All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2452fig1.eps}\end{figure}$ Figure 1: Map of M 82 around the ULXs D and F (see Table 4). The brightest radio source in the field is e₂ which is coincident with the X-ray point source E. The FWHM of all X-ray point sources has been set to 1''. Even though the radio source d₁ is outside of the r=0.5'' circle for ULX D, its offset (0.77'') is consistent with the ULX X-ray position.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{2452fig2.eps}\end{figure}$ Figure 2: The double source in NGC 4736. The upper source is called source a and the lower and stronger source is called b.
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In the text

$\begin{figure} \par\includegraphics[width=10cm,clip]{2452fig3.eps}\end{figure}$ Figure 3: The upper limits of the ULXs with respect to the low/hard state XRB and AGN population. The lines correspond to different black hole masses. From top to bottom $6, 6\times 10^2$ , $6\times 10^6$ , $6 \times 10^9~{M}_{\odot}$ . The left ULX radio detection represents NGC 5408, while the right is the radio flare in M 82. The correlation should not hold for fares; this was just plotted for comparison. As GRS 1915 and Cyg X-3 are both radio transients, they are not expected to follow the correlation.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2452fig4.eps}\end{figure}$ Figure A.1: Light-curve of NGC 4736. Note that the VLA array configuration changed from A to B during the last epochs.

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2452fig1.eps}\end{figure}$	Figure 1: Map of M 82 around the ULXs D and F (see Table 4). The brightest radio source in the field is e₂ which is coincident with the X-ray point source E. The FWHM of all X-ray point sources has been set to 1''. Even though the radio source d₁ is outside of the r=0.5'' circle for ULX D, its offset (0.77'') is consistent with the ULX X-ray position.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{2452fig2.eps}\end{figure}$	Figure 2: The double source in NGC 4736. The upper source is called source a and the lower and stronger source is called b.
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