Figure 13: Left panel: A Arecibo observation of the binary pulsar B1913+16. The
assumption that the pulsar has a constant period during this time is clearly inappropriate given the
quadratic drifting in phase of the pulse during the observation (linear grey scale plot). Right panel:
The same observation after applying an acceleration search. This shows the effective recovery of the
pulse shape and a significant improvement in the signal-to-noise ratio.
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