The strongest Pulsar in the northern hemisphere already detected in the past with self made software.
From the output of presto the trace of the pulsar signal is present in the entire frequency window while in the time window there is a deep scintillation (signal variation).
The presence of several RFI does not preclude to identify a well defined pulsar profile but deteriorates the pulsar definition.
A new observation, in a better noise condition, gives a much more gratifying result, the demonstration is in the chi-squared (X^2) parameter difference (33 1st observation, 240 the second),
Such a difference would be detrimental observing a weaker signal.
Below the 2 results:
Date of Observation |
Thursday, May 25, 2017 / Monday, August 14, 2017 |
Length of Observation |
2 Hours / 3 Hours |
Center Frequency |
1290 MHz |
Bandwidth |
10 MHz |
Pulsar Flux at 1400MHz |
203 mJy |
Distance |
3.460 light years |
Pulsar Period |
714 msec |
Age |
5.000.000 Years |
And now a third result obtained after years with the new B200 software , 56Mhz of bandwidth and 2 hours recording
Despite the increased RFI condition the output has a much cleaner and better definition
At run time a light mitigation was applied on time domain and a deeper one on frequency domain
As post processing only the deletion of few channels still including visible residual RFI
Date of Observation |
Thursday, February 10th, 2022 |
Length of Observation |
2 Hours |
Center Frequency |
1300 MHz |
Bandwidth |
56 MHz |