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Fig. 13


A 12 h observation of PSR B0809+74 made with 4 incoherently added HBA stations in the frequency range 140–164 MHz. The left-most plots highlight how the S/N varies throughout the observation, mostly due to scintillation but also from the changing telescope sensitivity with zenith angle. The dashed line marks the time when the pulsar crosses the meridian. The S/N value shown in the left hand plot is calculated for each 7.2 min integration. The middle plot shows an hour of data when the pulsar most frequently nulled and exhibited mode changing. The right-most plot zooms in on two long nulls (grey), that are easily distinguished from the on-pulses (black). Note the quality of the data even in this region when the pulsar was not particularly bright, and at a high zenith angle, where the sensitivity of LOFAR is reduced by a factor of roughly two.

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