ISS Plots:

Plot of Pulse broadening time at 1 GHz vs. dispersion measure DM for 196 pulsars.


Filled circles denote measurements of pulse broadening that, where necessary, have been scaled to 1 GHz using a f**(-4.4) scaling. Open circles represent broadening times calculated from scintillation bandwidth measurements. The solid line is a parabolic fit,

log(tau) = -7.231 + 0.9255 log(DM) + 0.814613 log(DM)^2,

while the solid lines represent fluctuations based on residuals from the fit. A similar plot with fewer pulsars appears in Nature, 354, 121, 1991 (Cordes, Weisberg, Frail, Spangler & Ryan).

Probability density for pulsar luminosity with & without ISS


The figure shows the probability density function (pdf) of the pseudo luminosity for a L^{-2} power law: (heavy solid line:) without interstellar scintillations; (light solid line:) with scintillations and no time-bandwidth averageing; (dotted lines:) with ISS and t-b averaging by the specified number of independent fluctuations. [From Cordes & Chernoff, ApJ, in press, 1997 June]

Dynamic Spectra from Pulsar B1919+21 in 1980-1981.


These data obtained at the Arecibo Observatory were reported by Cordes, Weisberg & Boriakoff 1985, ApJ, 288, 221 and Cordes 1986, ApJ, 311, 183.

Dynamic Spectra from Pulsar B0329+54.


These unpublished data were obtained in 1990 at the NRAO/Green Bank 43-m Telescope by Roger Foster and Ralph Fiedler (NRL) and JMC.

Dynamic Spectra from Pulsar B1933+16.


These data were obtained in 1999 with the AOFTM.

Dynamic Spectra from Pulsar B1133+16.


These data were obtained in 1999 with the AOFTM.