2 General Relativity Measurements from Pulsars
57
Fig. 2.3
Frequency vs. pulse phase plots for PSR J1721−3532: the observing band is split into 96 3 MHz-wide channels in each of which the pulse is clearly
visible (darker parts of the gray-scale). On the left panel
the signal is dispersed and the resulting pulse profile (reported at the bottom
of the panel) is broadened
so much over the entire bandwidth that its impulsive nature is completely washed out. On the right panel,
the various frequency channels are delayed one with
respect to the other, taking into account the effects of the dispersion in the ISM. The integrated pulse profile is thus neatly recovered
57
Fig. 2.3
Frequency vs. pulse phase plots for PSR J1721−3532: the observing band is split into 96 3 MHz-wide channels in each of which the pulse is clearly
visible (darker parts of the gray-scale). On the left panel
the signal is dispersed and the resulting pulse profile (reported at the bottom
of the panel) is broadened
so much over the entire bandwidth that its impulsive nature is completely washed out. On the right panel,
the various frequency channels are delayed one with
respect to the other, taking into account the effects of the dispersion in the ISM. The integrated pulse profile is thus neatly recovered