and DEC.
Aim During the evaluation of pulsar J1903-0632s
single pulse plots we came across two pulses at
two very different DMs. This suggests that there
may be another pulsar in close vicinity to the
known one. Using gridding, we hoped to isolate
the two. We also wished to obtain 820 MHz data
for the known pulsar, J1311-1228.
Above Known Pulsar J1903-0632
Results Our results came back inconclusive.
Without the proper gridding coordinates, we did
not see any other radio signals other than the
pulses emitted by J1903-0632. Due to a
miscalculation of the telescope, the declination
was significantly off one of our other targets,
J1311-1228, leading to only noise being detected.
Finally, RFI plagued our last graph, a source
given to us at the GBT, and we were unable to
successfully draw any conclusions from it.

• Method
• Data for all three pulsars was originally
  discovered through the data collected from the
  GBT 350 MHz survey of the sky. After narrowing
  down our 15 datasets into the known pulsars and
  the potential candidate, the GBT telescope was
  used to perform a more thorough sweep of where
  the pulsars were believed to be with the 820 MHz
  receiver.

Conclusion Unfortunately, without the capability
to grid our segment of the sky we were unable to
obtain conclusive information about the
possibility of a pulsar behind J1903-0632. In the
future, we hope that we will be able to grid this
area and find conclusive evidence one way or
another. We also desire to discover the source of
the noise that was interfering with our last
source in the GBT to avoid further RFI.
New data of J1903 and the space around it.
Cannot see evidence of Phantom Pulsar
Acknowledgements NRAO Joe Swiggum Peter
Gentile Sue Ann Heatherly
The GBT.,