All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=6cm,clip]{8683fig1.ps} \end{figure}$ Figure 1: Schematics showing the geometrical variables associated with a pulsar P (see main text for the exact definitions).
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In the text

$\begin{figure*} \par\includegraphics[angle=-90,width=12.3cm,clip]{8683fig2a.ps}\... ...m} \par\includegraphics[angle=-90,width=12.3cm,clip]{8683fig2b.ps} \end{figure*}$ Figure 2: Grids used in our study overlaid on the face-on distribution of our 482 low-latitude ( $\vert b\vert<10\hbox {$^\circ $ }$ ) pulsars. Pulsars with a positive (negative) RM are denoted with crosses (circles). (x, y) are Galactocentric cartesian coordinates. The Sun is located at ( $x=8.5 ~ {\rm kpc}, y=0$ ). In the upper panel, the circles underlying the grids are at $r = 4~{\rm kpc},\ 5~ {\rm kpc},\ 6\ {\rm kpc},\ 7~ {\rm kpc} {\rm \ and}\ 8~ {\rm kpc}$ , while in the lower panel, they are at $r = 3.5~ {\rm kpc},\ 4.5~ {\rm kpc},\ 5.5~ {\rm kpc},\ 6.5~ {\rm kpc}, \ 7.5~ {\rm kpc} {\rm \ and}\ 8.5~ {\rm kpc}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{8683fig3a.ps}\bigskip\\ \includegraphics[angle=-90,width=9cm,clip]{8683fig3b.ps} \end{figure}$ Figure 3: Plots of RM versus distance ( left panels) and versus DM ( right panels) for the pulsars lying in two different boxes. The first box ( top row) is delimited by the circles r=r_5.5 and r=r_6.5 in the radial direction and by the tangential lines l=l_5.5 and l=l_6.5 in the longitudinal direction. The second box ( bottom row) is delimited by the circles r=r_6.5 and r=r_7.5 and by the tangential lines l=l_4.5 and l=l_6.5. For each box, the best-fit straight line through the points (DM, RM) is drawn in the right panel, and the corresponding value of $\left < \overline {B_{\vert\vert}} \right >$ with its statistical uncertainty are written in the upper right corner. The red points represent outliers.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12cm]{8683fig4.ps} \end{figure}$ Figure 4: Face-on map showing the average line-of-sight component of the magnetic field, $\left < \overline {B_{\vert\vert}} \right >$ , obtained in the different boxes of our two grids. Each $\left < \overline {B_{\vert\vert}} \right >$ is plotted in the form of a vector centered on the box midpoint (point at middle radius, r=r_i, and middle longitude, $l = (l_{\rm min} + l_{\rm max}) /2$ ), and oriented along the local line of sight.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{8683fig5.ps} \end{figure}$ Figure 5: Observational values of the average azimuthal fields, $\left <\overline {B_\theta }\right >_{ij}$ , versus Galactic azimuthal angles, $\theta _{ij}$ , in all the boxes jof the 9 successive rings i, for the ring model. The uncertainties $(\sigma _\theta )_{ij}$ in the field values are plotted as standard error bars. For each ring i, the best-fit value of the model parameter $\left <B_\theta \right >_i$ is indicated by the horizontal dot-dashed line.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{8683fig6.ps} \end{figure}$ Figure 6: Best-fit values of the model parameters, $\left <B_\theta \right >_i$ , versus ring middle radii, r_i, for the ring model. The acceptable values (those consistent with the pulsar data) are shown with their consistency ranges, while the unacceptable values are indicated with crosses. The results obtained with the rule-of-thumb consistency condition, $\chi ^2 \le n_i-1$ , are plotted in the upper panel. Those obtained with the more rigorous consistency condition, $\chi ^2 \le \chi ^2_{\rm crit} (0.1)$ , are plotted in the lower panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip]{8683fig7.ps} \end{figure}$ Figure 7: Consistency domains in the parameter planes $(\left <B_r\right >_i,\left <B_{\theta }\right >_i)$ of the 9 different rings, for the axisymmetric model. The grey contour lines define the consistency domains obtained with the rule-of-thumb consistency condition, $\chi ^2 \le n_i-2$ . The black contour lines define those obtained with the more rigorous consistency condition, $\chi ^2 \le \chi ^2_{\rm crit} (0.1)$ . The crosses mark the locations of the unacceptable best fits (those inconsistent with the pulsar data according to both criteria).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip]{8683fig8.ps} \end{figure}$ Figure 8: Projections of the 3D consistency domains of the 9 different rings on their parameter planes $(b_{r,i},b_{\theta ,i})$ , for the bisymmetric model. The grey contour lines correspond to the consistency domains obtained with the rule-of-thumb consistency condition, $\chi ^2 \le n_i-3$ . The black contour lines correspond to those obtained with the more rigorous consistency condition, $\chi ^2 \le \chi ^2_{\rm crit} (0.1)$ . The crosses mark the locations of the unacceptable best fits (those inconsistent with the pulsar data according to both criteria).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6cm,clip]{8683fig1.ps} \end{figure}$	Figure 1: Schematics showing the geometrical variables associated with a pulsar P (see main text for the exact definitions).
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