All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{ms4103f1.eps} \end{figure}$ Figure 1: Stokes V profiles in the region of the H $_\beta$ line in the two roAp stars HD 128898 and HD 83368 and in the strongly magnetic Ap star HD 94660. The spectra of HD 83368 and HD 128898 are shifted in the vertical direction by 0.01 and 0.02 respectively. The thickness of the plotted lines corresponds to the uncertainty of the measurement of polarization determined from photon noise. A strong polarization signal close to the wavelength $\lambda \approx 4876$ Å is probably due to the presence of the blend of strong lines belonging to Nd II and Cr II.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{ms4103f2.eps} \end{figure}$ Figure 2: Pulsational behaviour of the Stokes V profiles in the region of the H $_\beta$ line over four consecutive exposures in the star HD 128898 with the smallest measured longitudinal magnetic field. As in Fig. 1, the thickness of the plotted lines corresponds to the uncertainty of the measurements of polarization determined from photon noise.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{ms4103f3.eps} \end{figure}$ Figure 3: Pulsational behaviour of the Stokes V profiles in the region of the H $_\beta$ line over four consecutive exposures in the star HD 137949 with the largest measured longitudinal magnetic field. As in Fig. 1, the thickness of the plotted lines corresponds to the uncertainty of the measurements of polarization determined from photon noise.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ms4103f4.ps} \end{figure}$ Figure 4: An amplitude spectrum of the magnetic field measurements of HD 83368 over the entire wavelength range studied. This is typical of the amplitude spectra for the stars in the sample. The highest peak is at $\nu = 1.246$ mHz (P = 13.38 min) which is not at the known pulsation frequency of 1.428 mHz (P = 11.67 min), hence is probably a noise peak.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ms4103f5_1.ps}\par\includegraphics[width=7.5cm,clip]{ms4103f5_2.ps} \end{figure}$ Figure 5: Amplitude spectra of the magnetic field measurements of HD 101065. The top panel shows the amplitude spectrum for the first 2.4 h run with the highest peak at the known photometric pulsation frequency, 1.365 mHz, with an amplitude of $39 \pm 12$ G. The lower panel shows the amplitude spectrum of a 4 h run under Director's Discretionary Time that fails to confirm the highest peak in the upper panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{ms4103f2.eps} \end{figure}$	Figure 2: Pulsational behaviour of the Stokes V profiles in the region of the H $_\beta$ line over four consecutive exposures in the star HD 128898 with the smallest measured longitudinal magnetic field. As in Fig. 1, the thickness of the plotted lines corresponds to the uncertainty of the measurements of polarization determined from photon noise.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{ms4103f3.eps} \end{figure}$	Figure 3: Pulsational behaviour of the Stokes V profiles in the region of the H $_\beta$ line over four consecutive exposures in the star HD 137949 with the largest measured longitudinal magnetic field. As in Fig. 1, the thickness of the plotted lines corresponds to the uncertainty of the measurements of polarization determined from photon noise.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ms4103f4.ps} \end{figure}$	Figure 4: An amplitude spectrum of the magnetic field measurements of HD 83368 over the entire wavelength range studied. This is typical of the amplitude spectra for the stars in the sample. The highest peak is at $\nu = 1.246$ mHz (P = 13.38 min) which is not at the known pulsation frequency of 1.428 mHz (P = 11.67 min), hence is probably a noise peak.
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