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Figure 12: Left panel: Pulse scattering caused by irregularities in the interstellar medium. The
different path lengths and travel times of the scattered rays result in a “scattering tail” in the observed
pulse profile which lowers its signal-to-noise ratio. Right panel: A simulation showing the percentage
of Galactic pulsars that are likely to be undetectable due to scattering as a function of observing
frequency. Low-frequency ( |