All Figures

$\begin{figure} \par\includegraphics[angle=270,width=7.8cm,clip]{8670fig1.ps} \end{figure}$ Figure 1: Polarisation angle, linear and total flux for G339-1.26, as observed by the LBA (this paper, blue open squares) and the ATCA (Ellingsen, priv. comm., red closed circles). The spectra is scalar summed across the image (Stokes I, Q and U), and shows good agreement between the VLBI and the connected array results. The found Stokes I flux from the 2001 observations is slightly higher between (-34.5 to -33.0 $\mbox{km~s}^{-1}$ ), whereas the fractional polarisation is slightly lower. This is the region found to be varible in Goedhart et al. (2004). The errors are the absolute errors based on the confidence in the polarisation calibration (2% and 0.4% respectively), not the relative errors. Where errors are not shown they could not be calculated.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.8cm,clip]{8670fig2.cps}\end{figure}$ Figure 2: Spot plot of G339.88-1.26. The sizes represent the square root of the component flux and the colour the velocity. There are three clusters of points, to the North, the East and the West. The position errors are much less than the symbol sizes. The line shows the best fit to the disk, at $-61^\circ$ .
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.8cm,clip]{8670fig3.cps}\end{figure}$ Figure 3: Velocity-major axis plot, showing the distance along the major axis (the best fit to the disk) against velocity. The spots are extended in velocity perpendicular to the major axis, and the fit as a linear distribution due to emission from a ring around a central gravitational source - which gives 11 $M_\odot$ (shown) - is very poor.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=11cm,clip]{8670fig4.eps}\end{figure}$ Figure 4: Total flux (contours at 2, 8, 32 and 128 Jy/beam) overlaid with the polarisation intensity and direction (scaled vectors). The beam size shown in top left, along with bar representing 10 Jy of linearly polarised flux. The polarisation vectors are rotated to represent the magnetic field. The four regions with significant polarised emission are expanded.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{8670fg5a.cps}\par\vspace*{2mm} \includegraphics[width=7.2cm,clip]{8670fg5b.cps} \end{figure}$ Figure 5: a) Image of the SE feature with magnetic fields lying perpendicular to it. The image shows the total flux image, along with a colour bar, in Jy/beam. The linear polarised flux contours (4, 6, 8, 10 and 12 Jy/beam), and the polarisation vectors, scaled to the fractional polarised flux, rotated to represent the magnetic field direction. The beam size and a bar representing 10% fractional polarised flux is shown in the bottom left. b) The Velocity-Major Axis plot shows that this feature is linear in velocity space, and therefore could be represented by a ring (or partial ring) of emission around a central gravitational source.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.8cm,clip]{8670fig2.cps}\end{figure}$	Figure 2: Spot plot of G339.88-1.26. The sizes represent the square root of the component flux and the colour the velocity. There are three clusters of points, to the North, the East and the West. The position errors are much less than the symbol sizes. The line shows the best fit to the disk, at $-61^\circ$ .
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$\begin{figure} \par\includegraphics[angle=270,width=7.8cm,clip]{8670fig3.cps}\end{figure}$	Figure 3: Velocity-major axis plot, showing the distance along the major axis (the best fit to the disk) against velocity. The spots are extended in velocity perpendicular to the major axis, and the fit as a linear distribution due to emission from a ring around a central gravitational source - which gives 11 $M_\odot$ (shown) - is very poor.
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$\begin{figure} \par\includegraphics[angle=90,width=11cm,clip]{8670fig4.eps}\end{figure}$	Figure 4: Total flux (contours at 2, 8, 32 and 128 Jy/beam) overlaid with the polarisation intensity and direction (scaled vectors). The beam size shown in top left, along with bar representing 10 Jy of linearly polarised flux. The polarisation vectors are rotated to represent the magnetic field. The four regions with significant polarised emission are expanded.
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