Hawkesbury Radio Astronomy Observatory

Vela Pulsar Observations

Observing PSR B0833-45 with a Small Aperture Antenna

Daily Observations

Please Note: Unfortunately since the beginning of July 2018 local RFI at the observation frequency of 436 MHz has increased significantly and severely degraded the accuracy of the spin frequency measurement. It has become necessary to investigate other frequencies within the existing hardware bandpass to avoid this new RFI - currently trialling 427 - 440 MHz.

In addition testing is being done with various antenna configurations as well as software changes.  Due to these factors, the parameters used to determine a valid observation are not optimal.  Consequently, results displayed here may be in error - for example 'glitch alerts' may appear which are actually RFI events.  This situation will continue (and this notice will remain) until a solution to the RFI problem is found.

Below are the last HawkRAO observatory results of reception of Vela pulsar signals showing the Observatory Status, the Period Search Panel, the Glitch Monitor Panel, a Vela Information Panel and an Aggregate Pulse Profile.  For further details about the data displayed here see the 'Observation Information' page (opens a new window).  Also a daily observation summary text file can be viewed here.  In addition details of science results can be seen here. The current position of the Vela pulsar as observed at HawkRAO can be viewed on the 'Vela' page (see tab above).

Current HawkRAO Vela Pulsar Observation Status
HawkRAO Observatory Status
Period Search Panel
HawkRAO Observatory Panel
Glitch Alert Panel
HawkRAO Glitch Monitor Panel
Vela Information Panel
Vela Information Panel
Aggregate Pulse Profile Panel
Aggregate Pulse Profile

See the 'Observation Information' page (opens new window) for further details.

Note: Due to the sensitivity of the Yagi antenna to water on its elements, observation in raining conditions is unfortunately not possible. This is evident in the 'Period Search' graphic as a 'flat-line' result which causes the estimation of the spin frequency to be grossly in error. A 'scan quality' algorithm in software prevents such observations from being included in the results.


Comments and suggestions are always welcome.  Please use the following email address...