$\begin{figure} \par\subfigure[]{\includegraphics[angle=-90,width=8.8cm,clip]{H43... ...igure[]{\includegraphics[angle=-90,width=8.8cm,clip]{H4303F2.PS} } \end{figure}$ Figure 1: Our results for the MCF as a function of phase delay calculated for pulsars B0950+08 a) and B0329+54 b) before bandpass correction, obtained from 2 320 and 5 200 time series of real data obtained with WSRT, respectively. The time resolution is 50 ns for PSR B0950+08 and 100 ns for PSR B0329+54. Note that the peak at zero phase delay has been set to zero.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4303F3.PS} \end{figure}$ Figure 2: Our results of the MCF calculated for PSR B0329+54 after bandpass correction. See Fig. 1 for explanation.
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In the text

$\begin{figure} \par\subfigure[]{\includegraphics[width=5.4cm,clip]{H4303F4.PS} }... ...} \subfigure[]{\includegraphics[width=5.4cm,clip]{H4303F7.PS} } \par\end{figure}$ Figure 3: Bandpass of one polarisation of WSRT for a) on-pulse of B0950+08, b) on-pulse of B0329+54, c) off-pulse of B0950+08, d) off-pulse of B0329+54, all averaged over 2000 pulses. The peaks are caused by interference. The on-pulse of B0329+54 shows scintillation with a width of approximately 30 kHz (or 25 bins).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4303F8.PS} \end{figure}$ Figure 4: The MCF of simulated scintillation at a frequency of 328 MHz and a bandwidth of 5 MHz. The input parameters are set to generate scintillation similar to that in our data from B0329+54.
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In the text

$\begin{figure} \par\subfigure[]{\includegraphics[angle=-90,width=8.8cm,clip]{H43... ...igure[]{\includegraphics[angle=-90,width=8.8cm,clip]{H4303F2.PS} } \end{figure}$	Figure 1: Our results for the MCF as a function of phase delay calculated for pulsars B0950+08 a) and B0329+54 b) before bandpass correction, obtained from 2 320 and 5 200 time series of real data obtained with WSRT, respectively. The time resolution is 50 ns for PSR B0950+08 and 100 ns for PSR B0329+54. Note that the peak at zero phase delay has been set to zero.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4303F3.PS} \end{figure}$	Figure 2: Our results of the MCF calculated for PSR B0329+54 after bandpass correction. See Fig. 1 for explanation.
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$\begin{figure} \par\subfigure[]{\includegraphics[width=5.4cm,clip]{H4303F4.PS} }... ...} \subfigure[]{\includegraphics[width=5.4cm,clip]{H4303F7.PS} } \par\end{figure}$	Figure 3: Bandpass of one polarisation of WSRT for a) on-pulse of B0950+08, b) on-pulse of B0329+54, c) off-pulse of B0950+08, d) off-pulse of B0329+54, all averaged over 2000 pulses. The peaks are caused by interference. The on-pulse of B0329+54 shows scintillation with a width of approximately 30 kHz (or 25 bins).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4303F8.PS} \end{figure}$	Figure 4: The MCF of simulated scintillation at a frequency of 328 MHz and a bandwidth of 5 MHz. The input parameters are set to generate scintillation similar to that in our data from B0329+54.
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